explanation      blue bibcodes open ADS page with paths to full text
Author name code: bahcall
ADS astronomy entries on 2022-09-14
author:Bahcall, John N.

---------------------------------------------------------
Title: The Search for Muon Neutrinos from Northern Hemisphere
    Gamma-Ray Bursts with AMANDA
Authors: Achterberg, A.; Ackermann, M.; Adams, J.; Ahrens, J.; Andeen,
   K.; Auffenberg, J.; Bahcall, J. N.; Bai, X.; Baret, B.; Barwick,
   S. W.; Bay, R.; Beattie, K.; Becka, T.; Becker, J. K.; Becker,
   K. -H.; Berghaus, P.; Berley, D.; Bernardini, E.; Bertrand, D.;
   Besson, D. Z.; Blaufuss, E.; Boersma, D. J.; Bohm, C.; Bolmont, J.;
   Böser, S.; Botner, O.; Bouchta, A.; Braun, J.; Burgess, C.; Burgess,
   T.; Castermans, T.; Chirkin, D.; Christy, B.; Clem, J.; Cowen, D. F.;
   D'Agostino, M. V.; Davour, A.; Day, C. T.; De Clercq, C.; Demirörs,
   L.; Descamps, F.; Desiati, P.; DeYoung, T.; Diaz-Velez, J. C.;
   Dreyer, J.; Dumm, J. P.; Duvoort, M. R.; Edwards, W. R.; Ehrlich,
   R.; Eisch, J.; Ellsworth, R. W.; Evenson, P. A.; Fadiran, O.; Fazely,
   A. R.; Filimonov, K.; Foerster, M. M.; Fox, B. D.; Franckowiak, A.;
   Gaisser, T. K.; Gallagher, J.; Ganugapati, R.; Geenen, H.; Gerhardt,
   L.; Goldschmidt, A.; Goodman, J. A.; Gozzini, R.; Griesel, T.;
   Gross, A.; Grullon, S.; Gunasingha, R. M.; Gurtner, M.; Hallgren,
   A.; Halzen, F.; Han, K.; Hanson, K.; Hardtke, D.; Hardtke, R.; Hart,
   J. E.; Hasegawa, Y.; Hauschildt, T.; Hays, D.; Heise, J.; Helbing,
   K.; Hellwig, M.; Herquet, P.; Hill, G. C.; Hodges, J.; Hoffman,
   K. D.; Hommez, B.; Hoshina, K.; Hubert, D.; Hughey, B.; Hulth, P. O.;
   Hülss, J. -P.; Hultqvist, K.; Hundertmark, S.; Inaba, M.; Ishihara,
   A.; Jacobsen, J.; Japaridze, G. S.; Johansson, H.; Jones, A.; Joseph,
   J. M.; Kampert, K. -H.; Kappes, A.; Karg, T.; Karle, A.; Kawai, H.;
   Kelley, J. L.; Kitamura, N.; Klein, S. R.; Klepser, S.; Kohnen, G.;
   Kolanoski, H.; Köpke, L.; Kowalski, M.; Kowarik, T.; Krasberg, M.;
   Kuehn, K.; Labare, M.; Landsman, H.; Leich, H.; Leier, D.; Liubarsky,
   I.; Lundberg, J.; Lünemann, J.; Madsen, J.; Mase, K.; Matis, H. S.;
   McCauley, T.; McParland, C. P.; Meli, A.; Messarius, T.; Mészáros,
   P.; Miyamoto, H.; Mokhtarani, A.; Montaruli, T.; Morey, A.; Morse,
   R.; Movit, S. M.; Münich, K.; Nahnhauer, R.; Nam, J. W.; Niessen,
   P.; Nygren, D. R.; Ögelman, H.; Olivas, A.; Patton, S.; Peña-Garay,
   C.; Pérez de los Heros, C.; Piegsa, A.; Pieloth, D.; Pohl, A. C.;
   Porrata, R.; Pretz, J.; Price, P. B.; Przybylski, G. T.; Rawlins, K.;
   Razzaque, S.; Resconi, E.; Rhode, W.; Ribordy, M.; Rizzo, A.; Robbins,
   S.; Roth, P.; Rott, C.; Rutledge, D.; Ryckbosch, D.; Sander, H. -G.;
   Sarkar, S.; Schlenstedt, S.; Schmidt, T.; Schneider, D.; Seckel, D.;
   Semburg, B.; Seo, S. H.; Seunarine, S.; Silvestri, A.; Smith, A. J.;
   Solarz, M.; Song, C.; Sopher, J. E.; Spiczak, G. M.; Spiering, C.;
   Stamatikos, M.; Stanev, T.; Steffen, P.; Stezelberger, T.; Stokstad,
   R. G.; Stoufer, M. C.; Stoyanov, S.; Strahler, E. A.; Straszheim, T.;
   Sulanke, K. -H.; Sullivan, G. W.; Sumner, T. J.; Taboada, I.; Tarasova,
   O.; Tepe, A.; Thollander, L.; Tilav, S.; Tluczykont, M.; Toale, P. A.;
   Turčan, D.; van Eijndhoven, N.; Vandenbroucke, J.; Van Overloop, A.;
   Viscomi, V.; Voigt, B.; Wagner, W.; Walck, C.; Waldmann, H.; Walter,
   M.; Wang, Y. -R.; Wendt, C.; Wiebusch, C. H.; Wikström, G.; Williams,
   D. R.; Wischnewski, R.; Wissing, H.; Woschnagg, K.; Xu, X. W.; Yodh,
   G.; Yoshida, S.; Zornoza, J. D.; Interplanetary Network, The
2008ApJ...674..357A    Altcode: 2007arXiv0705.1186T
  We present the results of the analysis of neutrino observations by
  the Antarctic Muon and Neutrino Detector Array (AMANDA) correlated
  with photon observations of more than 400 gamma-ray bursts (GRBs) in
  the northern hemisphere from 1997 to 2003. During this time period,
  AMANDA's effective collection area for muon neutrinos was larger
  than that of any other existing detector. After the application of
  various selection criteria to our data, we expect ~1 neutrino event
  and <2 background events. Based on our observations of zero events
  during and immediately prior to the GRBs in the data set, we set
  the most stringent upper limit on muon neutrino emission correlated
  with GRBs. Assuming a Waxman-Bahcall spectrum and incorporating all
  systematic uncertainties, our flux upper limit has a normalization at
  1 PeV of E<SUP>2</SUP>Φ<SUB>ν</SUB> &lt;= 6.3 × 10<SUP>-9</SUP>
  GeV cm<SUP>-2</SUP> s<SUP>-1</SUP> sr<SUP>-1</SUP>, with 90% of the
  events expected within the energy range of ~10 TeV to ~3 PeV. The impact
  of this limit on several theoretical models of GRBs is discussed, as
  well as the future potential for detection of GRBs by next-generation
  neutrino telescopes. Finally, we briefly describe several modifications
  to this analysis in order to apply it to other types of transient
  point sources.

---------------------------------------------------------
Title: IceCube contributions to the XIV International Symposium on
    Very High Energy Cosmic Ray Interactions (ISVHECRI 2006)
Authors: IceCube Collaboration; Achterberg, A.; Ackermann, M.; Adams,
   J.; Ahrens, J.; Andeen, K.; Atlee, D. W.; Bahcall, J. N.; Bai, X.;
   Baret, B.; Barwick, S. W.; Bay, R.; Beattie, K.; Becka, T.; Becker,
   J. K.; Becker, K. -H.; Berghaus, P.; Berley, D.; Bernardini, E.;
   Bertrand, D.; Besson, D. Z.; Blaufuss, E.; Boersma, D. J.; Bohm,
   C.; Bolmont, J.; Böser, S.; Botner, O.; Bouchta, A.; Braun, J.;
   Burgess, C.; Burgess, T.; Castermans, T.; Chirkin, D.; Christy, B.;
   Clem, J.; Cowen, D. F.; D'Agostino, M. V.; Davour, A.; Day, C. T.;
   de Clercq, C.; Demirörs, L.; Descamps, F.; Desiati, P.; Deyoung, T.;
   Diaz-Velez, J. C.; Dreyer, J.; Dumm, J. P.; Duvoort, M. R.; Edwards,
   W. R.; Ehrlich, R.; Eisch, J.; Ellsworth, R. W.; Evenson, P. A.;
   Fadiran, O.; Fazely, A. R.; Feser, T.; Filimonov, K.; Fox, B. D.;
   Gaisser, T. K.; Gallagher, J.; Ganugapati, R.; Geenen, H.; Gerhardt,
   L.; Goldschmidt, A.; Goodman, J. A.; Gozzini, R.; Grullon, S.; Groß,
   A.; Gunasingha, R. M.; Gurtner, M.; Hallgren, A.; Halzen, F.; Han,
   K.; Hanson, K.; Hardtke, D.; Hardtke, R.; Harenberg, T.; Hart, J. E.;
   Hauschildt, T.; Hays, D.; Heise, J.; Helbing, K.; Hellwig, M.; Herquet,
   P.; Hill, G. C.; Hodges, J.; Hoffman, K. D.; Hommez, B.; Hoshina, K.;
   Hubert, D.; Hughey, B.; Hulth, P. O.; Hultqvist, K.; Hundertmark,
   S.; Hülß, J. -P.; Ishihara, A.; Jacobsen, J.; Japaridze, G. S.;
   Johansson, H.; Jones, A.; Joseph, J. M.; Kampert, K. -H.; Karle, A.;
   Kawai, H.; Kelley, J. L.; Kestel, M.; Kitamura, N.; Klein, S. R.;
   Klepser, S.; Kohnen, G.; Kolanoski, H.; Köpke, L.; Krasberg, M.;
   Kuehn, K.; Landsman, H.; Leich, H.; Leier, D.; Leuthold, M.; Liubarsky,
   I.; Lundberg, J.; Lünemann, J.; Madsen, J.; Mase, K.; Matis, H. S.;
   McCauley, T.; McParland, C. P.; Meli, A.; Messarius, T.; Mészáros,
   P.; Miyamoto, H.; Mokhtarani, A.; Montaruli, T.; Morey, A.; Morse,
   R.; Movit, S. M.; Münich, K.; Nahnhauer, R.; Nam, J. W.; Nießen,
   P.; Nygren, D. R.; Ögelman, H.; Olivas, A.; Patton, S.; Peña-Garay,
   C.; Pérez de Los Heros, C.; Piegsa, A.; Pieloth, D.; Pohl, A. C.;
   Porrata, R.; Pretz, J.; Price, P. B.; Przybylski, G. T.; Rawlins, K.;
   Razzaque, S.; Resconi, E.; Rhode, W.; Ribordy, M.; Rizzo, A.; Robbins,
   S.; Roth, P.; Rott, C.; Rutledge, D.; Ryckbosch, D.; Sander, H. -G.;
   Sarkar, S.; Schlenstedt, S.; Schmidt, T.; Schneider, D.; Seckel, D.;
   Seo, S. H.; Seunarine, S.; Silvestri, A.; Smith, A. J.; Solarz, M.;
   Song, C.; Sopher, J. E.; Spiczak, G. M.; Spiering, C.; Stamatikos, M.;
   Stanev, T.; Steffen, P.; Stezelberger, T.; Stokstad, R. G.; Stoufer,
   M. C.; Stoyanov, S.; Strahler, E. A.; Straszheim, T.; Sulanke, K. -H.;
   Sullivan, G. W.; Sumner, T. J.; Taboada, I.; Tarasova, O.; Tepe, A.;
   Thollander, L.; Tilav, S.; Tluczykont, M.; Toale, P. A.; Turčan, D.;
   van Eijndhoven, N.; Vandenbroucke, J.; van Overloop, A.; Voigt, B.;
   Wagner, W.; Walck, C.; Waldmann, H.; Walter, M.; Wang, Y. -R.; Wendt,
   C.; Wiebusch, C. H.; Wikström, G.; Williams, D. R.; Wischnewski,
   R.; Wissing, H.; Woschnagg, K.; Xu, X. W.; Yodh, G.; Yoshida, S.;
   Zornoza, J. D.
2008NuPhS.175..407I    Altcode: 2008NuPhS.175..407A
  No abstract at ADS

---------------------------------------------------------
Title: Search for Neutrino-induced Cascades from Gamma-Ray Bursts
    with AMANDA
Authors: Achterberg, A.; Ackermann, M.; Adams, J.; Ahrens, J.; Andeen,
   K.; Auffenberg, J.; Bahcall, J. N.; Bai, X.; Baret, B.; Barwick,
   S. W.; Bay, R.; Beattie, K.; Becka, T.; Becker, J. K.; Becker,
   K. -H.; Berghaus, P.; Berley, D.; Bernardini, E.; Bertrand, D.;
   Besson, D. Z.; Blaufuss, E.; Boersma, D. J.; Bohm, C.; Bolmont, J.;
   Böser, S.; Botner, O.; Bouchta, A.; Braun, J.; Burgess, C.; Burgess,
   T.; Castermans, T.; Chirkin, D.; Christy, B.; Clem, J.; Cowen, D. F.;
   D'Agostino, M. V.; Davour, A.; Day, C. T.; De Clercq, C.; Demirörs,
   L.; Descamps, F.; Desiati, P.; De Young, T.; Diaz-Velez, J. C.;
   Dreyer, J.; Dumm, J. P.; Duvoort, M. R.; Edwards, W. R.; Ehrlich,
   R.; Eisch, J.; Ellsworth, R. W.; Evenson, P. A.; Fadiran, O.; Fazely,
   A. R.; Filimonov, K.; Foerster, M. M.; Fox, B. D.; Franckowiak, A.;
   Gaisser, T. K.; Gallagher, J.; Ganugapati, R.; Geenen, H.; Gerhardt,
   L.; Goldschmidt, A.; Goodman, J. A.; Gozzini, R.; Griesel, T.;
   Grullon, S.; Groß, A.; Gunasingha, R. M.; Gurtner, M.; Hallgren,
   A.; Halzen, F.; Han, K.; Hanson, K.; Hardtke, D.; Hardtke, R.; Hart,
   J. E.; Hasegawa, Y.; Hauschildt, T.; Hays, D.; Heise, J.; Helbing,
   K.; Hellwig, M.; Herquet, P.; Hill, G. C.; Hodges, J.; Hoffman,
   K. D.; Hommez, B.; Hoshina, K.; Hubert, D.; Hughey, B.; Hulth,
   P. O.; Hultqvist, K.; Hülß, J. -P.; Hundertmark, S.; Inaba, M.;
   Ishihara, A.; Jacobsen, J.; Japaridze, G. S.; Johansson, H.; Jones,
   A.; Joseph, J. M.; Kampert, K. -H.; Karg, T.; Karle, A.; Kawai, H.;
   Kelley, J. L.; Kitamura, N.; Klein, S. R.; Klepser, S.; Kohnen, G.;
   Kolanoski, H.; Köpke, L.; Kowalski, M.; Kowarik, T.; Krasberg, M.;
   Kuehn, K.; Labare, M.; Landsman, H.; Leich, H.; Leier, D.; Liubarsky,
   I.; Lundberg, J.; Lünemann, J.; Madsen, J.; Mase, K.; Matis, H. S.;
   McCauley, T.; McParland, C. P.; Meli, A.; Messarius, T.; Mészáros,
   P.; Miyamoto, H.; Mokhtarani, A.; Montaruli, T.; Morey, A.; Morse,
   R.; Movit, S. M.; Münich, K.; Nahnhauer, R.; Nam, J. W.; Nießen,
   P.; Nygren, D. R.; Ögelman, H.; Olivas, A.; Patton, S.; Peña-Garay,
   C.; Pérez de los Heros, C.; Piegsa, A.; Pieloth, D.; Pohl, A. C.;
   Porrata, R.; Pretz, J.; Price, P. B.; Przybylski, G. T.; Rawlins, K.;
   Razzaque, S.; Resconi, E.; Rhode, W.; Ribordy, M.; Rizzo, A.; Robbins,
   S.; Roth, P.; Rott, C.; Rutledge, D.; Ryckbosch, D.; Sander, H. -G.;
   Sarkar, S.; Schlenstedt, S.; Schmidt, T.; Schneider, D.; Seckel, D.;
   Semburg, B.; Seo, S. H.; Seunarine, S.; Silvestri, A.; Smith, A. J.;
   Solarz, M.; Song, C.; Sopher, J. E.; Spiczak, G. M.; Spiering, C.;
   Stamatikos, M.; Stanev, T.; Steffen, P.; Stezelberger, T.; Stokstad,
   R. G.; Stoufer, M. C.; Stoyanov, S.; Strahler, E. A.; Straszheim, T.;
   Sulanke, K. -H.; Sullivan, G. W.; Sumner, T. J.; Taboada, I.; Tarasova,
   O.; Tepe, A.; Thollander, L.; Tilav, S.; Tluczykont, M.; Toale, P. A.;
   Turčan, D.; van Eijndhoven, N.; Vandenbroucke, J.; Van Overloop, A.;
   Viscomi, V.; Voigt, B.; Wagner, W.; Walck, C.; Waldmann, H.; Walter,
   M.; Wang, Y. -R.; Wendt, C.; Wiebusch, C. H.; Wikström, G.; Williams,
   D. R.; Wischnewski, R.; Wissing, H.; Woschnagg, K.; Xu, X. W.; Yodh,
   G.; Yoshida, S.; Zornoza, J. D.
2007ApJ...664..397A    Altcode: 2007astro.ph..2265I
  Using the neutrino telescope AMANDA-II, we have conducted two
  analyses searching for neutrino-induced cascades from gamma-ray
  bursts. No evidence of astrophysical neutrinos was found, and limits
  are presented for several models. We also present neutrino effective
  areas which allow the calculation of limits for any neutrino production
  model. The first analysis looked for a statistical excess of events
  within a sliding window of 1 or 100 s (for short and long burst
  classes, respectively) during the years 2001-2003. The resulting
  upper limit on the diffuse flux normalization times E<SUP>2</SUP>
  for the Waxman-Bahcall model at 1 PeV is 1.6×10<SUP>-6</SUP> GeV
  cm<SUP>-2</SUP> s<SUP>-1</SUP> sr<SUP>-1</SUP> (a factor of 120 above
  the theoretical prediction). For this search 90% of the neutrinos
  would fall in the energy range 50 TeV to 7 PeV. The second analysis
  looked for neutrino-induced cascades in coincidence with 73 bursts
  detected by BATSE in the year 2000. The resulting upper limit on
  the diffuse flux normalization times E<SUP>2</SUP>, also at 1 PeV, is
  1.5×10<SUP>-6</SUP> GeV cm<SUP>-2</SUP> s<SUP>-1</SUP> sr<SUP>-1</SUP>
  (a factor of 110 above the theoretical prediction) for the same energy
  range. The neutrino-induced cascade channel is complementary to the
  up-going muon channel. We comment on its advantages for searches of
  neutrinos from GRBs and its future use with IceCube.

---------------------------------------------------------
Title: Five years of searches for point sources of astrophysical
    neutrinos with the AMANDA-II neutrino telescope
Authors: Achterberg, A.; Ackermann, M.; Adams, J.; Ahrens, J.; Andeen,
   K.; Atlee, D. W.; Bahcall, J. N.; Bai, X.; Baret, B.; Barwick, S. W.;
   Bay, R.; Beattie, K.; Becka, T.; Becker, J. K.; Becker, K. -H.;
   Berghaus, P.; Berley, D.; Bernardini, E.; Bertrand, D.; Besson,
   D. Z.; Blaufuss, E.; Boersma, D. J.; Bohm, C.; Bolmont, J.; Böser,
   S.; Botner, O.; Bouchta, A.; Braun, J.; Burgess, C.; Burgess, T.;
   Castermans, T.; Chirkin, D.; Christy, B.; Clem, J.; Cowen, D. F.;
   D'Agostino, M. V.; Davour, A.; Day, C. T.; de Clercq, C.; Demirörs,
   L.; Descamps, F.; Desiati, P.; De Young, T.; Diaz-Velez, J. C.; Dreyer,
   J.; Dumm, J. P.; Duvoort, M. R.; Edwards, W. R.; Ehrlich, R.; Eisch,
   J.; Ellsworth, R. W.; Evenson, P. A.; Fadiran, O.; Fazely, A. R.;
   Feser, T.; Filimonov, K.; Fox, B. D.; Gaisser, T. K.; Gallagher, J.;
   Ganugapati, R.; Geenen, H.; Gerhardt, L.; Goldschmidt, A.; Goodman,
   J. A.; Gozzini, R.; Grullon, S.; Groß, A.; Gunasingha, R. M.;
   Gurtner, M.; Hallgren, A.; Halzen, F.; Han, K.; Hanson, K.; Hardtke,
   D.; Hardtke, R.; Harenberg, T.; Hart, J. E.; Hauschildt, T.; Hays,
   D.; Heise, J.; Helbing, K.; Hellwig, M.; Herquet, P.; Hill, G. C.;
   Hodges, J.; Hoffman, K. D.; Hommez, B.; Hoshina, K.; Hubert, D.;
   Hughey, B.; Hulth, P. O.; Hultqvist, K.; Hundertmark, S.; Hülß,
   J. -P.; Ishihara, A.; Jacobsen, J.; Japaridze, G. S.; Johansson,
   H.; Jones, A.; Joseph, J. M.; Kampert, K. -H.; Karle, A.; Kawai, H.;
   Kelley, J. L.; Kestel, M.; Kitamura, N.; Klein, S. R.; Klepser, S.;
   Kohnen, G.; Kolanoski, H.; Kowalski, M.; Köpke, L.; Krasberg, M.;
   Kuehn, K.; Landsman, H.; Leich, H.; Leier, D.; Leuthold, M.; Liubarsky,
   I.; Lundberg, J.; Lünemann, J.; Madsen, J.; Mase, K.; Matis, H. S.;
   McCauley, T.; McParland, C. P.; Meli, A.; Messarius, T.; Mészáros,
   P.; Miyamoto, H.; Mokhtarani, A.; Montaruli, T.; Morey, A.; Morse,
   R.; Movit, S. M.; Münich, K.; Nahnhauer, R.; Nam, J. W.; Nießen,
   P.; Nygren, D. R.; Ögelman, H.; Olivas, A.; Patton, S.; Peña-Garay,
   C.; Pérez de Los Heros, C.; Piegsa, A.; Pieloth, D.; Pohl, A. C.;
   Porrata, R.; Pretz, J.; Price, P. B.; Przybylski, G. T.; Rawlins, K.;
   Razzaque, S.; Resconi, E.; Rhode, W.; Ribordy, M.; Rizzo, A.; Robbins,
   S.; Roth, P.; Rott, C.; Rutledge, D.; Ryckbosch, D.; Sander, H. -G.;
   Sarkar, S.; Schlenstedt, S.; Schmidt, T.; Schneider, D.; Seckel, D.;
   Seo, S. H.; Seunarine, S.; Silvestri, A.; Smith, A. J.; Solarz, M.;
   Song, C.; Sopher, J. E.; Spiczak, G. M.; Spiering, C.; Stamatikos, M.;
   Stanev, T.; Steffen, P.; Stezelberger, T.; Stokstad, R. G.; Stoufer,
   M. C.; Stoyanov, S.; Strahler, E. A.; Straszheim, T.; Sulanke, K. -H.;
   Sullivan, G. W.; Sumner, T. J.; Taboada, I.; Tarasova, O.; Tepe, A.;
   Thollander, L.; Tilav, S.; Tluczykont, M.; Toale, P. A.; Turčan, D.;
   van Eijndhoven, N.; Vandenbroucke, J.; van Overloop, A.; Voigt, B.;
   Wagner, W.; Walck, C.; Waldmann, H.; Walter, M.; Wang, Y. -R.; Wendt,
   C.; Wiebusch, C. H.; Wikström, G.; Williams, D. R.; Wischnewski,
   R.; Wissing, H.; Woschnagg, K.; Xu, X. W.; Yodh, G.; Yoshida, S.;
   Zornoza, J. D.
2007PhRvD..75j2001A    Altcode: 2006astro.ph.11063A
  We report the results of a five-year survey of the northern sky to
  search for point sources of high energy neutrinos. The search was
  performed on the data collected with the AMANDA-II neutrino telescope
  in the years 2000 to 2004, with a live time of 1001 days. The sample
  of selected events consists of 4282 upward going muon tracks with high
  reconstruction quality and an energy larger than about 100 GeV. We found
  no indication of point sources of neutrinos and set 90% confidence
  level flux upper limits for an all-sky search and also for a catalog
  of 32 selected sources. For the all-sky search, our average (over
  declination and right ascension) experimentally observed upper limit
  Φ<SUP>0</SUP>=((E)/(1TeV))<SUP>γ</SUP>·(dΦ)/(dE) to a point source
  flux of muon and tau neutrino (detected as muons arising from taus) is
  Φ<SUB>ν<SUB>μ</SUB>+ν¯<SUB>μ</SUB></SUB><SUP>0</SUP>+Φ<SUB>ν<SUB>τ</SUB>+ν¯<SUB>τ</SUB></SUB><SUP>0</SUP>=11.1×10<SUP>-11</SUP>TeV<SUP>-1</SUP>cm<SUP>-2</SUP>s<SUP>-1</SUP>,
  in the energy range between 1.6 TeV and 2.5 PeV for a flavor ratio
  Φ<SUB>ν<SUB>μ</SUB>+ν¯<SUB>μ</SUB></SUB><SUP>0</SUP>/Φ<SUB>ν<SUB>τ</SUB>+ν¯<SUB>τ</SUB></SUB><SUP>0</SUP>=1
  and assuming a spectral index γ=2. It should be noticed
  that this is the first time we set upper limits to the flux
  of muon and tau neutrinos. In previous papers we provided
  muon neutrino upper limits only neglecting the sensitivity
  to a signal from tau neutrinos, which improves the limits
  by 10% to 16%. The value of the average upper limit presented
  in this work corresponds to twice the limit on the muon neutrino flux
  Φ<SUB>ν<SUB>μ</SUB>+ν¯<SUB>μ</SUB></SUB><SUP>0</SUP>=5.5×10<SUP>-11</SUP>TeV<SUP>-1</SUP>cm<SUP>-2</SUP>s<SUP>-1</SUP>.
  A stacking analysis for preselected active galactic nuclei and a search
  based on the angular separation of the events were also performed. We
  report the most stringent flux upper limits to date, including the
  results of a detailed assessment of systematic uncertainties.

---------------------------------------------------------
Title: VizieR Online Data Catalog: AGN neutrino source candidates
    (Achterberg+, 2006)
Authors: Achterberg, A.; Ackermann, M.; Adams, J.; Ahrens, J.;
   Atlee, D. W.; Bahcall, J. N.; Bair, X.; Baret, B.; Bartelt, M.;
   Barwick, S. W.; Bay, R.; Beattie, K.; Becka, T.; Becker, J. K.;
   Becker, K. -H.; Berghaus, P.; Berley, D.; Bernardini, E.; Bertrand,
   D.; Besson, D. Z.; Blaufuss, E.; Boersma, D. J.; Bohm, C.; Boeser,
   S.; Botner, O.; Bouchta, A.; Braun, J.; Burgess, C.; Burgess, T.;
   Castermans, T.; Chirkin, D.; Clem, J.; Collin, B.; Conrad, J.; Cooley,
   J.; Cowen, D. F.; D'Agostino, M. V.; Davour, A.; Day, C. T.; de Clercq,
   C.; Desiati, P.; De Young, T.; Dreyer, J.; Duvoort, M. R.; Edwards,
   W. R.; Ehrlich, R.; Ellsworth, R. W.; Evenson, P. A.; Fazely, A. R.;
   Feser, T.; Filimonov, K.; Gaisser, T. K.; Gallagher, J.; Ganugapati,
   R.; Geenen, H.; Gerhardt, L.; Goldschmidt, A.; Goodman, J. A.; Greene,
   M. G.; Grullon, S.; Gross, A.; Gunasingha, R. M.; Hallgren, A.; Halzen,
   F.; Han, K.; Hanson, K.; Hardtke, D.; Hardtke, R.; Harenberg, T.; Hart,
   J. E.; Hauschildt, T.; Hays, D.; Heise, J.; Helbing, K.; Hellwig,
   M.; Herquet, P.; Hill, G. C.; Hodges, J.; Hoffman, K. D.; Hoshina,
   K.; Hubert, D.; Hughey, B.; Hulth, P. O.; Hultqvist, K.; Hundertmark,
   S.; Ishihara, A.; Jacobsen, J.; Japaridze, G. S.; Jones, A.; Joseph,
   J. M.; Kampert, K. -H.; Karle, A.; Kawai, H.; Kelley, J. L.; Kestel,
   M.; Kitamura, N.; Klein, S. R.; Klepser, S.; Kohnen, G.; Kolanoski, H.;
   Koepke, L.; Krasberg, M.; Kuehn, K.; Landsman, H.; Lang, R.; Leich,
   H.; Leuthold, M.; Liubarsky, I.; Lundbert, J.; Madsen, J.; Mase, K.;
   Matis, H. S.; McCauley, T.; McParland, C. P.; Meli, A.; Messarius, T.;
   Meszaros, P.; Minor, R. H.; Miocinovic, P.; Miyamoto, H.; Mokhtarani,
   A.; Montaruli, T.; Morey, A.; Morse, R.; Movit, S. M.; Munich, K.;
   Nahnhauer, R.; Nam, J. W.; Niessen, P.; Nygren, D. R.; Oegelman, H.;
   Olbrechts, Ph.; Olivas, A.; Patton, S.; Pena-Garay, C.; Perez de los
   Heros, C.; Pieloth, D.; Pohl, A. C.; Porrata, R.; Pretz, J.; Price,
   P. B.; Przybylski, G. T.; Rawlins, K.; Razzaque, S.; Refflinghaus, F.;
   Resconi, E.; Rhode, W.; Ribordy, M.; Richter, S.; Rizzo, A.; Robbins,
   S.; Rott, C.; Rutledge, D.; Sander, H. -G.; Schlenstedt, S.; Schneider,
   D.; Seckel, D.; Seo, S. H.; Seunarine, S.; Silvestri, A.; Smith, A. J.;
   Solarz, M.; Song, C.; Sopher, J. E.; Spiczak, G. M.; Spiering, C.;
   Stamatikos, M.; Stanev, T.; Steffen, P.; Steele, D.; Stezelberger,
   T.; Stokstad, R. G.; Stoufer, M. C.; Stoyanov, S.; Sulanke, K. -H.;
   Sullivan, G. W.; Sumner, T. J.; Taboada, I.; Tarasova, O.; Tepe, A.;
   Thollander, L.; Tilav, S.; Toale, P. A.; Turcan, D.; Van Eijndhoven,
   T. J.; Vandenbroucke, J.; Voigt, B.; Wagner, W.; Walck, C.; Waldmann,
   H.; Walter, M.; Wang, Y. -R.; Wendt, C.; Wiesbusch, C. H.; Wikstroem,
   G.; Williams, D. R.; Wischnewski, R.; Wissing, H.; Woschnagg, K.;
   Xu, X. W.; Yodh, G.; Yoshida, S.; Zornoza, J. D.; Biermann, P. L.
2007yCatp030002601A    Altcode:
  The sensitivity of a search for sources of TeV neutrinos can be
  improved by grouping potential sources together into generic classes
  in a procedure that is known as source stacking. In this paper,
  we define catalogs of Active Galactic Nuclei (AGN) and use them to
  perform a source stacking analysis. The grouping of AGN into classes is
  done in two steps: first, AGN classes are defined, then, sources to be
  stacked are selected assuming that a potential neutrino flux is linearly
  correlated with the photon luminosity in a certain energy band (radio,
  IR, optical, keV, GeV, TeV). Lacking any secure detailed knowledge on
  neutrino production in AGN, this correlation is motivated by hadronic
  AGN models, as briefly reviewed in this paper. <P />The source stacking
  search for neutrinos from generic AGN classes is illustrated using the
  data collected by the AMANDA-II high-energy neutrino detector during
  the year 2000. No significant excess for any of the suggested groups
  was found. <P />(11 data files).

---------------------------------------------------------
Title: Limits on the High-Energy Gamma and Neutrino Fluxes from
    the SGR 1806-20 Giant Flare of 27 December 2004 with the AMANDA-II
    Detector
Authors: Achterberg, A.; Ackermann, M.; Adams, J.; Ahrens, J.; Andeen,
   K.; Atlee, D. W.; Bahcall, J. N.; Bai, X.; Baret, B.; Bartelt, M.;
   Barwick, S. W.; Bay, R.; Beattie, K.; Becka, T.; Becker, J. K.;
   Becker, K. -H.; Berghaus, P.; Berley, D.; Bernardini, E.; Bertrand,
   D.; Besson, D. Z.; Blaufuss, E.; Boersma, D. J.; Bohm, C.; Bolmont, J.;
   Böser, S.; Botner, O.; Bouchta, A.; Braun, J.; Burgess, C.; Burgess,
   T.; Castermans, T.; Chirkin, D.; Christy, B.; Clem, J.; Cowen, D. F.;
   D'Agostino, M. V.; Davour, A.; Day, C. T.; de Clercq, C.; Demirörs,
   L.; Descamps, F.; Desiati, P.; De Young, T.; Diaz-Velez, J. C.; Dreyer,
   J.; Dumm, J. P.; Duvoort, M. R.; Edwards, W. R.; Ehrlich, R.; Eisch,
   J.; Ellsworth, R. W.; Evenson, P. A.; Fadiran, O.; Fazely, A. R.;
   Feser, T.; Filimonov, K.; Fox, B. D.; Gaisser, T. K.; Gallagher, J.;
   Ganugapati, R.; Geenen, H.; Gerhardt, L.; Goldschmidt, A.; Goodman,
   J. A.; Gozzini, R.; Grullon, S.; Groß, A.; Gunasingha, R. M.;
   Gurtner, M.; Hallgren, A.; Halzen, F.; Han, K.; Hanson, K.; Hardtke,
   D.; Hardtke, R.; Harenberg, T.; Hart, J. E.; Hauschildt, T.; Hays, D.;
   Heise, J.; Helbing, K.; Hellwig, M.; Herquet, P.; Hill, G. C.; Hodges,
   J.; Hoffman, K. D.; Hommez, B.; Hoshina, K.; Hubert, D.; Hughey,
   B.; Hulth, P. O.; Hultqvist, K.; Hundertmark, S.; Hülß, J. -P.;
   Ishihara, A.; Jacobsen, J.; Japaridze, G. S.; Jones, A.; Joseph,
   J. M.; Kampert, K. -H.; Karle, A.; Kawai, H.; Kelley, J. L.; Kestel,
   M.; Kitamura, N.; Klein, S. R.; Klepser, S.; Kohnen, G.; Kolanoski,
   H.; Köpke, L.; Krasberg, M.; Kuehn, K.; Landsman, H.; Leich, H.;
   Liubarsky, I.; Lundberg, J.; Madsen, J.; Mase, K.; Matis, H. S.;
   McCauley, T.; McParland, C. P.; Meli, A.; Messarius, T.; Mészáros,
   P.; Miyamoto, H.; Mokhtarani, A.; Montaruli, T.; Morey, A.; Morse,
   R.; Movit, S. M.; Münich, K.; Nahnhauer, R.; Nam, J. W.; Nießen,
   P.; Nygren, D. R.; Ögelman, H.; Olbrechts, Ph.; Olivas, A.; Patton,
   S.; Peña-Garay, C.; Pérez de Los Heros, C.; Piegsa, A.; Pieloth, D.;
   Pohl, A. C.; Porrata, R.; Pretz, J.; Price, P. B.; Przybylski, G. T.;
   Rawlins, K.; Razzaque, S.; Refflinghaus, F.; Resconi, E.; Rhode, W.;
   Ribordy, M.; Rizzo, A.; Robbins, S.; Roth, P.; Rott, C.; Rutledge, D.;
   Ryckbosch, D.; Sander, H. -G.; Sarkar, S.; Schlenstedt, S.; Schmidt,
   T.; Schneider, D.; Seckel, D.; Seo, S. H.; Seunarine, S.; Silvestri,
   A.; Smith, A. J.; Solarz, M.; Song, C.; Sopher, J. E.; Spiczak, G. M.;
   Spiering, C.; Stamatikos, M.; Stanev, T.; Steffen, P.; Stezelberger,
   T.; Stokstad, R. G.; Stoufer, M. C.; Stoyanov, S.; Strahler, E. A.;
   Straszheim, T.; Sulanke, K. -H.; Sullivan, G. W.; Sumner, T. J.;
   Taboada, I.; Tarasova, O.; Tepe, A.; Thollander, L.; Tilav, S.;
   Toale, P. A.; Turčan, D.; van Eijndhoven, N.; Vandenbroucke, J.;
   van Overloop, A.; Voigt, B.; Wagner, W.; Walck, C.; Waldmann, H.;
   Walter, M.; Wang, Y. -R.; Wendt, C.; Wiebusch, C. H.; Wikström, G.;
   Williams, D. R.; Wischnewski, R.; Wissing, H.; Woschnagg, K.; Xu,
   X. W.; Yodh, G.; Yoshida, S.; Zornoza, J. D.
2006PhRvL..97v1101A    Altcode: 2006astro.ph..7233T
  On 27 December 2004, a giant γ flare from the Soft Gamma-Ray Repeater
  1806-20 saturated many satellite gamma-ray detectors, being the
  brightest transient event ever observed in the Galaxy. AMANDA-II was
  used to search for down-going muons indicative of high-energy gammas
  and/or neutrinos from this object. The data revealed no significant
  signal, so upper limits (at 90% C.L.) on the normalization constant
  were set: 0.05(0.5)TeV<SUP>-1</SUP>m<SUP>-2</SUP>s<SUP>-1</SUP>
  for γ=-1.47 (-2) in the gamma flux and
  0.4(6.1)TeV<SUP>-1</SUP>m<SUP>-2</SUP>s<SUP>-1</SUP> for γ=-1.47 (-2)
  in the high-energy neutrino flux.

---------------------------------------------------------
Title: On the selection of AGN neutrino source candidates for a
    source stacking analysis with neutrino telescopes
Authors: Achterberg, A.; Ackermann, M.; Adams, J.; Ahrens, J.;
   Atlee, D. W.; Bahcall, J. N.; Bai, X.; Baret, B.; Bartelt, M.;
   Barwick, S. W.; Bay, R.; Beattie, K.; Becka, T.; Becker, J. K.;
   Becker, K. -H.; Berghaus, P.; Berley, D.; Bernardini, E.; Bertrand,
   D.; Besson, D. Z.; Blaufuss, E.; Boersma, D. J.; Bohm, C.; Böser,
   S.; Botner, O.; Bouchta, A.; Braun, J.; Burgess, C.; Burgess, T.;
   Castermans, T.; Chirkin, D.; Clem, J.; Collin, B.; Conrad, J.; Cooley,
   J.; Cowen, D. F.; D'Agostino, M. V.; Davour, A.; Day, C. T.; de Clercq,
   C.; Desiati, P.; De Young, T.; Dreyer, J.; Duvoort, M. R.; Edwards,
   W. R.; Ehrlich, R.; Ellsworth, R. W.; Evenson, P. A.; Fazely, A. R.;
   Feser, T.; Filimonov, K.; Gaisser, T. K.; Gallagher, J.; Ganugapati,
   R.; Geenen, H.; Gerhardt, L.; Goldschmidt, A.; Goodman, J. A.; Greene,
   M. G.; Grullon, S.; Groß, A.; Gunasingha, R. M.; Hallgren, A.; Halzen,
   F.; Han, K.; Hanson, K.; Hardtke, D.; Hardtke, R.; Harenberg, T.; Hart,
   J. E.; Hauschildt, T.; Hays, D.; Heise, J.; Helbing, K.; Hellwig,
   M.; Herquet, P.; Hill, G. C.; Hodges, J.; Hoffman, K. D.; Hoshina,
   K.; Hubert, D.; Hughey, B.; Hulth, P. O.; Hultqvist, K.; Hundertmark,
   S.; Ishihara, A.; Jacobsen, J.; Japaridze, G. S.; Jones, A.; Joseph,
   J. M.; Kampert, K. -H.; Karle, A.; Kawai, H.; Kelley, J. L.; Kestel,
   M.; Kitamura, N.; Klein, S. R.; Klepser, S.; Kohnen, G.; Kolanoski, H.;
   Köpke, L.; Krasberg, M.; Kuehn, K.; Landsman, H.; Lang, R.; Leich,
   H.; Leuthold, M.; Liubarsky, I.; Lundberg, J.; Madsen, J.; Mase, K.;
   Matis, H. S.; McCauley, T.; McParland, C. P.; Meli, A.; Messarius,
   T.; Mészáros, P.; Minor, R. H.; Miočinović, P.; Miyamoto, H.;
   Mokhtarani, A.; Montaruli, T.; Morey, A.; Morse, R.; Movit, S. M.;
   Münich, K.; Nahnhauer, R.; Nam, J. W.; Nießen, P.; Nygren, D. R.;
   Ögelman, H.; Olbrechts, Ph.; Olivas, A.; Patton, S.; Peña-Garay,
   C.; Pérez de Los Heros, C.; Pieloth, D.; Pohl, A. C.; Porrata, R.;
   Pretz, J.; Price, P. B.; Przybylski, G. T.; Rawlins, K.; Razzaque,
   S.; Refflinghaus, F.; Resconi, E.; Rhode, W.; Ribordy, M.; Richter,
   S.; Rizzo, A.; Robbins, S.; Rott, C.; Rutledge, D.; Sander, H. -G.;
   Schlenstedt, S.; Schneider, D.; Seckel, D.; Seo, S. H.; Seunarine,
   S.; Silvestri, A.; Smith, A. J.; Solarz, M.; Song, C.; Sopher,
   J. E.; Spiczak, G. M.; Spiering, C.; Stamatikos, M.; Stanev, T.;
   Steffen, P.; Steele, D.; Stezelberger, T.; Stokstad, R. G.; Stoufer,
   M. C.; Stoyanov, S.; Sulanke, K. -H.; Sullivan, G. W.; Sumner, T. J.;
   Taboada, I.; Tarasova, O.; Tepe, A.; Thollander, L.; Tilav, S.; Toale,
   P. A.; Turčan, D.; van Eijndhoven, N.; Vandenbroucke, J.; Voigt, B.;
   Wagner, W.; Walck, C.; Waldmann, H.; Walter, M.; Wang, Y. -R.; Wendt,
   C.; Wiebusch, C. H.; Wikström, G.; Williams, D. R.; Wischnewski,
   R.; Wissing, H.; Woschnagg, K.; Xu, X. W.; Yodh, G.; Yoshida, S.;
   Zornoza, J. D.; Biermann, P. L.
2006APh....26..282A    Altcode: 2006astro.ph..9534A
  The sensitivity of a search for sources of TeV neutrinos can be
  improved by grouping potential sources together into generic classes
  in a procedure that is known as source stacking. In this paper,
  we define catalogs of Active Galactic Nuclei (AGN) and use them to
  perform a source stacking analysis. The grouping of AGN into classes is
  done in two steps: first, AGN classes are defined, then, sources to be
  stacked are selected assuming that a potential neutrino flux is linearly
  correlated with the photon luminosity in a certain energy band (radio,
  IR, optical, keV, GeV, TeV). Lacking any secure detailed knowledge on
  neutrino production in AGN, this correlation is motivated by hadronic
  AGN models, as briefly reviewed in this paper. <P />The source stacking
  search for neutrinos from generic AGN classes is illustrated using the
  data collected by the AMANDA-II high-energy neutrino detector during
  the year 2000. No significant excess for any of the suggested groups
  was found.

---------------------------------------------------------
Title: First year performance of the IceCube neutrino telescope
Authors: IceCube Collaboration; Achterberg, A.; Ackermann, M.; Adams,
   J.; Ahrens, J.; Andeen, K.; Atlee, D. W.; Baccus, J.; Bahcall, J. N.;
   Bai, X.; Baret, B.; Bartelt, M.; Barwick, S. W.; Bay, R.; Beattie, K.;
   Becka, T.; Becker, J. K.; Becker, K. -H.; Berghaus, P.; Berley, D.;
   Bernardini, E.; Bertrand, D.; Besson, D. Z.; Blaufuss, E.; Boersma,
   D. J.; Bohm, C.; Böser, S.; Botner, O.; Bouchta, A.; Braun, J.;
   Burgess, C.; Burgess, T.; Castermans, T.; Cherwinka, J.; Chirkin, D.;
   Clem, J.; Cowen, D. F.; D'Agostino, M. V.; Davour, A.; Day, C. T.;
   de Clercq, C.; Demirörs, L.; Desiati, P.; De Young, T.; Diaz-Velez,
   J. C.; Dreyer, J.; Duvoort, M. R.; Edwards, W. R.; Ehrlich, R.; Eisch,
   J.; Elcheikh, A.; Ellsworth, R. W.; Evenson, P. A.; Fadiran, O.;
   Fazely, A. R.; Feser, T.; Filimonov, K.; Fox, B. D.; Gaisser, T. K.;
   Gallagher, J.; Ganugapati, R.; Geenen, H.; Gerhardt, L.; Goldschmidt,
   A.; Goodman, J. A.; Gozzini, R.; Greene, M. G.; Grullon, S.; Groß,
   A.; Gunasingha, R. M.; Gurtner, M.; Hallgren, A.; Halzen, F.; Han,
   K.; Hanson, K.; Hardtke, D.; Hardtke, R.; Harenberg, T.; Hart, J. E.;
   Haugen, J.; Hauschildt, T.; Hays, D.; Heise, J.; Helbing, K.; Hellwig,
   M.; Herquet, P.; Hill, G. C.; Hodges, J.; Hoffman, K. D.; Hoshina, K.;
   Hubert, D.; Hughey, B.; Hulth, P. O.; Hultqvist, K.; Hundertmark, S.;
   Hülß, J. -P.; Ishihara, A.; Jacobsen, J.; Japaridze, G. S.; Jones,
   A.; Joseph, J. M.; Kampert, K. -H.; Karle, A.; Kawai, H.; Kelley,
   J. L.; Kestel, M.; Kitamura, N.; Klein, S. R.; Klepser, S.; Kohnen,
   G.; Kolanoski, H.; Köpke, L.; Krasberg, M.; Kuehn, K.; Landsman, H.;
   Laundrie, A.; Leich, H.; Liubarsky, I.; Lundberg, J.; MacKenzie, C.;
   Madsen, J.; Mase, K.; Matis, H. S.; McCauley, T.; McParland, C. P.;
   Meli, A.; Messarius, T.; Mészáros, P.; Miyamoto, H.; Mokhtarani,
   A.; Montaruli, T.; Morey, A.; Morse, R.; Movit, S. M.; Münich, K.;
   Muratas, A.; Nahnhauer, R.; Nam, J. W.; Nießen, P.; Nygren, D. R.;
   Ögelman, H.; Olbrechts, Ph.; Olivas, A.; Patton, S.; Peña-Garay,
   C.; Pérez de Los Heros, C.; Pettersen, C.; Piegsa, A.; Pieloth, D.;
   Pohl, A. C.; Porrata, R.; Pretz, J.; Price, P. B.; Przybylski, G. T.;
   Rawlins, K.; Razzaque, S.; Refflinghaus, F.; Resconi, E.; Rhode, W.;
   Ribordy, M.; Rizzo, A.; Robbins, S.; Rott, C.; Rutledge, D.; Sander,
   H. -G.; Sandstrom, P.; Sarkar, S.; Schlenstedt, S.; Schneider, D.;
   Seckel, D.; Seo, S. H.; Seunarine, S.; Silvestri, A.; Smith, A. J.;
   Solarz, M.; Song, C.; Sopher, J. E.; Spiczak, G. M.; Spiering, C.;
   Stamatikos, M.; Stanev, T.; Steffen, P.; Stezelberger, T.; Stokstad,
   R. G.; Stoufer, M. C.; Stoyanov, S.; Strahler, E. A.; Sulanke, K. -H.;
   Sullivan, G. W.; Taboada, I.; Tarasova, O.; Tepe, A.; Thollander,
   L.; Tilav, S.; Toale, P. A.; Turčan, D.; van Eijndhoven, N.;
   Vandenbroucke, J.; van Overloop, A.; Voigt, B.; Wagner, W.; Walck,
   C.; Waldmann, H.; Walter, M.; Wang, Y. -R.; Wendt, C.; Whitney, M.;
   Wiebusch, C. H.; Wikström, G.; Williams, D. R.; Wischnewski, R.;
   Wisniewski, P.; Wissing, H.; Woschnagg, K.; Xu, X. W.; Yodh, G.;
   Yoshida, S.; Zornoza, J. D.
2006APh....26..155I    Altcode: 2006astro.ph..4450T
  The first sensors of the IceCube neutrino observatory were deployed at
  the South Pole during the austral summer of 2004 2005 and have been
  producing data since February 2005. One string of 60 sensors buried
  in the ice and a surface array of eight ice Cherenkov tanks took data
  until December 2005 when deployment of the next set of strings and tanks
  began. We have analyzed these data, demonstrating that the performance
  of the system meets or exceeds design requirements. Times are determined
  across the whole array to a relative precision of better than 3 ns,
  allowing reconstruction of muon tracks and light bursts in the ice,
  of air-showers in the surface array and of events seen in coincidence
  by surface and deep-ice detectors separated by up to 2.5 km.

---------------------------------------------------------
Title: Limits on the muon flux from neutralino annihilations at the
    center of the Earth with AMANDA
Authors: Achterberg, A.; Ackermann, M.; Adams, J.; Ahrens, J.; Andeen,
   K.; Atlee, D. W.; Bahcall, J. N.; Bai, X.; Baret, B.; Bartelt, M.;
   Barwick, S. W.; Bay, R.; Beattie, K.; Becka, T.; Becker, J. K.;
   Becker, K. -H.; Berghaus, P.; Berley, D.; Bernardini, E.; Bertrand,
   D.; Besson, D. Z.; Blaufuss, E.; Boersma, D. J.; Bohm, C.; Böser,
   S.; Botner, O.; Bouchta, A.; Bouhali, O.; Braun, J.; Burgess,
   C.; Burgess, T.; Castermans, T.; Chirkin, D.; Clem, J.; Conrad,
   J.; Cooley, J.; Cowen, D. F.; D'Agostino, M. V.; Davour, A.; Day,
   C. T.; de Clercq, C.; Desiati, P.; De Young, T.; Diaz-Velez, J. C.;
   Dreyer, J.; Duvoort, M. R.; Edwards, W. R.; Ehrlich, R.; Ekström,
   P.; Ellsworth, R. W.; Evenson, P. A.; Fadiran, O.; Fazely, A. R.;
   Feser, T.; Filimonov, K.; Gaisser, T. K.; Gallagher, J.; Ganugapati,
   R.; Geenen, H.; Gerhardt, L.; Goldschmidt, A.; Goodman, J. A.;
   Gozzini, R.; Greene, M. G.; Grullon, S.; Groß, A.; Gunasingha,
   R. M.; Gurtner, M.; Hallgren, A.; Halzen, F.; Han, K.; Hanson, K.;
   Hardtke, D.; Hardtke, R.; Harenberg, T.; Hart, J. E.; Hauschildt,
   T.; Hays, D.; Heise, J.; Helbing, K.; Hellwig, M.; Herquet, P.; Hill,
   G. C.; Hodges, J.; Hoffman, K. D.; Hoshina, K.; Hubert, D.; Hughey,
   B.; Hulth, P. O.; Hultqvist, K.; Hundertmark, S.; Hülß, J. -P.;
   Ishihara, A.; Jacobsen, J.; Japaridze, G. S.; Jones, A.; Joseph,
   J. M.; Kampert, K. -H.; Karle, A.; Kawai, H.; Kelley, J. L.; Kestel,
   M.; Klein, S. R.; Klepser, S.; Kohnen, G.; Kolanoski, H.; Köpke,
   L.; Krasberg, M.; Kuehn, K.; Landsman, H.; Leich, H.; Leuthold, M.;
   Liubarsky, I.; Lundberg, J.; Madsen, J.; Marciniewski, P.; Mase, K.;
   Matis, H. S.; McCauley, T.; McParland, C. P.; Meli, A.; Messarius,
   T.; Mészáros, P.; Minaeva, Y.; Miočinović, P.; Miyamoto, H.;
   Mokhtarani, A.; Montaruli, T.; Morey, A.; Morse, R.; Movit, S. M.;
   Münich, K.; Nahnhauer, R.; Nam, J. W.; Neunhöffer, T.; Nießen, P.;
   Nygren, D. R.; Ögelman, H.; Olbrechts, Ph.; Olivas, A.; Patton, S.;
   Peña-Garay, C.; Pérez de Los Heros, C.; Piegsa, A.; Pieloth, D.;
   Pohl, A. C.; Porrata, R.; Pretz, J.; Price, P. B.; Przybylski, G. T.;
   Rawlins, K.; Razzaque, S.; Refflinghaus, F.; Resconi, E.; Rhode, W.;
   Ribordy, M.; Rizzo, A.; Robbins, S.; RodríGuez Martino, J.; Rott,
   C.; Rutledge, D.; Sander, H. -G.; Schlenstedt, S.; Schneider, D.;
   Schwarz, R.; Seckel, D.; Seo, S. H.; Seunarine, S.; Silvestri, A.;
   Smith, A. J.; Solarz, M.; Song, C.; Sopher, J. E.; Spiczak, G. M.;
   Spiering, C.; Stamatikos, M.; Stanev, T.; Steffen, P.; Stezelberger,
   T.; Stokstad, R. G.; Stoufer, M. C.; Stoyanov, S.; Strahler, E. A.;
   Sulanke, K. -H.; Sullivan, G. W.; Sumner, T. J.; Taboada, I.; Tarasova,
   O.; Tepe, A.; Thollander, L.; Tilav, S.; Toale, P. A.; Turčan, D.;
   van Eijndhoven, N.; Vandenbroucke, J.; Voigt, B.; Wagner, W.; Walck,
   C.; Waldmann, H.; Walter, M.; Wang, Y. -R.; Wendt, C.; Wiebusch,
   C. H.; Wikström, G.; Williams, D. R.; Wischnewski, R.; Wissing, H.;
   Woschnagg, K.; Xu, X. W.; Yodh, G.; Yoshida, S.; Zornoza, J. D.
2006APh....26..129A    Altcode:
  A search has been performed for nearly vertically upgoing
  neutrino-induced muons with the Antarctic Muon And Neutrino Detector
  Array (AMANDA), using data taken over the three year period 1997-99. No
  excess above the expected atmospheric neutrino background has been
  found. Upper limits at 90% confidence level have been set on the
  annihilation rate of neutralinos at the center of the Earth, as well
  as on the muon flux at AMANDA induced by neutrinos created by the
  annihilation products.

---------------------------------------------------------
Title: 10,000 Standard Solar Models: A Monte Carlo Simulation
Authors: Bahcall, John N.; Serenelli, Aldo M.; Basu, Sarbani
2006ApJS..165..400B    Altcode: 2005astro.ph.11337B
  We have evolved 10,000 solar models using 21 input parameters that are
  randomly drawn for each model from separate probability distributions
  for every parameter. We use the results of these models to determine the
  theoretical uncertainties in the predicted surface helium abundance,
  the profile of the sound speed versus radius, the profile of the
  density versus radius, the depth of the solar convective zone, the
  eight principal solar neutrino fluxes, and the fractions of nuclear
  reactions that occur in the CNO cycle or in the three branches of
  the p-p chains. We also determine the correlation coefficients of the
  neutrino fluxes for use in analysis of solar neutrino oscillations. Our
  calculations include the most accurate available input parameters,
  including radiative opacity, equation of state, and nuclear cross
  sections. We incorporate both the recently determined heavy element
  abundances recommended by Asplund et al. and the older (higher) heavy
  element abundances recommended by Grevesse &amp; Sauval. We present
  best estimates of many characteristics of the standard solar model
  for both sets of recommended heavy element compositions.

---------------------------------------------------------
Title: A Survey of z&gt;5.7 Quasars in the Sloan Digital Sky
    Survey. IV. Discovery of Seven Additional Quasars
Authors: Fan, Xiaohui; Strauss, Michael A.; Richards, Gordon
   T.; Hennawi, Joseph F.; Becker, Robert H.; White, Richard L.;
   Diamond-Stanic, Aleksandar M.; Donley, Jennifer L.; Jiang, Linhua; Kim,
   J. Serena; Vestergaard, Marianne; Young, Jason E.; Gunn, James E.;
   Lupton, Robert H.; Knapp, Gillian R.; Schneider, Donald P.; Brandt,
   W. N.; Bahcall, Neta A.; Barentine, J. C.; Brinkmann, J.; Brewington,
   Howard J.; Fukugita, Masataka; Harvanek, Michael; Kleinman, S. J.;
   Krzesinski, Jurek; Long, Dan; Neilsen, Eric H., Jr.; Nitta, Atsuko;
   Snedden, Stephanie A.; Voges, Wolfgang
2006AJ....131.1203F    Altcode: 2005astro.ph.12080F
  We present the discovery of seven quasars at z&gt;5.7, selected
  from ~2000 deg<SUP>2</SUP> of multicolor imaging data of the Sloan
  Digital Sky Survey. The new quasars have redshifts z from 5.79 to
  6.13. Five are selected as part of a complete flux-limited sample in
  the SDSS northern Galactic cap; two have larger photometric errors
  and are not part of the complete sample. One of the new quasars, SDSS
  J1335+3533 (z=5.93), exhibits no emission lines; the 3 σ limit on the
  rest-frame equivalent width of the Lyα+N V line is 5 Å. It is the
  highest redshift lineless quasar known and could be a gravitational
  lensed galaxy, a BL Lac object, or a new type of quasar. Two new z&gt;6
  quasars, SDSS 1250+3130 (z=6.13) and SDSS J1137+3549 (z=6.01), show deep
  Gunn-Peterson absorption gaps in Lyα. These gaps are narrower than
  the complete Gunn-Peterson absorption troughs observed among quasars
  at z&gt;6.2 and do not have complete Lyβ absorption. <P />Based on
  observations obtained with the Sloan Digital Sky Survey; the Apache
  Point Observatory's 3.5 m telescope, which is owned and operated by
  the Astrophysical Research Consortium; the MMT Observatory, a joint
  facility of the University of Arizona and the Smithsonian Institution;
  the University of Arizona's 2.3 m Bok Telescope; the Kitt Peak National
  Observatory's 4 m Mayall Telescope; the 6.5 m Walter Baade Telescope at
  the Las Campanas Observatory, a collaboration between the Observatories
  of the Carnegie Institution of Washington, the University of Arizona,
  Harvard University, the University of Michigan, and the Massachusetts
  Institute of Technology; and the W. M. Keck Observatory, which is
  operated as a scientific partnership among the California Institute of
  Technology, the University of California, and the National Aeronautics
  and Space Administration, and made possible by the generous financial
  support of the W. M. Keck Foundation. <P />This paper is dedicated to
  the memory of John N. Bahcall.

---------------------------------------------------------
Title: Stellar Energy Generation and Solar Neutrinos
Authors: Bahcall, John N.; Salpeter, Edwin E.
2006hbp..book..147B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: What Is the Neon Abundance of the Sun?
Authors: Bahcall, John N.; Basu, Sarbani; Serenelli, Aldo M.
2005ApJ...631.1281B    Altcode: 2005astro.ph..2563B
  We have evolved a series of 13 complete solar models that utilize
  different assumed heavy-element compositions. Models that are
  based upon the heavy-element abundances recently determined by
  Asplund and coworkers are inconsistent with helioseismological
  measurements. However, models in which the neon abundance is
  increased by 0.4-0.5 dex to logN(Ne)=8.29+/-0.05 [on the scale in which
  logN(H)=12] are consistent with the helioseismological measurements even
  though the other heavy-element abundances are in agreement with the
  determinations of Asplund et al. These results sharpen and strengthen
  an earlier study by Antia &amp; Basu. The predicted solar neutrino
  fluxes are affected by the uncertainties in the composition by less
  than their 1 σ theoretical uncertainties.

---------------------------------------------------------
Title: Mapping Globular Cluster Tidal Streams
Authors: Grillmair, Carl J.; Dionatos, Odysseas; Bahcall, John;
   Cutri, Roc; Geisler, Douglas; Gieren, Wolfgang; Grebel, Eva; Johnston,
   Kathryn; Majewski, Steven; Patterson, Richard; Reid, Neill; Spergel,
   David; Tremaine, Scott
2005noao.prop..111G    Altcode:
  The primary scientific goal of this program is to detect and map
  the tidal streams emanating from halo globular clusters. We propose
  to obtain moderately deep V and I imaging of the regions within 2°
  of the centers of five globular clusters with R_sun &lt; 50 kpc and
  with a high probability of having strong tidal tails. Given that
  these cold tidal streams are on essentially the same orbits as their
  parent clusters, they can be used to constrain both the formation and
  evolution of the Galactic halo as well as the present shape of the
  Galactic potential field. With follow-up spectroscopy to eliminate
  foreground contaminants, the stars in these tidal streams will be used
  to construct a high-priority target list for the Space Interferometry
  Mission (SIM). Proper motion measurements of these stars with SIM will
  enable us to tightly constrain the detailed, three-dimensional structure
  of the Galactic potential field from the Solar Circle out to 50 kpc.

---------------------------------------------------------
Title: How Do Uncertainties in the Surface Chemical Composition of
    the Sun Affect the Predicted Solar Neutrino Fluxes?
Authors: Bahcall, John N.; Serenelli, Aldo M.
2005ApJ...626..530B    Altcode: 2004astro.ph.12096B
  We show that uncertainties in the values of the surface heavy-element
  abundances of the Sun are the largest source of the theoretical
  uncertainty in calculating the p-p, pep, <SUP>8</SUP>B, <SUP>13</SUP>N,
  <SUP>15</SUP>O, and <SUP>17</SUP>F solar neutrino fluxes. Our results
  focus attention on the necessity of improving the measurement of
  heavy-element abundances, while at the same time reducing the estimated
  uncertainties in the predicted solar neutrino fluxes due to abundance
  errors. We evaluate for the first time the sensitivity (partial
  derivative) of each solar neutrino flux with respect to the surface
  abundance of each element. We then calculate the uncertainties in each
  neutrino flux using the preferred “conservative” (based on changes of
  measured values with time) and “optimistic” (current values) estimates
  for the uncertainties in the element abundances. The total conservative
  (optimistic) composition uncertainty in the predicted <SUP>8</SUP>B
  neutrino flux is 11.6% (5.0%) when sensitivities to individual element
  abundances are used. The traditional method that lumps all abundances
  into a single quantity (total heavy element-to-hydrogen ratio, Z/X)
  yields a larger uncertainty, 20%. The uncertainties in the carbon,
  oxygen, neon, silicon, sulphur, and iron abundances all make significant
  contributions to the uncertainties in calculating solar neutrino
  fluxes; the uncertainties of different elements are most important for
  different neutrino fluxes. The uncertainty in the iron abundance is
  the largest source of the estimated composition uncertainties of the
  important <SUP>7</SUP>Be and <SUP>8</SUP>B solar neutrinos. Carbon
  is the largest contributor to the uncertainty in the calculation of
  the p-p, <SUP>13</SUP>N, and <SUP>15</SUP>O neutrino fluxes. However,
  for all neutrino fluxes, several elements contribute comparable amounts
  to the total composition uncertainty.

---------------------------------------------------------
Title: Probing Galactic Dark Matter With SIM Observations of Tidal
    Tails
Authors: Majewski, S. R.; Bahcall, J. N.; Geisler, D.; Gieren,
   W.; Grebel, E. K.; Grillmair, C. J.; Johnston, K. V.; Law, D. R.;
   Patterson, R. J.; Polak, A. A.; Reid, I. N.; Spergel, D. N.; Sumi,
   T.; Tremaine, S.
2005AAS...206.1413M    Altcode: 2005BAAS...37..454M
  The nature of the dark matter that composes 90 Galaxy remains a profound
  mystery. Astronomical observations can provide crucial insight on this
  fundamental issue by probing the large-scale spatial distribution of
  dark matter, addressing, in particular, the following questions: Is dark
  matter in our Galaxy centrally concentrated and lumpy as predicted for
  cold dark matter (such as the lightest SUSY particles or axions) or is
  it more smoothly distributed and less lumpy? Is the overall shape of
  the dark matter halo oblate (Johnston, Law &amp; Majewski 2005, ApJ,
  619, 800), prolate (Helmi 2004, ApJ, 610, L97) or triaxial (Newberg
  &amp; Yanny 2004, AAS, 205, 142.04)? What is the total mass and extent
  of the Milky Way, and what is its corresponding role in the dynamics
  of the Local Group? We intend to tackle these questions directly,
  through observations of stars in objects whose dynamics reflect the
  large-scale Galactic potential: satellite galaxies, star clusters,
  and halo tidal streams. Measuring the motions of dynamical tracers
  in the outer Galaxy demands proper motions accurate to better than
  10 microarcsecond yr<SUP>-1</SUP> at magnitudes V &gt; 18. NASA's SIM
  PlanetQuest is the only currently planned mission that can provide such
  data. SIM observations of the well-mapped Sagittarius star stream will,
  in addition, provide a definitive determination of the rotation speed
  of the Sun, pinning down the scale of the Galactic rotation curve to
  constrain the mass distribution in the inner Milky Way. <P />Funded
  by NASA/JPL contract 1228235 for the Taking Measure of the Milky Way
  Key Project for SIM PlanetQuest.

---------------------------------------------------------
Title: New Solar Opacities, Abundances, Helioseismology, and
    Neutrino Fluxes
Authors: Bahcall, John N.; Serenelli, Aldo M.; Basu, Sarbani
2005ApJ...621L..85B    Altcode: 2004astro.ph.12440B
  We construct solar models with the newly calculated radiative
  opacities from the Opacity Project (OP) and with recently determined
  (lower) heavy-element abundances. We compare the results from the
  new models with the predictions of a series of models that use OPAL
  radiative opacities, older determinations of the surface heavy-element
  abundances, and refinements of nuclear reaction rates. For all the
  variations we consider, solar models that are constructed with the
  newer and lower heavy-element abundances advocated by Asplund et
  al. disagree by much more than the estimated measuring errors with the
  helioseismological determinations of the depth of the solar convective
  zone, the surface helium composition, the internal sound speeds, and
  the density profile. Using the new OP radiative opacities, the ratio of
  the <SUP>8</SUP>B neutrino flux calculated with the older and larger
  heavy-element abundances (or with the newer and lower heavy-element
  abundances) to the total neutrino flux measured by the Sudbury Neutrino
  Observatory is 1.09 (0.87) with a 9% experimental uncertainty and a 16%
  theoretical uncertainty, 1σ errors.

---------------------------------------------------------
Title: Neutrino Astronomy and Cosmic Rays at the South Pole:. Latest
    Results from AMANDA and Perspectives for Icecube
Authors: Desiati, Paolo; Achterberg, A.; Ackermann, M.; Ahrens, J.;
   Albrecht, H.; Atlee, D. W.; Bahcall, J. N.; Bai, X.; Bartelt, M.; Bay,
   R.; Barwick, S. W.; Becka, T.; Becker, K. H.; Becker, J. K.; Berghaus,
   P.; Bergmans, J.; Berley, D.; Bernardini, E.; Bertrand, D.; Besson,
   D. Z.; Blaufuss, E.; Boersma, D. J.; Bohm, C.; Böser, S.; Botner,
   O.; Bouchta, A.; Bouhali, O.; Braun, J.; Burgess, C.; Burgess, T.;
   Carithers, W.; Castermans, T.; Cavin, J.; Chinowsky, W.; Chirkin, D.;
   Clem, J.; Coarasa, J. A.; Collin, B.; Conrad, J.; Cooley, J.; Cowen,
   D. F.; Davour, A.; Day, C. T.; de Clercq, C.; De Young, T.; Edwards,
   W. R.; Ehrlich, R.; Ekström, P.; Ellsworth, R. W.; Evenson, P. A.;
   Fazely, A. R.; Feser, T.; Gaisser, T. K.; Gallagher, J.; Ganugapati,
   R.; Geenen, H.; Gerhardt, L.; Goldschmidt, A.; Gross, A.; Gunasingha,
   R. M.; Hallgren, A.; Halzen, F.; Hanson, K.; Hardtke, D.; Hardtke,
   R.; Harenberg, T.; Hauschildt, T.; Hays, D.; Helbing, K.; Hellwig,
   M.; Herquet, P.; Hill, G. C.; Hodges, J.; Hoshina, K.; Hubert, D.;
   Hughey, B.; Hulth, P. O.; Hultqvist, K.; Hundertmark, S.; Jacobsen,
   J.; Japaridze, G. S.; Jones, A.; Joseph, J. M.; Kampert, K. H.;
   Karle, A.; Kawai, H.; Kelley, J.; Kestel, M.; Kitamura, N.; Klein,
   S. R.; Koch, R.; Kohnen, G.; Köpke, L.; Kowalski, M.; Krasberg,
   M.; Kuehn, K.; Kujawski, E.; Langer, N.; Leich, H.; Leuthold, M.;
   Liubarsky, I.; Lundberg, J.; Madsen, J.; Mandli, K.; Marciniewski,
   P.; Matis, H. S.; McParland, C. P.; Messarius, T.; Mészáros, P.;
   Minaeva, Y.; Minor, R. H.; Miočinović, P.; Miyamoto, H.; Morse, R.;
   Münich, K.; Nahnhauer, R.; Nam, J. W.; Neunhöffer, T.; Niessen, P.;
   Nygren, D. R.; Ögelman, H.; Olbrechts, Ph.; Patton, S.; Paulos, R.;
   Peña-Garay, C.; Pérez de Los Heros, C.; Pohl, A. C.; Porrata, R.;
   Pretz, J.; Price, P. B.; Przybylski, G. T.; Rawlins, K.; Razzaque, S.;
   Resconi, E.; Rhode, W.; Ribordy, M.; Richter, S.; Rodríguez Martino,
   J.; Sander, H. G.; Schinarakis, K.; Schlenstedt, S.; Schneider, D.;
   Schwarz, R.; Seckel, D.; Seo, S. H.; Silvestri, A.; Smith, A. J.;
   Solarz, M.; Sopher, J. E.; Spiczak, G. M.; Spiering, C.; Stamatikos,
   M.; Stanev, T.; Steele, D.; Steffen, P.; Stezelberger, T.; Stokstad,
   R. G.; Stoyanov, S.; Straszheim, T. D.; Sulanke, K. H.; Sullivan,
   G. W.; Sumner, T. J.; Taboada, I.; Tarasova, O.; Thollander, L.; Tilav,
   S.; Turčan, D.; van Eijndhoven, N.; Vandenbroucke, J.; Voicu, L. C.;
   Wagner, W.; Walck, C.; Walter, M.; Wang, Y. R.; Wiebusch, C. H.;
   Wischnewski, R.; Wissing, H.; Woschnagg, K.; Yeck, J.; Yoshida, S.;
   Yodh, G.
2005IJMPA..20.6919D    Altcode:
  The AMANDA neutrino telescope has been in operation at the South Pole
  since 1996. The present final array configuration, operational since
  2000, consists of 677 photomultiplier tubes arranged in 19 strings,
  buried at depths between 1500 and 2000 m in the ice. The most recent
  results on a multi-year search for point sources of neutrinos will
  be shown. The study of events triggered in coincidence with the
  surface array SPASE and AMANDA provided a result on cosmic ray
  composition. Expected improvements from IceCube/IceTop will also
  be discussed.

---------------------------------------------------------
Title: Solar Models and Solar Neutrinos
Authors: Bahcall, J. N.
2005PhST..121...46B    Altcode: 2004hep.ph...12068B
  I provide a summary of the current theoretical knowledge of solar
  neutrino fluxes as derived from precise solar models.

---------------------------------------------------------
Title: Stellar Energy Generation and Solar Neutrinos
Authors: Bahcall, John N.; Salpeter, Edwin E.
2005PhT....58j..44B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Helioseismological Implications of Recent Solar Abundance
    Determinations
Authors: Bahcall, John N.; Basu, Sarbani; Pinsonneault, Marc;
   Serenelli, Aldo M.
2005ApJ...618.1049B    Altcode: 2004astro.ph..7060B
  We show that standard solar models are in good agreement with the
  helioseismologically determined sound speed and density as a function of
  solar radius, the depth of the convective zone, and the surface helium
  abundance, as long as those models do not incorporate the most recent
  heavy-element abundance determinations. However, sophisticated new
  analyses of the solar atmosphere infer lower abundances of the lighter
  metals (like C, N, O, Ne, and Ar) than the previously widely used
  surface abundances. We show that solar models that include the lower
  heavy-element abundances disagree with the solar profiles of sound speed
  and density as well as the depth of the convective zone and the helium
  abundance. The disagreements for models with the new abundances range
  from factors of several to many times the quoted uncertainties in the
  helioseismological measurements. The disagreements are at temperatures
  that are too low to affect significantly solar neutrino emission. If
  errors in the calculated OPAL opacities are solely responsible for the
  disagreements, then the corrections in the opacity must extend from
  2×10<SUP>6</SUP> K (R=0.7 R<SUB>solar</SUB>) to 5×10<SUP>6</SUP> K
  (R=0.4 R<SUB>solar</SUB>), with opacity increases of the order of 10%.

---------------------------------------------------------
Title: Solar Neutrinos: A Popular Account
Authors: Bahcall, John N.
2004physics..11190B    Altcode:
  This encyclopedia article addresses questions like the following. How
  does the Sun shine? Does the neutrino have a mass? Are there weak
  interactions beyond those described by the standard model of particle
  physics?

---------------------------------------------------------
Title: Helioseismological Implications of Recent Solar Abundance
    Determinations
Authors: Serenelli, A. M.; Bahcall, J. N.; Basu, S.; Pinsonneault,
   M. H.
2004ESASP.559..623S    Altcode: 2004soho...14..623S
  No abstract at ADS

---------------------------------------------------------
Title: How Accurately Can We Calculate the Depth of the Solar
    Convective Zone?
Authors: Bahcall, John N.; Serenelli, Aldo M.; Pinsonneault, Marc
2004ApJ...614..464B    Altcode: 2004astro.ph..3604B
  We evaluate the logarithmic derivative of the depth of the solar
  convective zone (CZ) with respect to the logarithm of the radiative
  opacity, ∂lnR<SUB>CZ</SUB>/∂lnκ. We use this expression to
  show that the radiative opacity near the base of the solar CZ
  must be known to an accuracy of +/-1% in order to calculate the
  CZ depth to the accuracy of the helioseismological measurement,
  R<SUB>CZ</SUB>=0.713+/-0.001 R<SUB>solar</SUB>. The radiative opacity
  near the base of the CZ that is obtained from OPAL tables must be
  increased by ~21% in the 2004 Bahcall-Pinsonneault solar model if
  one wants to invoke opacity errors in order to reconcile recent solar
  heavy abundance determinations with the helioseismological measurement
  of R<SUB>CZ</SUB>. We show that the radiative opacity near the base of
  the CZ depends sensitively on the assumed heavy-element mass fraction,
  Z. The uncertainty in the measured value of Z is currently the limiting
  factor in our ability to calculate the depth of the CZ. Different
  state-of-the-art interpolation schemes using the existing OPAL tables
  yield opacity values that differ by ~4%. We describe the finer grid
  spacings that are necessary to interpolate the radiative opacity to
  +/-1%. Uncertainties due to the equation of state do not significantly
  affect the calculated depth of the CZ.

---------------------------------------------------------
Title: Solar Neutrinos Before and After Neutrino 2004
Authors: Bahcall, John N.; Gonzalez-Garcia, M. C.; Pena-Garay, Carlos
2004JHEP...08..016B    Altcode: 2004hep.ph....6294B
  We compare, using a three neutrino analysis, the allowed neutrino
  oscillation parameters and solar neutrino fluxes determined by the
  experimental data available Before and After Neutrino 2004. New data
  available after Neutrino 2004 include refined KamLAND and gallium
  measurements. We use six different approaches to analyzing the KamLAND
  data. We present detailed results using all the available neutrino
  and anti-neutrino data for Deltam<SUP>2</SUP><SUB>21</SUB>, tan
  <SUP>2</SUP>theta<SUB>12</SUB>, sin <SUP>2</SUP>theta<SUB>13</SUB>,
  and sin <SUP>2</SUP>eta (sterile fraction). Using the same complete
  data sets, we also present Before and After determinations of all the
  solar neutrino fluxes (which are treated as free parameters), an upper
  limit to the luminosity fraction associated with CNO neutrinos, and
  the predicted rate for a <SUP>7</SUP>Be solar neutrino experiment. The
  1sigma (3sigma) allowed range of Deltam<SUP>2</SUP><SUB>21</SUB> =
  8.2<SUP>+0.3</SUP><SUB>-0.3</SUB>(<SUP>+1.0</SUP><SUB>-0.8</SUB>)
  × 10<SUP>-5</SUP> eV<SUP>2</SUP> is decreased by a factor of
  1.7 (5), but the allowed ranges of all other neutrino oscillation
  parameters and neutrino fluxes are not significantly changed. Maximal
  theta<SUB>12</SUB> mixing is disfavored at 5.8sigma and the bound
  on the mixing angle theta<SUB>13</SUB> is slightly improved to sin
  <SUP>2</SUP>theta<SUB>13</SUB>&lt;0.048 at 3sigma. The predicted
  rate in a <SUP>7</SUP>Be neutrino-electron scattering experiment is
  0.665+/-0.015 (<SUP>+0.045</SUP><SUB>-0.040</SUB>) of the rate implied
  by the BP04 solar model in the absence of neutrino oscillations. The
  corresponding predictions for p-p and pep experiments are, respectively,
  0.707<SUP>+0.011</SUP><SUB>-0.013</SUB>(<SUP>+0.041</SUP><SUB>-0.039</SUB>)
  and
  0.644<SUP>+0.011</SUP><SUB>-0.013</SUB>(<SUP>+0.045</SUP><SUB>-0.037</SUB>).
  In order to clarify what measurements constrain which parameters
  best, we also analyze the solar neutrino data separately and the
  reactor anti-neutrino data separately, both Before and After Neutrino
  2004. We derive upper limits to CPT violation in the weak sector by
  comparing reactor anti-neutrino oscillation parameters with neutrino
  oscillation parameters. We also show that the recent data disfavor at
  91% CL a proposed non-standard interaction description of solar neutrino
  oscillations. We have verified that our results are insensitive (changes
  much less than 1sigma) to which of six approaches we use in analyzing
  the KamLAND data, which of the published <SUP>8</SUP>B neutrino energy
  spectra we adopt, and the precise value of the gallium solar neutrino
  event rate.

---------------------------------------------------------
Title: What can we learn from neutrinoless double beta decay
    experiments?
Authors: Bahcall, John N.; Murayama, Hitoshi; Peña-Garay, C.
2004PhRvD..70c3012B    Altcode: 2004hep.ph....3167B
  We assess how well next-generation neutrinoless double beta decay and
  normal neutrino beta decay experiments can answer four fundamental
  questions. (1) If neutrinoless double beta decay searches do not detect
  a signal, and if the spectrum is known to be inverted hierarchy, can
  we conclude that neutrinos are Dirac particles? (2) If neutrinoless
  double beta decay searches are negative and a next-generation ordinary
  beta decay experiment detects the neutrino mass scale, can we conclude
  that neutrinos are Dirac particles? (3) If neutrinoless double beta
  decay is observed with a large neutrino mass element, what is the total
  mass in neutrinos? (4) If neutrinoless double beta decay is observed,
  but next-generation beta decay searches for a neutrino mass only set
  a mass upper limit, can we establish whether the mass hierarchy is
  normal or inverted? We base our answers on the expected performance
  of next-generation neutrinoless double beta decay experiments and on
  simulations of the accuracy of calculations of nuclear matrix elements.

---------------------------------------------------------
Title: Solving the Mystery of the Missing Neutrinos
Authors: Bahcall, John
2004physics...6040B    Altcode:
  The three years 2001 to 2003 were the golden years of solar neutrino
  research. In this period, scientists solved a mystery with which they
  had been struggling for four decades. The solution turned out to be
  important for both physics and for astronomy. In this article, I tell
  the story of those fabulous three years.

---------------------------------------------------------
Title: Solar models and solar neutrino oscillations
Authors: Bahcall, John N.; Peña-Garay, Carlos
2004NJPh....6...63B    Altcode: 2004hep.ph....4061B
  We provide a summary of the current knowledge, theoretical and
  experimental, of solar neutrino fluxes and of the masses and mixing
  angles that characterize solar neutrino oscillations. We also summarize
  the principal reasons for performing new solar neutrino experiments
  and what we anticipate from future studies.

---------------------------------------------------------
Title: Status of the IceCube Neutrino Observatory
Authors: Ahrens, J.; Bahcall, J. N.; Bai, X.; Bay, R. C.; Becka, T.;
   Becker, K. -H.; Berley, D.; Bernardini, E.; Bertrand, D.; Besson,
   D. Z.; Blaufuss, E.; Boersma, D. J.; Böser, S.; Bohm, C.; Botner, O.;
   Bouchta, A.; Bouhali, O.; Burgess, T.; Carithers, W.; Castermans, T.;
   Cavin, J.; Chinowsky, W.; Chirkin, D.; Collin, B.; Conrad, J.; Cooley,
   J.; Cowen, D. F.; Davour, A.; De Clercq, C.; DeYoung, T.; Desiati,
   P.; Ehrlich, R.; Ellsworth, R. W.; Evenson, P. A.; Fazely, A. R.;
   Feser, T.; Gaisser, T. K.; Gallagher, J.; Ganugapati, R.; Geenen,
   H.; Goldschmidt, A.; Goodman, J. A.; Gunasingha, R. M.; Hallgren,
   A.; Halzen, F.; Hanson, K.; Hardtke, R.; Hauschildt, T.; Hays, D.;
   Helbing, K.; Hellwig, M.; Herquet, P.; Hill, G. C.; Hubert, D.;
   Hughey, B.; Hulth, P. O.; Hultqvist, K.; Hundertmark, S.; Jacobsen,
   J.; Japaridze, G. S.; Jones, A.; Karle, A.; Kawai, H.; Kestel, M.;
   Kitamura, N.; Koch, R.; Köpke, L.; Kowalski, M.; Lamoureux, J. I.;
   Leich, H.; Liubarsky, I.; Madsen, J.; Matis, H. S.; McParland, C. P.;
   Messarius, T.; Mészáros, P.; Minaeva, Y.; Minor, R. H.; Miočinović,
   P.; Miyamoto, H.; Morse, R.; Nahnhauer, R.; Neunhöffer, T.; Niessen,
   P.; Nygren, D. R.; Ögelman, H.; Olbrechts, Ph; Patton, S.; Paulos,
   R.; Pérez de los Heros, C.; Pohl, A. C.; Pretz, J.; Price, P. B.;
   Przybylski, G. T.; Rawlins, K.; Razzaque, S.; Resconi, E.; Rhode,
   W.; Ribordy, M.; Richter, S.; Sander, H. -G.; Schinarakis, K.;
   Schlenstedt, S.; Schneider, D.; Schwarz, R.; Seckel, D.; Smith, A. J.;
   Solarz, M.; Spiczak, G. M.; Spiering, C.; Stamatikos, M.; Stanev, T.;
   Steele, D.; Steffen, P.; Stezelberger, T.; Stokstad, R. G.; Sulanke,
   K. -H.; Sullivan, G. W.; Sumner, T. J.; Taboada, I.; Tilav, S.;
   van Eijndhoven, N.; Wagner, W.; Walck, C.; Wang, R. -R.; Wiebusch,
   C. H.; Wiedemann, C.; Wischnewski, R.; Wissing, H.; Woschnagg, K.;
   Yoshida, S.; IceCube Collaboration
2004NewAR..48..519A    Altcode: 2004NewAR..48..519I
  The IceCube neutrino telescope, to be constructed near the Antarctic
  South Pole, represents the next generation of neutrino telescope. Its
  large 1 km <SUP>3</SUP> size will make it uniquely sensitive to the
  detection of neutrinos from astrophysical sources. The current design
  of the detector is presented. The basic performance of the detector
  and its ability to search for neutrinos from various astrophysical
  sources has been studied using detailed simulations and is discussed.

---------------------------------------------------------
Title: What Do We (Not) Know Theoretically about Solar Neutrino
    Fluxes?
Authors: Bahcall, John N.; Pinsonneault, M. H.
2004PhRvL..92l1301B    Altcode: 2004astro.ph..2114B
  Solar model predictions of <SUP>8</SUP>B and p-p neutrinos agree
  with the experimentally determined fluxes (including oscillations):
  φ(pp)<SUB>measured</SUB>=(1.02±00.02±0.01)φ(pp)<SUB>theory</SUB> and
  φ(<SUP>8</SUP>B)<SUB>measured</SUB>=(0.88±0.04±0.23)φ(<SUP>8</SUP>B)<SUB>theory</SUB>,
  1σ experimental and theoretical uncertainties, respectively. We
  use improved input data for nuclear fusion reactions, the
  equation of state, and the chemical composition of the Sun. The
  solar composition is the dominant uncertainty in calculating the
  <SUP>8</SUP>B and CNO neutrino fluxes; the cross section for the
  <SUP>3</SUP>He(<SUP>4</SUP>He,γ)<SUP>7</SUP>Be reaction is the most
  important uncertainty for the calculated <SUP>7</SUP>Be neutrino flux.

---------------------------------------------------------
Title: Sensitivity of the IceCube detector to astrophysical sources
    of high energy muon neutrinos
Authors: Ahrens, J.; Bahcall, J. N.; Bai, X.; Bay, R. C.; Becka, T.;
   Becker, K. -H.; Berley, D.; Bernardini, E.; Bertrand, D.; Besson,
   D. Z.; Biron, A.; Blaufuss, E.; Boersma, D. J.; Böser, S.; Bohm, C.;
   Botner, O.; Bouchta, A.; Bouhali, O.; Burgess, T.; Carithers, W.;
   Castermans, T.; Cavin, J.; Chinowsky, W.; Chirkin, D.; Collin, B.;
   Conrad, J.; Cooley, J.; Cowen, D. F.; Davour, A.; de Clercq, C.; De
   Young, T.; Desiati, P.; Ehrlich, R.; Ellsworth, R. W.; Evenson, P. A.;
   Fazely, A. R.; Feser, T.; Gaisser, T. K.; Gallagher, J.; Ganugapati,
   R.; Geenen, H.; Goldschmidt, A.; Goodman, J. A.; Gunasingha, R. M.;
   Hallgren, A.; Halzen, F.; Hanson, K.; Hardtke, R.; Hauschildt,
   T.; Hays, D.; Helbing, K.; Hellwig, M.; Herquet, P.; Hill, G. C.;
   Hubert, D.; Hughey, B.; Hulth, P. O.; Hultqvist, K.; Hundertmark,
   S.; Jacobsen, J.; Japaridze, G. S.; Jones, A.; Karle, A.; Kawai,
   H.; Kestel, M.; Kitamura, N.; Koch, R.; Köpke, L.; Kowalski, M.;
   Lamoureux, J. I.; Leich, H.; Leuthold, M.; Liubarsky, I.; Madsen,
   J.; Matis, H. S.; McParland, C. P.; Messarius, T.; Mészáros, P.;
   Minaeva, Y.; Minor, R. H.; Miočinović, P.; Miyamoto, H.; Morse, R.;
   Nahnhauer, R.; Neunhöffer, T.; Niessen, P.; Nygren, D. R.; Ögelman,
   H.; Olbrechts, Ph.; Patton, S.; Paulos, R.; Pérez de Los Heros, C.;
   Pohl, A. C.; Pretz, J.; Price, P. B.; Przybylski, G. T.; Rawlins, K.;
   Razzaque, S.; Resconi, E.; Rhode, W.; Ribordy, M.; Richter, S.; Sander,
   H. -G.; Schinarakis, K.; Schlenstedt, S.; Schmidt, T.; Schneider, D.;
   Schwarz, R.; Seckel, D.; Smith, A. J.; Solarz, M.; Spiczak, G. M.;
   Spiering, C.; Stamatikos, M.; Stanev, T.; Steele, D.; Steffen, P.;
   Stezelberger, T.; Stokstad, R. G.; Sulanke, K. -H.; Sullivan, G. W.;
   Sumner, T. J.; Taboada, I.; Tilav, S.; van Eijndhoven, N.; Wagner, W.;
   Walck, C.; Wang, R. -R.; Wiebusch, C. H.; Wiedemann, C.; Wischnewski,
   R.; Wissing, H.; Woschnagg, K.; Yoshida, S.
2004APh....20..507A    Altcode: 2003astro.ph..5196A; 2003astro.ph..5196T
  We present results of a Monte Carlo study of the sensitivity of
  the planned IceCube detector to predicted fluxes of muon neutrinos
  at TeV to PeV energies. A complete simulation of the detector and
  data analysis is used to study the detector's capability to search
  for muon neutrinos from potential sources such as active galaxies
  and gamma-ray bursts (GRBs). We study the effective area and the
  angular resolution of the detector as a function of muon energy
  and angle of incidence. We present detailed calculations of the
  sensitivity of the detector to both diffuse and pointlike neutrino
  fluxes, including an assessment of the sensitivity to neutrinos
  detected in coincidence with GRB observations. After three years
  of data taking, IceCube will be able to detect a point-source flux of
  E<SUB>ν</SUB><SUP>2</SUP>×dN<SUB>ν</SUB>/dE<SUB>ν</SUB>=7×10<SUP>-9</SUP>
  cm<SUP>-2</SUP>s<SUP>-1</SUP>GeV at a 5σ significance, or,
  in the absence of a signal, place a 90% c.l. limit at a level of
  E<SUB>ν</SUB><SUP>2</SUP>×dN<SUB>ν</SUB>/dE<SUB>ν</SUB>=2×10<SUP>-9</SUP>
  cm<SUP>-2</SUP>s<SUP>-1</SUP>GeV. A diffuse E<SUP>-2</SUP>
  flux would be detectable at a minimum strength of
  E<SUB>ν</SUB><SUP>2</SUP>×dN<SUB>ν</SUB>/dE<SUB>ν</SUB>=10<SUP>-8</SUP>
  cm<SUP>-2</SUP>s<SUP>-1</SUP>sr<SUP>-1</SUP>GeV. A GRB model following
  the formulation of Waxman and Bahcall would result in a 5σ effect
  after the observation of 200 bursts in coincidence with satellite
  observations of the gamma rays.

---------------------------------------------------------
Title: Distribution of Dark Matter in the Spiral Galaxy NGC 3198
Authors: van Albada, T. S.; Begeman, K.; Sanscisi, R.; Bahcall, J. N.
2004dmu..book....7V    Altcode:
  Two-component mass models, consisting of an exponential disk and
  a spherical halo, are constructed to fit a newly determined
  rotation curve of NGC 3198 that extends to 11 disk scale
  lengths. The amount of dark matter inside the last point of the
  rotation curve, at 30 kpc, is at least 4 times larger than the
  amount of visible matter, with (M/L<SUB>B</SUB>)<SUB>tot</SUB> =
  18M<SUB>⊙</SUB>/L<SUB>B⊙</SUB>. The maximum mass-to-light ratio
  for the disk is M/L<SUB>B</SUB> = 3.6. The available data cannot
  discriminate between disk models with low M/L and high M/L, but we
  present arguments which suggest that the true mass-to-light ratio
  of the disk is close to the maximum computed value. The core radius
  of the distribution of dark matter is found to satisfy 1.7 &lt;
  R<SUB>core</SUB> &lt; 12.5 kpc.

---------------------------------------------------------
Title: M Dwarfs from Hubble Space Telescope Star Counts. V. The
    I-Band Luminosity Function
Authors: Zheng, Zheng; Flynn, Chris; Gould, Andrew; Bahcall, John N.;
   Salim, Samir
2004ApJ...601..500Z    Altcode: 2003astro.ph..8359Z
  We derive the disk I-band luminosity function from the Zheng et
  al. sample of ~1400 disk M dwarfs observed with the Hubble Space
  Telescope. We adopt a Galactic-height-dependent color-magnitude relation
  to account for the metallicity gradient above the Galactic plane. The
  resultant I-band luminosity function peaks at M<SUB>I</SUB>~9.5 and
  drops sharply toward M<SUB>I</SUB>~10.5. <P />Based on observations with
  the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope
  Science Institute, which is operated by the Association of Universities
  for Research in Astronomy, Inc., under NASA contract NAS5-26555.

---------------------------------------------------------
Title: Dark Matter in the Universe (Second Edition) - 4th Jerusalem
    Winter School for Theoretical Physics Lectures
Authors: Bahcall, John; Piran, Tsvi; Weinberg, Steven
2004dmu..book.....B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Some Possible Regularities in Missing Mass
Authors: Bahcall, John N.; Casertano, Stefano
2004dmu..book...25B    Altcode:
  The unseen matter in a sample of spiral galaxies exhibits simple
  regularities and characteristic numerical values.

---------------------------------------------------------
Title: Introduction
Authors: Bahcall, John N.
2004dmu..book....1B    Altcode:
  Every so often in the history of physics a golden opportunity for
  great progress becomes apparent to contemporary physicists. In the
  twentieth century, enormous progress was made when, for example,
  the regularities of atomic spectra became apparent, when the Lamb
  shift was measured, and when the symmetries of supposedly elementary
  particles were recognized…

---------------------------------------------------------
Title: Does the Fine-Structure Constant Vary with Cosmological Epoch?
Authors: Bahcall, John N.; Steinhardt, Charles L.; Schlegel, David
2004ApJ...600..520B    Altcode: 2003astro.ph..1507B
  We use the strong nebular emission lines of O III,
  λλ5007 and 4959, to set a robust upper limit on the
  time dependence of the fine-structure constant. We find
  α<SUP>-1</SUP>dα(t)/dt&lt;2×10<SUP>-13</SUP> yr<SUP>-1</SUP>,
  corresponding to Δα/α(0)=(0.7+/-1.4)×10<SUP>-4</SUP> for
  quasars with 0.16&lt;z&lt;0.80 obtained from the SDSS Early Data
  Release. Using a blind analysis, we show that the upper limit given
  here is invariant with respect to 17 different ways of selecting the
  sample and analyzing the data. As a by-product, we show that the ratio
  of transition probabilities corresponding to the λλ5007 and 4959
  lines is 2.99+/-0.02, in good agreement with (but more accurate than)
  theoretical estimates. We compare and contrast the O III emission line
  method used here with the many-multiplet method that was used recently
  to suggest evidence for a time-dependent α. In an appendix we analyze
  the quasars from the recently available SDSS Data Release One sample
  and find Δα/α(0)=(1.2+/-0.7)×10<SUP>-4</SUP>.

---------------------------------------------------------
Title: Exploring Galactic Structure with the Fan Mountain Observatory
    Bench Spectrograph
Authors: Crane, J. D.; Majewski, S. R.; Patterson, R. J.; Bahcall,
   J. N.; Skrutskie, M. F.; Rhee, J.; Frinchaboy, P. M.
2003AAS...20311206C    Altcode: 2003BAAS...35.1384C
  The Bench Spectrograph at the University of Virginia's Fan Mountain
  Observatory has recently seen first light through the facility's
  primary research telescope, the 1-meter astrometric reflector. As a
  single-object, fiber-fed instrument with moderate resolution (5-10
  km s<SUP>-1</SUP>) capabilities, the spectrograph was motivated
  by several ongoing projects requiring stellar spectroscopy at the
  University of Virginia. The spectrograph was designed to supply moderate
  resolution Northern hemisphere spectra needed for the Grid Giant Star
  Survey (GGSS), which in addition to identifying candidates for the
  Astrometric Grid of NASA's Space Interferometry Mission (SIM), will
  provide a unique, unfilled all-sky catalog of low metallicity halo
  K giants that may be used to address a host of problems related to
  Galactic structure and kinematics. Because the GGSS candidate sample is
  extensive, bright (V&lt;13), and uniformly distributed over the sky,
  a fiber-fed design was selected to provide maximal spectral stability
  and uniformity while optimizing observing efficiency. The spectrograph
  will be useful for observing stars brighter than V ∼14 throughout
  the optical spectrum. The instrument will also be used to estimate the
  dark matter content of the local Galactic disk by measuring dynamically
  the local disk volume density (the “Oort limit”) reflected by the
  motions of a set of K giant “tracers” photometrically selected
  from a large-area survey of the North Galactic Pole. The Fan Mountain
  spectrograph will be used to refine our sample to the best possible
  homogeneity and to determine radial velocities. Once complete, this
  study should provide the largest and most reliable sample of dynamical
  “Oort limit” tracers assembled to date.

---------------------------------------------------------
Title: A road map to solar neutrino fluxes, neutrino oscillation
    parameters, and tests for new physics
Authors: Bahcall, John N.; Peña-Garay, Carlos
2003JHEP...11..004B    Altcode: 2003hep.ph....5159B
  We analyze all available solar and related reactor neutrino experiments,
  as well as simulated future <SUP>7</SUP>Be, p-p, and pep solar neutrino
  experiments. We treat all solar neutrino fluxes as free parameters
  subject to the condition that the total luminosity represented by
  the neutrinos equals the observed solar luminosity (the `luminosity
  constraint'). Existing experiments plus the luminosity constraint show
  that the p-p solar neutrino flux is 1.02+/-0.02 (1sigma) times the flux
  predicted by the BP00 standard solar model; the <SUP>7</SUP>Be neutrino
  flux is 0.93<SUP>+0.25</SUP><SUB>-0.63</SUB> the predicted flux;
  and the <SUP>8</SUP>B flux is 1.01+/-0.04 the predicted flux. The
  CNO fluxes are very poorly determined. The neutrino oscillation
  parameters are: Deltam<SUP>2</SUP> = 7.3<SUP>+0.4</SUP><SUB>-0.6</SUB>
  × 10<SUP>-5</SUP> eV<SUP>2</SUP> and tan <SUP>2</SUP>theta<SUB>12</SUB>
  = 0.41+/-0.04. We evaluate how accurate future experiments must
  be to determine more precisely neutrino oscillation parameters
  and solar neutrino fluxes, and to elucidate the transition from
  vacuum-dominated to matter-dominated oscillations at low energies. A
  future <SUP>7</SUP>Be nu-e scattering experiment accurate to +/-10% can
  reduce the uncertainty in the experimentally determined <SUP>7</SUP>Be
  neutrino flux by a factor of four and the uncertainty in the p-p
  neutrino flux by a factor of 2.5 (to +/-0.8%). A future p-p experiment
  must be accurate to better than +/-3% to shrink the uncertainty in tan
  <SUP>2</SUP>theta<SUB>12</SUB> by more than 15%. The idea that the Sun
  shines because of nuclear fusion reactions can be tested accurately by
  comparing the observed photon luminosity of the Sun with the luminosity
  inferred from measurements of solar neutrino fluxes. Based upon
  quantitative analyses of present and simulated future experiments, we
  answer the question: Why perform low-energy solar neutrino experiments?

---------------------------------------------------------
Title: Solar Models and Solar Neutrinos
Authors: Bahcall, John N.
2003phco.conf...31B    Altcode: 2003astro.ph.10030B
  I summarize 40 years of development of the standard solar model that
  is used to predict solar neutrino fluxes and then describe the current
  uncertainties in the predictions. I will also attempt to explain why
  it took so long, about three and a half decades, to reach a consensus
  view that new physics is being learned from solar neutrino experiments.

---------------------------------------------------------
Title: Does the Sun Shine by pp or CNO Fusion Reactions?
Authors: Bahcall, John N.; Gonzalez-Garcia, M. C.; Peña-Garay, Carlos
2003PhRvL..90m1301B    Altcode: 2002astro.ph.12331B
  We show that solar neutrino experiments set an upper limit of 7.8%
  (7.3% including the recent KamLAND measurements) to the fraction of
  energy that the Sun produces via the CNO fusion cycle, which is an
  order of magnitude improvement upon the previous limit. New experiments
  are required to detect CNO neutrinos corresponding to the 1.5% of the
  solar luminosity that the standard solar model predicts is generated
  by the CNO cycle.

---------------------------------------------------------
Title: IceCube - the next generation neutrino telescope at the
    South Pole
Authors: Karle, A.; Ahrens, J.; Bahcall, J. N.; Bai, X.; Becka, T.;
   Becker, K. -H.; Besson, D. Z.; Berley, D.; Bernardini, E.; Bertrand,
   D.; Binon, F.; Biron, A.; Böser, S.; Bohm, C.; Botner, O.; Bouhali,
   O.; Burgess, Th.; Castermans, T.; Chirkin, D.; Conrad, J.; Cooley, J.;
   Cowen, D. F.; Davour, A.; de Clercq, C.; De Young, T.; Desiati, P.;
   Dewulf, J. -P.; Dingus, B.; Ellsworth, R.; Evenson, P. A.; Fazely,
   A. R.; Feser, T.; Gaisser, T. K.; Gallagher, J.; Ganugapati, R.;
   Goldschmidt, A.; Goodman, J.; Hallgren, A.; Halzen, F.; Hanson,
   K.; Hardtke, R.; Hauschildt, T.; Hellwig, M.; Herquet, P.; Hill,
   G. C.; Hulth, P. O.; Hultgvist, K.; Hundertmark, S.; Jacobsen, J.;
   Japaridze, G. S.; Karle, A.; Köpke, L.; Kowalski, M.; Lamoureux,
   J. I.; Leich, H.; Leuthold, M.; Lindahl, P.; Liubarsky, I.; Madson,
   J.; Marciniewski, P.; Matis, H. S.; McParland, C. P.; Minaeva, Y.;
   Miočinović, P.; Morse, R.; Nahnhauer, R.; Neunhöffer, T.; Niessen,
   P.; Nygren, D. R.; Ogelman, H.; Olbrechts, Ph.; Pérez de Los Heros,
   C.; Pohl, A. C.; Price, P. B.; Przybylski, G. T.; Rawlins, K.; Resconi,
   E.; Rhode, W.; Ribordy, M.; Richter, S.; Sander, H. -G.; Schmidt, T.;
   Schneider, D.; Seckel, D.; Solarz, M.; Sparke, L.; Spiczak, G. M.;
   Spiering, C.; Stanev, T.; Steele, D.; Steffen, P.; Stokstad, R. G.;
   Sudhoff, P.; Sulanke, K. -H.; Sullivan, G. W.; Sumners, T.; Taboada,
   I.; Thollander, L.; Tilav, S.; Walck, C.; Weinheimer, C.; Wiebusch,
   C. H.; Wiedemann, Ch.; Wischnewski, R.; Wissing, H.; Woschnagg, K.;
   Yoshida, Sh.
2003NuPhS.118..388K    Altcode: 2002astro.ph..9556K
  IceCube is a large neutrino telescope of the next generation to be
  constructed in the Antarctic Ice Sheet near theSouth Pole. We present
  the conceptual design and the sensitivity of the IceCube detector to
  predicted fluxes of neutrinos, both atmospheric and extra-terrestrial. A
  complete simulation of the detector design has been used to study the
  detector's capability to search for neutrinos from sources such as
  active galaxies, and gamma-ray bursts.

---------------------------------------------------------
Title: Solar models: An historical overview
Authors: Bahcall, John N.
2003NuPhS.118...77B    Altcode: 2002astro.ph..9080B
  I will summarize in four slides the 40 years of development of the
  standard solar model that is used to predict solar neutrino fluxes
  and then describe the current uncertainties in the predictions. I will
  dispel the misconception that the p-p neutrino flux is determined by the
  solar luminosity and present a related formula that gives, in terms of
  the p-p and <SUP>7</SUP>Be neutrino fluxes, the ratio of the rates of
  the two primary ways of terminating the p-p fusion chain. I will also
  attempt to explain why it took so long, about three and a half decades,
  to reach a consensus view that new physics is being learned from solar
  neutrino experiments. Finally, I close with a personal confession.

---------------------------------------------------------
Title: Has the GZK suppression been discovered?
Authors: Bahcall, John N.; Waxman, Eli
2003PhLB..556....1B    Altcode: 2002hep.ph....6217B
  The energy spectra of ultra-high energy cosmic rays reported by the
  AGASA, Fly's Eye, Haverah Park, HiRes, and Yakutsk experiments are
  all shown to be in agreement with each other for energies below
  10<SUP>20</SUP> eV (after small adjustments, within the known
  uncertainties, of the absolute energy scales). The data from HiRes,
  Fly's Eye, and Yakutsk are consistent with the expected flux suppression
  above 5×10<SUP>19</SUP> eV due to interactions of cosmic rays with
  the cosmic microwave background, the Greisen-Zatsepin-Kuzmin (GZK)
  suppression, and are inconsistent with a smooth extrapolation of the
  observed cosmic-ray energy spectrum to energies &gt;5×10<SUP>19</SUP>
  eV. AGASA data show an excess of events above 10<SUP>20</SUP> eV,
  compared to the predicted GZK suppression and to the flux measured by
  the other experiments.

---------------------------------------------------------
Title: Solar Neutrinos Before and After KamLAND
Authors: Bahcall, John N.; Concepcion Gonzalez-Garcia, M.; na-Garay,
   Carlos Pe
2003JHEP...02..009B    Altcode: 2002hep.ph...12147B
  We use the recently reported KamLAND measurements on oscillations of
  reactor anti-neutrinos, together with the data of previously reported
  solar neutrino experiments, to show that: (1) the total 8B neutrino flux
  emitted by the Sun is 1.00(1.0 +/- 0.06) of the standard solar model
  (BP00) predicted flux, (2) the fraction of the 8B flux that is in the
  form of sterile neutrinos is 0.00<SUP>+0.09</SUP><SUB>-0.00</SUB>,
  (3) the KamLAND measurements reduce the area of the globally allowed
  oscillation regions that must be explored in model fitting by six orders
  of magnitude in the Deltam<SUP>2</SUP>-tan <SUP>2</SUP>theta plane,
  (4) LMA is now the unique oscillation solution to a CL of 4.7sigma,
  (5) maximal mixing is disfavored at 3.3 sigma, (6) active-sterile
  admixtures are constrained to sin <SUP>2</SUP>eta &lt; 0.13, and (7)
  non-standard solar models that were invented to completely avoid solar
  neutrino oscillations are excluded by KamLAND (KamLAND plus solar)
  at 3.6 (7.9) sigma. We also refine quantitative predictions for future
  7Be and p-p solar neutrino experiments.

---------------------------------------------------------
Title: Mapping Globular Cluster Tidal Streams
Authors: Grillmair, Carl J.; Bahcall, John; Geisler, Douglas; Gieren,
   Wolfgang; Grebel, Eva; Irwin, Michael; Johnston, Kathryn; Majewski,
   Steven; Patterson, Richard; Reid, Neill; Spergel, David; Tremaine,
   Scott
2003noao.prop..215G    Altcode:
  The primary scientific goal of this program is to detect and map
  the tidal streams emanating from halo globular clusters. We propose
  to obtain moderately deep V and I imaging of the regions within 2°
  of the centers of five globular clusters with R_sun &lt; 50 kpc and
  with a high probability of having strong tidal tails. Given that
  these cold tidal streams are on essentially the same orbits as their
  parent clusters, they can be used to constrain both the formation and
  evolution of the Galactic halo as well as the present shape of the
  Galactic potential field. With follow-up spectroscopy to eliminate
  foreground contaminants, the stars in these tidal streams will be used
  to construct a high-priority target list for the Space Interferometry
  Mission (SIM). Proper motion measurements of these stars with SIM will
  enable us to tightly constrain the detailed, three-dimensional structure
  of the Galactic potential field from the Solar Circle out to 50 kpc.

---------------------------------------------------------
Title: Solar models: structure, neutrinos, and helioseismological
    properties
Authors: Bahcall, J. N.; Basu, S.; Pinsonneault, M. H.
2003dysu.book....8B    Altcode:
  Solar models remain at the frontiers of two different scientific
  disciplines solar neutrino studies and helioseismology. After presenting
  the details of some state-of-the-art solar models, this chapter gives
  an overview of solar neutrino physics in some detail. The neutrino
  predictions from the set of solar models discussed have been contrasted
  with the results of the solar neutrino experiments. Finally, the
  structure of the solar models are compared with helioseismic results
  obtained using different data sets.

---------------------------------------------------------
Title: Astrophysical Neutrinos:. 20&lt;LC&gt;th&lt;/LC&gt; Century
    and Beyond
Authors: Bahcall, J. N.
2002nmgm.meet..190B    Altcode:
  I summarize the first four decades of solar neutrino research and
  suggest what may be possible to learn with extragalactic neutrinos
  and with solar neutrinos in the next decade.

---------------------------------------------------------
Title: The Birth of the HST Snapshot Programs
Authors: Bahcall, John N.
2002astro.ph.11193B    Altcode:
  This article describes the unconventional and occassionally stormy
  birth and early history of the HST Snapshot Program.

---------------------------------------------------------
Title: If sterile neutrinos exist, how can one determine the total
    solar neutrino fluxes?
Authors: Bahcall, John N.; Gonzalez-Garcia, M. C.; Peña-Garay, C.
2002PhRvC..66c5802B    Altcode: 2002hep.ph....4194B
  The <SUP>8</SUP>B solar neutrino flux inferred from a global analysis
  of solar neutrino experiments is within 11% (1σ) of the predicted
  standard solar model value if only active neutrinos exist, but could
  be as large as 1.7 times the standard prediction if sterile neutrinos
  exist. We show that the total <SUP>8</SUP>B neutrino flux (active
  plus sterile neutrinos) can be determined experimentally to about 10%
  (1σ) by combining charged current measurements made with the KamLAND
  reactor experiment and with the SNO CC solar neutrino experiment,
  provided the LMA neutrino oscillation solution is correct and the
  simulated performance of KamLAND is valid. Including also SNO NC
  data, the sterile component of the <SUP>8</SUP>B neutrino flux can
  be measured by this method to an accuracy of about 12% (1σ) of the
  standard solar model flux. Combining Super-Kamiokande and KamLAND
  measurements and assuming the oscillations occur only among active
  neutrinos, the <SUP>8</SUP>B neutrino flux can be measured to 6% (1σ)
  the total flux can be measured to an accuracy of about 9%. The total
  <SUP>7</SUP>Be solar neutrino flux can be determined to an accuracy
  of about 28% (1σ) by combining measurements made with the KamLAND,
  SNO, and gallium neutrino experiments. One can determine the total
  <SUP>7</SUP>Be neutrino flux to a 1σ accuracy of about 11% or better
  by comparing data from the KamLAND experiment and the BOREXINO solar
  neutrino experiment provided both detectors work as expected. The
  pp neutrino flux can be determined to about 15% using data from the
  gallium, KamLAND, BOREXINO, and SNO experiments.

---------------------------------------------------------
Title: Before and After: How has the SNO NC measurement changed
    things?
Authors: Bahcall, John N.; Gonzalez-Garcia, Concepción M.; Pena-Garay,
   Carlos
2002JHEP...07..054B    Altcode: 2002hep.ph....4314B
  We present `Before and After' global oscillation solutions, as well as
  predicted `Before and After' values and ranges for ten future solar
  neutrino observables (for BOREXINO, KamLAND, SNO, and a generic p-p
  neutrino detector). The `Before' case includes all solar neutrino data
  (and some theoretical improvements) available prior to April 20, 2002
  and the `After' case includes, in addition, the new SNO data on the
  CC, NC, and day-night asymmetry. We have performed global analyses
  using the full SNO day-night energy spectrum and, alternatively,
  using just the SNO NC and CC rates and the day-night asymmetry. The
  LMA solution is the only currently allowed MSW oscillation solution
  at ~ 99% CL. The LOW solution is allowed only at more than 2.5sigma,
  SMA is now excluded at 3.7sigma or 4.7sigma depending upon analysis
  strategy, and pure sterile oscillations are excluded at more than
  4.7sigma. Small mixing angles are `out' (pure sterile is `way out');
  MSW with large mixing angles is definitely `in'. Vacuum oscillations
  are allowed at 3sigma, but not at 2sigma. Precise maximal mixing is
  excluded at 3.2sigma for MSW solutions and at more than 2.8sigma for
  vacuum solutions. Most of the predicted values for future observables
  for the BOREXINO, KamLAND, and future SNO measurements are changed only
  by minor amounts by the inclusion of the recent SNO data. In order to
  test the robustness of the allowed neutrino oscillation regions that
  are inferred from the measurements and the predicted values for future
  solar neutrino observables, we have carried out calculations using a
  variety of strategies for analyzing the SNO and other experimental data.

---------------------------------------------------------
Title: Erratum: The Salpeter plasma corrections for solar fusion
    reactions
Authors: Bahcall, J. N.; Brown, L. S.; Gruzinov, A.; Sawyer, R. F.
2002A&A...388..660B    Altcode:
  In the paper by Bahcall, J. N., Brown, L. S., Gruzinov, A., &amp;
  Sawyer, R. F. 2002, A&amp;A, 383, 291, the paper by Weiss, A.,
  Fleiskamp, M., &amp; Tsytovich, N. 2001, A&amp;A, 371, 1123 was wrongly
  cited as suggesting a modification of the Salpeter formula for screening
  of nuclear reactions. The main point of the paper by Weiss et al. was
  actually to show that significant deviations from the Salpeter formula
  are strongly disfavored by helioseismology measurements.

---------------------------------------------------------
Title: How accurately can one test CPT conservation with reactor
    and solar neutrino experiments?
Authors: Bahcall, John N.; Barger, V.; Marfatia, Danny
2002PhLB..534..120B    Altcode: 2002hep.ph....1211B
  We show that the combined data from solar neutrino experiments and
  from the KamLAND reactor neutrino experiment can establish an upper
  limit on, or detect, potential CPT violation in the neutrino sector
  of order 10<SUP>-20</SUP> to 10<SUP>-21</SUP> GeV.

---------------------------------------------------------
Title: Robust signatures of solar neutrino oscillation solutions
Authors: Bahcall, John N.; Concepcion Gonzalez-Garcia, M.; Peña-Garay,
   Carlos
2002JHEP...04..007B    Altcode: 2001hep.ph...11150B
  With the goal of identifying signatures that select specific neutrino
  oscillation parameters, we test the robustness of global oscillation
  solutions that fit all the available solar and reactor experimental
  data. We use three global analysis strategies previously applied
  by different authors and also determine the sensitivity of the
  oscillation solutions to the critical nuclear fusion cross section,
  S<SUB>17</SUB>(0), for the production of <SUP>8</SUP>B. Our standard
  results make use of the precise new measurement of S<SUB>17</SUB>(0)
  by Junghans et al. The globally favored solutions are, in order of
  goodness of fit: LMA (the only solution at 2sigma), LOW, and VAC. The
  NC to CC ratio for SNO is predicted by the standard global analysis
  to be 3.45<SUP>+0.70</SUP><SUB>-0.54</SUB>(1sigma) which is separated
  from the no-oscillation value of 1.0 by much more than the expected
  experimental error. The predicted range of the day-night difference in
  CC rates is 8.3<SUP>+5.0</SUP><SUB>-5.6</SUB>(1sigma)%. A measurement
  by SNO of either a NC to CC ratio &gt; 3.3 or a day-night difference
  &gt;10%, would favor a small region of the currently allowed LMA
  neutrino parameter space. The global oscillation solution predicts
  a <SUP>7</SUP>Be neutrino-electron scattering rate in BOREXINO and
  KamLAND in the range 0.65<SUP>+0.04</SUP><SUB>-0.03</SUB>(1sigma) of
  the BP00 standard solar model rate, a prediction which can be used to
  test both the solar model and the neutrino oscillation theory. Only
  the LOW solution predicts a large day-night effect (leq 42%, 3sigma)
  in BOREXINO and KamLAND. For the reactor KamLAND experiment, the LMA
  solution predicts a charged current rate relative to the standard model
  of 0.44<SUP>+0.22</SUP><SUB>-0.07</SUB>(1sigma), E<SUB>threshold</SUB>
  = 1.22 MeV. We have also evaluated the effects of including preliminary
  Super-Kamiokande data for 1496 days of observations.

---------------------------------------------------------
Title: Measuring Local Dark Matter with K giants at the North
    Galactic Pole
Authors: Crane, Jeffrey D.; Majewski, Steven R.; Bahcall, John N.;
   Patterson, Richard J.
2002noao.prop..302C    Altcode:
  Local dark matter can be studied by measuring dynamically the local
  Galactic disk volume density (the “Oort limit” and comparing it to the
  volume density one gets by adding up local visible mass components. This
  is typically done by measuring the density and dynamics of a sample
  of “tracer” stars toward the Galactic poles. Using a variety of
  tracers and techniques, many such studies have been done, but with
  disparate results suggesting everything from no dark matter in the
  disk to more dark than visible matter. The construction of a large,
  uniform, and systematically well-measured tracer sample is a crucial
  part of this method. We have used Washington + DDO photometry to
  select a large sample of subsolar metallicity K giants at the North
  Galactic Pole. This proposal concerns the collection of spectroscopic
  data to refine our sample to the best possible homogeneity to minimize
  distance errors and to determine radial velocities. Once complete, this
  study should provide the largest and most reliable sample of dynamical
  “Oort limit” tracers yet assembled. As a result, we expect to place
  the strongest constraints yet on the density and scale height of dark
  matter in the disk. In the future, this same sample will be used in a
  Space Interferometry Mission Key Project study of the Oort limit which
  will refine our ground-based result by supplying transverse motions that
  can be incorporated into a 3-dimensional analysis of the potential and
  account for off-diagonal elements of the velocity correlation tensor,
  as well as provide extremely good trigonometric parallaxes.

---------------------------------------------------------
Title: The luminosity constraint on solar neutrino fluxes
Authors: Bahcall, John N.
2002PhRvC..65b5801B    Altcode: 2001hep.ph....8148B
  A specific linear combination of the total solar neutrino fluxes must
  equal the measured solar photon luminosity if nuclear fusion reactions
  among light elements are responsible for solar energy generation. This
  luminosity constraint, previously used in a limited form in testing
  the no neutrino oscillation hypothesis, is derived in a generality
  that includes all of the relevant solar neutrino fluxes and which is
  suitable for analyzing the results of many different solar neutrino
  experiments. With or without allowing for neutrino oscillations,
  the generalized luminosity constraint can be used in future analyses
  of solar neutrino data. Accurate numerical values for the linear
  coefficients are provided.

---------------------------------------------------------
Title: The Salpeter plasma correction for solar fusion reactions
Authors: Bahcall, J. N.; Brown, L. S.; Gruzinov, A.; Sawyer, R. F.
2002A&A...383..291B    Altcode: 2000astro.ph.10055B
  We describe five different ways of obtaining the Salpeter formula for
  the plasma corrections to fusion rates; this formula is valid at the
  center of the sun with insignificant errors ( ~ percent). Several
  recent papers have obtained a variety of answers in conflict with
  this result. We analyse the arguments of these papers, identifying
  sources of the discrepancies in some cases, and pointing out internal
  inconsistencies in the arguments given in other cases.

---------------------------------------------------------
Title: Astrophysical Neutrinos
Authors: Bahcall, J. N.
2002IJMPA..17S...6B    Altcode: 2002IJMPA..17....6B
  I summarize the first four decades of solar neutrino research and
  suggest what may be possible to learn with extragalactic neutrinos
  and with solar neutrinos in the next decade.

---------------------------------------------------------
Title: Taking Measure of the Milky Way
Authors: Majewski, Steven R.; Bahcall, John N.; Geisler, Douglas;
   Gieren, Wolfgang; Grebel, Eva; Grillmair, Carl; Irwin, Michael;
   Johnston, Kathryn V.; Patterson, Richard J.; Reid, Neill I.; Spergel,
   David; Tremaine, Scott
2002swsi.conf...15M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Neutrinos: An Overview
Authors: Bahcall, J. N.
2002cocm.book...37B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Astrophysical Neutrinos: 20th Century and Beyond
Authors: Bahcall, J. N.
2002spod.conf....6B    Altcode:
  I summarize the first four decades of solar neutrino research and
  suggest what may be possible to learn with extragalactic neutrinos
  and with solar neutrinos in the next decade.

---------------------------------------------------------
Title: How many σ's is the solar neutrino effect?
Authors: Bahcall, John N.
2001PhRvC..65a5802B    Altcode: 2001hep.ph....8147B; 2002PhRvC..65a5802B
  The minimal standard electroweak model can be tested by allowing all
  the solar neutrino fluxes, with undistorted energy spectra, to be free
  parameters in fitting the measured solar neutrino event rates, subject
  only to the condition that the total observed luminosity of the Sun be
  produced by nuclear fusion. The rates of the five experiments prior to
  SNO (chlorine, Kamiokande, SAGE, GALLEX, Super-Kamiokande) cannot be fit
  by an arbitrary choice of undistorted neutrino fluxes at the level of
  2.5σ (formally 99% C.L.). Considering just SNO and Super-Kamiokande,
  the discrepancy is at the 3.3σ level (10<SUP>-3</SUP> C.L.). If
  all six experiments are fit simultaneously, the formal discrepancy
  increases to 4σ (7×10<SUP>-5</SUP> C.L.). If the relative scaling in
  temperature of the nuclear reactions that produce <SUP>7</SUP>Be and
  <SUP>8</SUP>B neutrinos is taken into account, the formal discrepancy
  is at the 7.4σ level.

---------------------------------------------------------
Title: How the Sun Shines
Authors: Bahcall, John
2001Mercu..30e..30B    Altcode:
  After nearly two centuries of debate, recent neutrino experiments have
  solidified our understanding of solar energy production.

---------------------------------------------------------
Title: Global analysis of solar neutrino oscillations including SNO
    CC measurement
Authors: Bahcall, John N.; Concha Gonzalez-Garcia, M.; Peña-Garay,
   Carlos
2001JHEP...08..014B    Altcode: 2001hep.ph....6258B
  For active and sterile neutrinos, we present the globally allowed
  solutions for two neutrino oscillations. We include the SNO CC
  measurement and all other relevant solar neutrino and reactor
  data. Five active neutrino oscillation solutions (LMA, LOW, SMA,
  VAC, and Just So<SUP>2</SUP>) are currently allowed at 3sigma; three
  sterile neutrino solutions (Just So<SUP>2</SUP>, SMA, and VAC) are
  allowed at 3sigma. The goodness of fit is satisfactory for all eight
  solutions. We also investigate the robustness of the allowed solutions
  by carrying out global analyses with and without: 1) imposing solar
  model constraints on the <SUP>8</SUP>B neutrino flux, 2) including
  the Super-Kamiokande spectral energy distribution and day-night data,
  3) including a continuous mixture of active and sterile neutrinos,
  4) using an enhanced CC cross section for deuterium (due to radiative
  corrections), and 5) an optimistic, hypothetical reduction by a factor
  of three of the error of the SNO CC rate. For every analysis strategy
  used in this paper, the most favored solutions all involve large mixing
  angles: LMA, LOW, or VAC. The favored solutions are robust, but the
  existence at 3sigma of individual sterile solutions and the active
  Just So<SUP>2</SUP> solution is sensitive to the analysis assumptions.

---------------------------------------------------------
Title: M Dwarfs from Hubble Space Telescope Star Counts. IV.
Authors: Zheng, Zheng; Flynn, Chris; Gould, Andrew; Bahcall, John N.;
   Salim, Samir
2001ApJ...555..393Z    Altcode: 2001astro.ph..2442Z
  We study a sample of about 1400 disk M dwarfs that are found in
  148 fields observed with the Wide Field Camera 2 (WFC2) on the
  Hubble Space Telescope and 162 fields observed with pre-repair
  Planetary Camera 1 (PC1), of which 95 of the WFC2 fields are newly
  analyzed. The method of maximum likelihood is applied to derive the
  luminosity function and the Galactic disk parameters. At first,
  we use a local color-magnitude relation and a locally determined
  mass-luminosity relation in our analysis. The results are consistent
  with those of previous work but with considerably reduced statistical
  errors. These small statistical errors motivate us to investigate
  the systematic uncertainties. Considering the metallicity gradient
  above the Galactic plane, we introduce a modified color-magnitude
  relation that is a function of Galactic height. The resultant M
  dwarf luminosity function has a shape similar to that derived using
  the local color-magnitude relation but with a higher peak value. The
  peak occurs at M<SUB>V</SUB>~12, and the luminosity function drops
  sharply toward M<SUB>V</SUB>~14. We then apply a height-dependent
  mass-luminosity function interpolated from theoretical models with
  different metallicities to calculate the mass function. Unlike the mass
  function obtained using local relations, which has a power-law index
  α=0.47, the one derived from the height-dependent relations tends
  to be flat (α=-0.10). The resultant local surface density of disk
  M dwarfs (12.2+/-1.6 M<SUB>solar</SUB> pc<SUP>-2</SUP>) is somewhat
  smaller than the one obtained using local relations (14.3+/-1.3
  M<SUB>solar</SUB> pc<SUP>-2</SUP>). Our measurement favors a short
  disk scale length, H=2.75+/-0.16 (statistical)+/-0.25 (systematic)
  kpc. Based on observations with the NASA/ESA Hubble Space Telescope,
  obtained at the Space Telescope Science Institute, which is operated
  by the Association of Universities for Research in Astronomy, Inc.,
  under NASA contract NAS5-26555.

---------------------------------------------------------
Title: Solar Models: Current Epoch and Time Dependences, Neutrinos,
    and Helioseismological Properties
Authors: Bahcall, John N.; Pinsonneault, M. H.; Basu, Sarbani
2001ApJ...555..990B    Altcode: 2000astro.ph.10346B
  We calculate accurate solar models and report the detailed time
  dependences of important solar quantities. We use helioseismology
  to constrain the luminosity evolution of the Sun and report the
  discovery of semiconvection in evolved solar models that include
  diffusion. In addition, we compare the computed sound speeds with
  the results of p-mode observations by BiSON, GOLF, GONG, LOWL, and
  MDI instruments. We contrast the neutrino predictions from a set
  of eight standard-like solar models and four deviant (or deficient)
  solar models with the results of solar neutrino experiments. For solar
  neutrino and helioseismological applications, we present present-epoch
  numerical tabulations of characteristics of the standard solar model
  as a function of solar radius, including the principal physical and
  composition variables, sound speeds, neutrino fluxes, and functions
  needed for calculating solar neutrino oscillations.

---------------------------------------------------------
Title: High-energy physics: Neutrinos reveal split personalities
Authors: Bahcall, John N.
2001Natur.412...29B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: High energy astrophysical neutrinos: The upper bound is robust
Authors: Bahcall, John; Waxman, Eli
2001PhRvD..64b3002B    Altcode: 1999hep.ph....2383B
  We elucidate the physical basis for the upper bound on high energy
  neutrino fluxes implied by the observed cosmic ray flux. We stress that
  the bound is valid for neutrinos produced either by p,γ reactions
  or by p-p(n) reactions in sources which are optically thin for high
  energy protons to photo-meson and nucleon-meson interactions. We show
  that the upper bound is robust and conservative. The Waxman-Bahcall
  bound overestimates the most likely neutrino flux by a factor ~5/τ,
  for small optical depths τ. The upper limit cannot be plausibly evaded
  by invoking magnetic fields, optically thick active galactic nuclei
  (AGNs), or large hidden fluxes of extragalactic protons. We describe
  the implications of the bound for future experiments including the
  AMANDA, ANTARES, Auger, ICECUBE, NESTOR, and OWL/AIRWATCH detectors.

---------------------------------------------------------
Title: Astrophysical neutrinos
Authors: Bahcall, J. N.
2001NuPhS.100....5B    Altcode:
  I summarize the first four decades of solar neutrino research and
  suggest what may be possible to learn with extragalactic neutrinos
  and with solar neutrinos in the next decade.

---------------------------------------------------------
Title: Solar neutrinos: global analysis and implications for SNO
Authors: Bahcall, John N.; Krastev, Plamen I.; Smirnov, Alexei Yu.
2001JHEP...05..015B    Altcode: 2001hep.ph....3179B
  We present a global analysis of all the available solar neutrino data
  treating consistently the <SUP>8</SUP>B and hep neutrino fluxes as free
  parameters. The analysis reveals at 99.7% C.L. eight currently-allowed
  discrete regions in two-neutrino oscillation space, five regions
  corresponding to active neutrinos and three corresponding to sterile
  neutrinos. Most of the allowed oscillation solutions are robust with
  respect to changes in the analysis procedures, but the traditional
  vacuum solution is fragile. The globally-permitted range of the
  <SUP>8</SUP>B neutrino flux, 0.45 to 1.95 in units of the BP2000
  flux, is comparable to the 3sigma range allowed by the standard
  solar model. We discuss the implications for SNO of a low mass,
  Deltam<SUP>2</SUP> ~ 6 × 10<SUP>-12</SUP> eV<SUP>2</SUP>, vacuum
  oscillation solution, previously found by Raghavan, and by Krastev and
  Petcov, but absent in recent analyses that included Super-Kamiokande
  data. For the SNO experiment, we present refined predictions for
  the charged-current rate and the ratio of the neutral-current rate
  to charged-current rate. The predicted charged-current rate can be
  clearly distinguished from the no-oscillation rate only for the
  LMA solution. The predicted ratio of the neutral-current rate to
  charged-current rate is distinguishable from the no-oscillation ratio
  for the LMA, SMA, LOW, and VAC solutions for active neutrinos.

---------------------------------------------------------
Title: Taking Measure of the Milky Way
Authors: Majewski, S. R.; Bahcall, J. N.; Geisler, D.; Gieren, W.;
   Grebel, E. K.; Grillmair, C.; Irwin, M.; Johnston, K. V.; Patterson,
   R. J.; Reid, I. N.; Spergel, D.; Tremaine, S.
2001AAS...198.6213M    Altcode: 2001BAAS...33..879M
  We plan to undertake fundamental measurements of the gravitational
  potential (mass distribution) and dynamical structure of the Milky Way
  using the Space Interferometry Mission (SIM). Among our goals will be:
  1. The determination of two fundamental parameters that play a central
  role in virtually every problem in Galactic astronomy, namely (a) the
  solar distance to the center of the Milky Way (b) the solar angular
  velocity around the Galactic center 2. The measurement of fundamental
  dynamical properties of the Milky Way, among them (a) the pattern speed
  of the central bar (b) the rotation field and velocity-dispersion
  tensor in the disk (c) the kinematics (mean rotational velocity and
  velocity dispersion tensor) of the halo as a function of position
  3. The definition of the mass distribution of the Galaxy, which is
  dominated by the presence of dark matter. We intend to measure (a)
  the relative contribution of the disk and halo to the gravitational
  potential (b) local volume and surface mass density of the disk (c)
  the shape, mass and extent of the dark halo of the Milky Way out to
  250 kpc We will take advantage of the data already being obtained for
  sub-solar metallicity K giants in the SIM Astrometric Grid. These data
  will be supplemented by SIM observations of other targets, among them:
  (1) counterparts to the Astrometric Grid stars at greater distances,(2)
  a sample of disk Mira and Cepheid variables, (3) a sample of disk
  open clusters with a well-defined and restricted age range, (4) the
  brightest few stars in every Galactic globular cluster and satellite
  dwarf galaxy, and (5) stars in tidal tails of disrupted satellite
  galaxies and globular clusters. In addition, we intend to address
  the wealth of information these data will yield on Galactic stellar
  populations and the insight they will provide into the formation history
  of the Milky Way. Therefore, we intend to supplement the astrometric
  data with ground-based observations of abundances, radial velocities,
  and other properties, to maximize the benefits of the SIM data for
  analyses of stellar populations.

---------------------------------------------------------
Title: Astrophysical Neutrinos:. 20th Century and Beyond
Authors: Bahcall, J. N.
2001neph.conf...56B    Altcode:
  I summarize the first four decades of solar neutrino research and
  suggest what may be possible to learn with extragalactic neutrinos
  and with solar neutrinos in the next decade.

---------------------------------------------------------
Title: Neutrino Physics Its Impact on Particle Physics, Astrophysics
    and Cosmology
Authors: Bahcall, J.; Haxton, W.; Kubodera, K.; Poole, C.
2001neph.conf.....B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Correlations of solar neutrino observables for SNO
Authors: Bahcall, John N.; Krastev, Plamen I.; Smirnov, Alexei Yu.
2001PhRvD..63e3012B    Altcode: 2000hep.ph....6078B
  Neutrino oscillation scenarios predict correlations, and zones
  of avoidance, among measurable quantities such as spectral energy
  distortions, total fluxes, time dependences, and flavor content. The
  comparison of observed and predicted correlations will enhance
  the diagnostic power of solar neutrino experiments. A general
  test of all presently allowed (2ν) oscillation solutions is that
  future measurements must yield values outside the predicted zones of
  avoidance. To illustrate the discriminatory power of the simultaneous
  analysis of multiple observables, we map currently allowed regions
  of Δm<SUP>2</SUP>-sin<SUP>2</SUP> 2θ onto planes of quantities
  measurable with the Sudbury Neutrino Observatory (SNO). We calculate the
  correlations that are predicted by vacuum and MSW (active and sterile)
  neutrino oscillation solutions that are globally consistent with all
  available neutrino data. We derive approximate analytic expressions
  for the dependence of individual observables and specific correlations
  upon neutrino oscillations parameters. We also discuss the prospects
  for identifying the correct oscillation solution using multiple SNO
  observables.

---------------------------------------------------------
Title: Solar Neutrinos:. an Overview
Authors: Bahcall, J. N.
2001ppu..conf...63B    Altcode:
  I summarize the current state of solar neutrino research.

---------------------------------------------------------
Title: Why do Solar Neutrino Experiments Below 1 Mev?
Authors: Bahcall, J. N.
2001lesn.conf..172B    Altcode: 2001hep.ex....6086B
  I discuss why we need solar neutrino experiments below 1 MeV. I
  also express my prejudices about the desired number and types of
  such experiments, emphasizing the importance of p-p solar neutrino
  experiments.

---------------------------------------------------------
Title: Astrophysical Neutrinos
Authors: Bahcall, J. N.
2001IJMPA..16.4955B    Altcode: 2000hep.ph....9044B
  I summarize the first four decades of solar neutrino research and
  suggest what may be possible to learn with extragalactic neutrinos
  and with solar neutrinos in the next decade.

---------------------------------------------------------
Title: Proceedings of the Carolina Symposium on Neutrino Physics
: its impact on particle physics, astrophysics and cosmology :
    University of South Carolina, 10-12 March 2000
Authors: Bahcall, John N.; Avignone, F. T.
2001npip.book.....B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Astrophysical Neutrinos: 20th Century and Beyond
Authors: Bahcall, J. N.
2001NuPhS..91....9B    Altcode:
  I summarize the first four decades of solar neutrino research and
  suggest what may be possible to learn with extragalactic neutrinos
  and with solar neutrinos in the next decade.

---------------------------------------------------------
Title: How the Sun Shines
Authors: Bahcall, John N.
2000JRASC..94..219B    Altcode: 2000astro.ph..9259B
  This historical essay describes the struggle to understand how the
  sun shines. The story begins with the disagreement between Kelvin and
  Darwin over the age of the sun in the middle of the 19th century and
  continues through the revelations of solar neutrino experiments at
  the conclusion of the 20th century.

---------------------------------------------------------
Title: Astronomy: The Big Bang is bang on
Authors: Bahcall, John
2000Natur.408..916B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Interior: Neutrinos
Authors: Bahcall, J.
2000eaa..bookE2072B    Altcode:
  Six experiments have observed solar NEUTRINOS, three of which are
  radiochemical experiments: Homestake (chlorine detector), GALLEX
  (gallium detector) and SAGE (gallium detectors). These radiochemical
  detectors register all neutrinos above a fixed threshold energy (0.8
  MeV for chlorine, 0.2 MeV for gallium), with no further information
  about energy. Three other experiments, Kamiokande, SUPER-KAMIO...

---------------------------------------------------------
Title: SNO: Predictions for ten measurable quantities
Authors: Bahcall, John N.; Krastev, Plamen I.; Smirnov, Alexei Yu.
2000PhRvD..62i3004B    Altcode: 2000hep.ph....2293B
  We calculate the range of predicted values for 10 quantities that will
  be measured by the Sudbury Neutrino Observatory (SNO). We use neutrino
  oscillation solutions (vacuum and MSW; active and sterile neutrinos)
  that are globally consistent with all available neutrino data and
  estimate realistic theoretical and experimental uncertainties. The
  neutral current to charged current double ratio is predicted to be more
  than 9σ from the no-oscillation solution for all of the currently
  favored neutrino oscillation solutions. The best-fit oscillation
  solutions predict a CC day-night rate difference between -0.1% and
  +12.5% and a NC day-night difference &lt;0.01%. We present also the
  predicted range for the first and the second moments of the charged
  current electron recoil energy spectrum, the charged current, the
  neutral current, and the ν-e scattering rates, the seasonal dependence
  of the charged current rate, and the double ratio of neutrino-electron
  scattering rate to charged current rate.

---------------------------------------------------------
Title: Ultra-High-Energy Cosmic Rays May Come from Clustered Sources
Authors: Bahcall, John N.; Waxman, Eli
2000ApJ...542..542B    Altcode: 1999hep.ph...12326B
  Clustering of cosmic-ray sources affects the flux observed beyond
  the cutoff imposed by the cosmic microwave background and may be
  important in interpreting the AGASA, Fly's Eye, and HiRes data. The
  standard deviation, σ, in the predicted number N of events above
  10<SUP>20</SUP> eV is σ/N=0.9(r<SUB>0</SUB>/10 Mpc)<SUP>0.9</SUP>,
  where r<SUB>0</SUB> is the unknown scale length of the correlation
  function (r<SUB>0</SUB>~=10 Mpc for field galaxies, H<SUB>0</SUB>=50
  km s<SUP>-1</SUP> Mpc<SUP>-1</SUP>). Future experiments will allow the
  determination of r<SUB>0</SUB> through the detection of anisotropies
  in arrival directions of ~10<SUP>20</SUP> eV cosmic rays over angular
  scales of Θ~r<SUB>0</SUB>/30 Mpc.

---------------------------------------------------------
Title: Neutrino Afterglow from Gamma-Ray Bursts: ~10<SUP>18</SUP> EV
Authors: Waxman, Eli; Bahcall, John N.
2000ApJ...541..707W    Altcode: 1999hep.ph....9286W
  We show that a significant fraction of the energy of
  a γ-ray burst (GRB) is probably converted to a burst of
  10<SUP>17</SUP>-10<SUP>19</SUP> eV neutrinos and multiple GeV γ-rays
  that follow the main GRB by ~10 s. If GRBs accelerate protons to
  ~10<SUP>20</SUP> eV, a suggestion that recently gained support from
  observations of GRB afterglows, then both the neutrinos and the γ-rays
  may be detectable.

---------------------------------------------------------
Title: Solar neutrinos: an overview
Authors: Bahcall, J. N.
2000PhR...333...47B    Altcode:
  I summarize the current state of solar neutrino research.

---------------------------------------------------------
Title: Solar neutrinos
Authors: Bahcall, J. N.
2000AIPC..533...91B    Altcode: 2000hep.ex....2018B
  I summarize the current state of solar neutrino research and then
  answer the question: What should we do next? .

---------------------------------------------------------
Title: 5-10 GeV Neutrinos from Gamma-Ray Burst Fireballs
Authors: Bahcall, John N.; Mészáros, Peter
2000PhRvL..85.1362B    Altcode: 2000hep.ph....4019B
  A gamma-ray burst fireball is likely to contain an admixture of
  neutrons. Inelastic collisions between differentially streaming
  protons and neutrons in the fireball produce ν<SUB>μ</SUB>
  \(ν¯<SUB>μ</SUB>\) of ~10 GeV as well as ν<SUB>e</SUB>
  \(ν¯<SUB>e</SUB>\) of ~5 GeV, which could produce ~7 events/year
  in km<SUP>3</SUP> detectors, if the neutron abundance is comparable
  to that of protons. Photons of ~10 GeV from π<SUP>0</SUP> decay and
  ~100 MeV ν¯<SUB>e</SUB> from neutron decay are also produced, but
  will be difficult to detect. Photons with energies &lt;~1 MeV from
  shocks following neutron decay produce a characteristic signal which
  may be distinguishable from the proton-related MeV photons.

---------------------------------------------------------
Title: The Hubble Space Telescope Quasar Absorption Line Key
    Project. XV. Milky Way Absorption Lines
Authors: Savage, Blair D.; Wakker, Bart; Jannuzi, Buell T.; Bahcall,
   John N.; Bergeron, Jacqueline; Boksenberg, Alec; Hartig, George F.;
   Kirhakos, Sofia; Murphy, Edward M.; Sargent, W. L. W.; Schneider,
   Donald P.; Turnshek, David; Wolfe, Arthur M.
2000ApJS..129..563S    Altcode:
  This paper presents the results of an analysis of the Milky Way
  absorption lines found in the Hubble Space Telescope (HST) Quasar
  Absorption Line Key Project database for 83 QSOs observed with the
  Faint Object Spectrograph G190H and G270H gratings, of which 16
  QSOs are also observed with the G130H grating. The HST Key Project
  observations are supplemented with high-quality 21 cm H I emission-line
  observations mostly obtained with the NRAO 43 m radio telescope. The
  Milky Way halo gas exhibits “mixed ionization” absorption with
  high-ionization absorption from Si IV and C IV substantially weaker
  than the extremely strong intermediate- and low-ionization absorption
  from Si III, Si II, C II, Mg II, and Fe II. For a sample of 16 QSOs
  observed in the far-UV, the median velocity equivalent widths of
  very strong lines of Si IV, Si III, and Si II are 60, 180, and 180
  km s<SUP>-1</SUP>, respectively. Velocity equivalent widths this
  large for Si III and Si II imply the existence of high velocity
  dispersion moderate- (Si III) and low-ionization (Si II) gas along
  many paths through the Galactic halo. Measures of the Galactic
  damped Lyα line toward 14 QSOs permit the determination of N(H
  I)<SUB>Lyα</SUB> through the gaseous disk and halo of the Galaxy. The
  values of N(H I)<SUB>Lyα</SUB> range from 0.64×10<SUP>20</SUP> to
  3.37×10<SUP>20</SUP> cm<SUP>-2</SUP> with N(H I)<SUB>Lyα</SUB>|sinb|
  averaging (1.29+/-0.49)×10<SUP>20</SUP> cm<SUP>-2</SUP>. A comparison
  of N(H I)<SUB>Lyα</SUB> with N(H I)<SUB>21cm</SUB> reveals that N(H
  I)<SUB>Lyα</SUB>/N(H I)<SUB>21cm</SUB> for the 10 sight lines where
  the value of N(H I)<SUB>Lyα</SUB> is not significantly affected by
  geocoronal emission ranges from 0.62 and 0.91. This difference is
  probably produced by a combination of systematic and random errors
  and contribution from the small angular scale structure in the H I
  distribution. Such structure can produce different column densities
  when sampling gas with an infinitesimal beam in the UV (the angular
  size of the QSO) compared to the much larger 21<SUP>'</SUP> beam of
  the NRAO 43 m radio telescope. <P />The overall strength of the Mg II
  λλ2796 and 2803 absorption appears to be correlated with the presence
  of high-velocity gas along the line to sight. Velocity-resolved Mg II
  absorption associated with high-velocity gas in the Magellanic Stream
  is detected toward eight QSOs, including PKS 0003+15, PG 0043+039,
  PKS 0637-75, 3C 454.3, PKS 2251+11, PG 2302+029, PKS 2340-36, and
  PKS 2344+09. Velocity-resolved Mg II absorption toward 15 QSOs is not
  accompanied by the existence of associated H I emission. Interesting
  objects in this category include PKS 0232-04 (l=174.5d, b=-56.2d),
  which has a high-velocity cloud (HVC) at v~+270 km s<SUP>-1</SUP>
  detected in Mg II, and PG 1116+215 (l=223.3d,b=68.2d) with a HVC at
  +200 km s<SUP>-1</SUP> detected in Mg II, C II, Si IV, and possibly
  C IV. The HVC toward PKS 0232-04 is interesting because all known H I
  HVCs in this general region of the sky have negative velocity rather
  than positive velocity. For 15 QSOs known to lie in the direction of
  H I HVCs, the Mg II lines have extremely strong principal absorption
  components, suggesting the detection of blended low- and high-velocity
  absorption. These lines of sight imply the detection of Mg II absorption
  by the high-velocity gas in HVC complexes C and A, in the outer Galaxy
  warp, and in the Magellanic Stream, as well as toward three smaller
  clouds. There are 11 QSO sight lines with very strong Mg II absorption
  for which there is no evidence for high-velocity H I emission. However,
  six of these sight lines lie near known H I HVCs. There are 38 QSOs
  with weak Mg II principal absorption and no known H I HVCs. These
  objects provide information about the H I absorption characteristics of
  disk and halo gas well away from H I HVCs. The sky covering factor of
  high-velocity Mg II is large, with 41 and 71 QSO lines of sight showing
  either resolved high-velocity Mg II absorption or principal absorption
  that is so strong that blended low- and high-velocity Mg II absorption
  is suggested. <P />Based on observations with the NASA/ESA Hubble
  Space Telescope, obtained at the Space Telescope Science Institute,
  which is operated by the Association of Universities for Research in
  Astronomy, Inc., under NASA contract NAS-26555.

---------------------------------------------------------
Title: VizieR Online Data Catalog: HST quasar absorption-line key
    project. VIII. (Kirhakos+, 1994)
Authors: Kirhakos, S.; Sargent, W. L. W.; Schneider, D. P.; Bahcall,
   J. N.; Jannuzi, B. T.; Maoz, D.; Small, T. A.
2000yCat..61060646K    Altcode:
  We present an analysis of CCD images (obtained at the Palomar 1.5m
  telescope) of more than 100 quasars; many of the objects have been
  or will be observed in the HST Key Project Quasar Absorption-Line
  Survey. The data set consists of B, g, and i photometry of 117
  quasars and deeper g (limiting magnitude of ~22) images of 101 quasar
  fields. Positions accurate to ~1", measured with the Space Telescope
  Science Institute's Astrometric Support Program, are listed for all of
  the quasars in this study. Positions, magnitudes, and classifications
  of stars and galaxies located within ~100" of the quasars are given
  for all of the deep g data. The positions of the stars and galaxies
  relative to the quasar are accurate to ~0.5". The results presented
  here can be used to prepare spectroscopic programs designed to obtain
  redshifts of galaxies in the fields of these quasars. (3 data files).

---------------------------------------------------------
Title: The Evolution of Neutrino Astronomy
Authors: Bahcall, John N.; Davis, Raymond, Jr.
2000PASP..112..429B    Altcode: 1999astro.ph.11486B
  This Essay is one of a series of invited contributions which will
  appear in the PASP throughout the year 2000 to mark the upcoming
  millennium. (Eds.)

---------------------------------------------------------
Title: What will the first year of SNO show?
Authors: Bahcall, J. N.; Krastev, P. I.; Smirnov, A. Y.
2000PhLB..477..401B    Altcode: 1999hep.ph...11248B
  The ratio of the measured to the predicted standard model CC event
  rates in SNO will be 0.47 if no oscillations occur. The best-fit active
  oscillation predictions for the CC ratio are: 0.35-39 (MSW) and 0.38-42
  (vacuum) (all for a /5 MeV energy threshold), typically about /20%
  less than the no-oscillation expectation. We calculate the predicted
  ratios for six active and sterile neutrino oscillation solutions
  allowed at 99% CL and determine the dependence of the ratios on energy
  threshold. If the high-energy anomaly observed by SuperKamiokande
  is due to an enhanced /hep flux, MSW active solutions predict that
  out of a total of /5000 CC events above /5 MeV in SNO between /49 and
  /54 events will be observed above /13 MeV whereas only /19 events are
  expected for no-oscillations and a nominal standard /hep flux.

---------------------------------------------------------
Title: How Much Do Helioseismological Inferences Depend on the
    Assumed Reference Model?
Authors: Basu, Sarbani; Pinsonneault, M. H.; Bahcall, John N.
2000ApJ...529.1084B    Altcode: 1999astro.ph..9247B
  We investigate systematic uncertainties in determining the profiles
  of the solar sound speed, density, and adiabatic index using
  helioseismological techniques. We find that rms uncertainties (averaged
  over the Sun) of ~0.02%-0.04% are contributed to the sound-speed
  profile by each of three sources: (1) the choice of assumed reference
  model, (2) the width of the inversion kernel, and (3) the measurement
  errors. The rms agreement between the standard solar model sound speeds
  and the best helioseismological determinations is about 0.07%. The
  profile of the adiabatic index, Γ<SUB>1</SUB>, is determined to
  an accuracy of about 0.02% with the Michelson Doppler Imager (MDI)
  data set. The density profile is about an order of magnitude less well
  determined by the helioseismological measurements. Five state-of-the-art
  models, each with a significant difference in the input physics or
  a parameter choice, all give comparably good agreement with global
  helioseismological measurements. We consider four deficient solar
  models that are constructed either using old input data, assuming the
  <SUP>3</SUP>He+<SUP>4</SUP>He fusion reaction does not occur, neglecting
  element diffusion, or artificially mixing the interior of the Sun. When
  used as reference models in the inversion process, these deficient
  models yield sound speeds for the Sun that differ only by 0.1% from
  the sound speeds obtained using the standard model. We conclude that
  even relatively crude reference models yield reasonably accurate solar
  parameters. Although acceptable for most purposes as reference models,
  nonstandard solar models in which the core is artificially mixed or
  in which element diffusion is neglected are strongly disfavored by the
  p-mode oscillation data. These nonstandard models produce sound-speed
  profiles with respect to the Sun that are 4.5 and 18 times worse,
  respectively, than the agreement obtained with the standard solar model.

---------------------------------------------------------
Title: Solar neutrinos
Authors: Bahcall, J. N.
2000upse.conf..126B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Neutrinos: an Overview
Authors: Bahcall, J. N.
2000PhST...85...63B    Altcode:
  I summarize the current state of solar neutrino research.

---------------------------------------------------------
Title: Solar neutrinos: An overview
Authors: Bahcall, J. N.
1999CSci...77.1487B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Ulrich's Explanation for the Solar Five Minute Oscillations
Authors: Bahcall, John
1999ApJ...525C1199B    Altcode: 1999ApJC..525.1199B
  No abstract at ADS

---------------------------------------------------------
Title: Is a large mixing angle MSW effect the solution of the solar
    neutrino problems?
Authors: Bahcall, J. N.; Krastev, P. I.; Smirnov, A. Yu.
1999PhRvD..60i3001B    Altcode: 1999hep.ph....5220B
  Recent results on solar neutrinos provide hints that the LMA
  MSW solution could be correct. We perform accurate calculations
  for potential “smoking-gun” effects of the LMA solution in
  the SuperKamiokande solar neutrino experiment, including (1) an
  almost constant reduction of the standard recoil electron energy
  spectrum (with a weak, &lt;10%, relative increase below 6.5 MeV),
  (2) an integrated difference in day-night rates (2%-14%), (3) an
  approximately constant zenith-angle dependence of the nighttime event
  rate, (4) a new test for the difference in the shape of the equally
  normalized day-night energy spectra (~1%), and (5) annual variations
  of the signal due to the regeneration effect (~6 times smaller than
  the integrated day-night effect). We also establish a relation between
  the integrated day-night asymmetry and the seasonal asymmetry due to
  LMA regeneration. As a cautionary example, we simulate the effect
  of an absolute energy calibration error on the shape (distortion)
  of the recoil energy spectrum. We compare LMA predictions with the
  available SuperKamiokande data for 708 days of operation and discuss
  the possibilities for distinguishing experimentally between LMA and
  vacuum oscillations. If LMA is correct, global solutions combining
  data from different types of measurements made by SuperKamiokande or
  by different solar neutrino experiments could reveal in the next few
  years a many σ indication of neutrino oscillations.

---------------------------------------------------------
Title: The Host Galaxies of Three Radio-loud Quasars: 3C 48, 3C 345,
    and B2 1425+267
Authors: Kirhakos, Sofia; Bahcall, John N.; Schneider, Donald P.;
   Kristian, Jerome
1999ApJ...520...67K    Altcode: 1999astro.ph..2175K
  Observations with the Wide-Field/Planetary Camera-2 of the Hubble
  Space Telescope are presented for three radio-loud quasars: 3C 48
  (z=0.367), B2 1425+267 (z=0.366), and 3C 345 (z=0.594). All three
  quasars have luminous (~4×L<SUP>*</SUP>) galaxies as hosts, which are
  either elliptical (B2 1425+267 and 3C345) or interacting (3C 48), and
  all hosts are 0.5-1.0 mag bluer in V-I than other galaxies with the same
  overall morphology at redshifts similar to those of the quasars. The
  host of 3C 48 has many H II regions and a very extended tidal tail. All
  nine of the radio-loud quasars studied here and in a previous paper
  by Bahcall et al. either have bright elliptical hosts or occur in
  interacting systems. There is a robust correlation between the radio
  emission of the quasar and the luminosity of host galaxy; the radio-loud
  quasars reside in galaxies that are on average ~1 mag brighter than
  hosts of the radio-quiet quasars. <P />Based on observations with the
  NASA/ESA Hubble Space Telescope obtained at the Space Telescope Science
  Institute, which is operated by the Association of Universities for
  Research in Astronomy, Inc., under NASA contract NAS5-26555.

---------------------------------------------------------
Title: What can we learn from past discoveries?
Authors: Bahcall, J. N.
1999AAS...194.9501B    Altcode: 1999BAAS...31..992B
  I will describe some ocassions during which I witnessed or talked
  to people who were making important astronomical discoveries. I will
  present my version of the lessons for the future that are to be learned
  from these discoveries and discoverers.

---------------------------------------------------------
Title: Standard solar models
Authors: Bahcall, John N.
1999NuPhS..77...64B    Altcode: 1998astro.ph..8162B
  I review recent developments that affect standard solar model
  predictions of solar neutrino fluxes.

---------------------------------------------------------
Title: How does the sun shine?
Authors: Bahcall, J. N.
1999AAS...194.2701B    Altcode: 1999BAAS...31..864B
  Neutrino astronomy was developed to test the theory that stars shine
  and evolve by burning light elements in their interiors. Five beautiful
  experiments have proven that the sun does shine by nuclear fusion
  reactions, but robust discrepancies between the standard predictions
  and the observations suggest that neutrinos exhibit physics beyond the
  standard model of electroweak interactions. I will review the neutrino
  and helioseismological evidence confirming solar fusion and suggesting
  new electroweak physics. Major new observatories are being built to
  search for smoking-gun evidence of non-standard neutrino phenomena.

---------------------------------------------------------
Title: How much do helioseismological inferences depend upon the
    assumed reference model?
Authors: Basu, S.; Pinsonneault, M. H.; Bahcall, J. N.
1999AAS...194.5603B    Altcode: 1999BAAS...31Q.912B
  We investigate systematic uncertainties in determining the profiles
  of the solar sound speed and the density by helioseismological
  techniques. We find that rms uncertainties averaged over the
  sun ~ 0.02%-0.04% are contributed to the sound speed profile by
  each of three sources: 1) the choice of assumed reference model,
  2) the width of the inversion kernel, and 3) the measurement
  errors. The rms agreement between the standard solar model and the
  best helioseismological determinations is about 0.07%. The density
  profile is about an order of magnitude less well determined by the
  helioseismological measurements. JNB and SB are supported in part by
  NSF grant #PHY95-13835.

---------------------------------------------------------
Title: BSGMODEL: The Bahcall-Soneira Galaxy Model
Authors: Bahcall, John N.
1999ascl.soft04001B    Altcode:
  BSGMODEL is used to construct the disk and spheroid components of the
  Galaxy from which the distribution of visible stars and mass in the
  Galaxy is calculated. The computer files accessible here are available
  for export use. The modifications are described in comment lines in
  the software. The Galaxy model software has been installed and used by
  different people for a large variety of purposes (see, e. g., the the
  review "Star Counts and Galactic Structure”, Ann. Rev. Astron. Ap. 24,
  577, 1986 ).

---------------------------------------------------------
Title: Faint Star Counts with HST
Authors: Flynn, Chris; Gould, Andrew; Bahcall, John
1999ASPC..165..387F    Altcode: 1999gaha.conf..387F; 1998astro.ph.12321F
  We describe a program of star counts in the range 19 &lt;~ I &lt;~
  26 made with the WFPC cameras aboard the Hubble Space Telescope. Red
  (V-I &gt; 1.0) stars at these magnitudes are primarily disk and spheroid
  M dwarfs. The stars are found both on dedicated images as part of the
  parallel program and by using appropriate archive data. We measure
  the faint end of the luminosity functions of the disk and spheroid
  (i.e.~stellar halo). We measure the low mass end of the mass function
  and show that M dwarfs do not dominate the total disk or spheroid
  mass. We place strong I band constraints on the amount of halo dark
  matter in the form of low mass stars (such as M dwarfs or cool white
  dwarfs). The disk and spheroid contribute only a minor amount of
  optical depth toward the Magellanic clouds.

---------------------------------------------------------
Title: Solar Neutrinos
Authors: Bahcall, J. N.
1999nwap.conf...28B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Standard Solar Models
Authors: Bahcall, J. N.
1999nenp.conf...77B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Prioritizing Science: A Story of the Decade Survey for
    the 1990s
Authors: Bahcall, John N.
1999aasf.book..289B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Neutrinos: An Overview
Authors: Bahcall, J. N.
1999ccmn.conf...37B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Neutrinos: Where We Are
Authors: Bahcall, J.
1999psc..conf....2B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: High energy neutrinos from astrophysical sources: An upper
    bound
Authors: Waxman, Eli; Bahcall, John
1998PhRvD..59b3002W    Altcode: 1999PhRvD..59b3002W; 1998hep.ph....7282W
  We show that cosmic-ray observations set a model-independent upper bound
  of E<SUP>2</SUP><SUB>ν</SUB>Φ<SUB>ν</SUB>&lt;2×10<SUP>-8</SUP>
  GeV/cm<SUP>2</SUP> s sr to the intensity of high-energy neutrinos
  produced by photo-meson (or p-p) interactions in sources of size not
  much larger than the proton photo-meson (or p-p) mean-free-path. This
  bound applies, in particular, to neutrino production by either AGN
  jets or GRBs. The upper limit is two orders of magnitude below the
  intensity predicted in some popular AGN jet models and therefore
  contradicts the theory that the cosmic gamma-ray background is due to
  photo-pion interactions in AGN jets. The upper bound is consistent
  with our predictions from GRB models. The predicted intensity from
  GRBs is E<SUP>2</SUP>dN/dE~0.3×10<SUP>-8</SUP> GeV/cm<SUP>2</SUP>
  s sr for 10<SUP>14</SUP> eV&lt;E&lt;10<SUP>16</SUP> eV; we also derive
  the expected intensity at higher energy.

---------------------------------------------------------
Title: An upper bound to the high-energy neutrino flux from
    astrophysical sources
Authors: Waxman, E.; Bahcall, J. N.
1998tx19.confE.618W    Altcode:
  An upper bound to the high-energy neutrino flux from astrophysical
  sources, imposed by cosmic-ray observations, is derived. The upper
  bound applies to sources which are optically thin to proton photo-meson
  interaction, and cannot be avoided by invoking source redshift evolution
  or inter-galactic magnetic fields. This upper limit is two orders of
  magnitude below the flux predicted in popular AGN jet models, but is
  consistent with our predictions from GRB models. Its implications to
  future neutrino detectors are discussed.

---------------------------------------------------------
Title: The Host Galaxy of the Gamma-Ray Burst 971214
Authors: Odewahn, S. C.; Djorgovski, S. G.; Kulkarni, S. R.; Dickinson,
   M.; Frail, D. A.; Ramaprakash, A. N.; Bloom, J. S.; Adelberger, K. L.;
   Halpern, J.; Helfand, D. J.; Bahcall, J.; Goodrich, R.; Frontera,
   F.; Feroci, M.; Piro, L.; Costa, E.
1998ApJ...509L...5O    Altcode: 1998astro.ph..7212O
  We report on Hubble Space Telescope (HST) observations of the
  host galaxy of GRB 971214, taken 4 months after the burst. The
  redshift of the proposed host galaxy at z=3.418, combined with
  optical and radio observations of the burst afterglow, implies the
  extremely large isotropic energy release from the burst in γ-rays of
  E<SUB>γ</SUB>~3×10<SUP>53</SUP> ergs, some 2 orders of magnitude
  higher than the previously commonly assumed numbers. The positional
  offset between the optical transient observed at the Keck telescope
  and the centroid of the proposed host galaxy in the HST image is
  0.14"+/-0.07". We find no evidence in our deep HST image for a chance
  foreground galaxy superposed along the line of sight to the proposed
  host at z=3.418. The morphology and photometric properties of this
  galaxy, such as the total flux, morphology, radial surface profile,
  and scale length, are typical as compared to other, spectroscopically
  confirmed z&gt;=3 galaxies. <P />Based on observations with the
  NASA/ESA Hubble Space Telescope obtained at the Space Telescope Science
  Institute, which is operated by AURA, Inc., under NASA contract NAS
  5-26555 and on observations obtained at the W. M. Keck Observatory,
  which is operated jointly by the California Institute of Technology
  and the University of California.

---------------------------------------------------------
Title: Where do we stand with solar neutrino oscillations?
Authors: Bahcall, J. N.; Krastev, P. I.; Smirnov, A. Yu.
1998PhRvD..58i6016B    Altcode: 1998hep.ph....7216B
  We determine parameters for MSW and vacuum oscillations
  (active and sterile neutrinos) that are allowed by separate,
  and collective, imposition of the constraints from total
  event rates in the chlorine, GALLEX, SAGE, and SuperKamiokande
  experiments (504 days), the SuperKamiokande energy spectrum, and
  the SuperKamiokande zenith-angle dependence. The small mixing angle
  MSW solution is acceptable at 7% C.L. (8% for sterile ν's) and the
  vacuum solution is acceptable at 6% C.L. The best-fit global MSW
  solution for active neutrinos is Δm<SUP>2</SUP>=5×10<SUP>-6</SUP>
  eV<SUP>2</SUP>, sin<SUP>2</SUP>2θ=5.5×10<SUP>-3</SUP> (and for
  sterile neutrinos Δm<SUP>2</SUP>=4×10<SUP>-6</SUP> eV<SUP>2</SUP>,
  sin<SUP>2</SUP>2θ=7×10<SUP>-3</SUP>). For vacuum oscillations,
  the best-fit solution is Δm<SUP>2</SUP>=6.5×10<SUP>-11</SUP>
  eV<SUP>2</SUP>, sin<SUP>2</SUP>2θ=0.75. An arbitrary combination of
  undistorted (no oscillations) pp, <SUP>7</SUP>Be, <SUP>8</SUP>B, and
  CNO neutrino fluxes is inconsistent with the combined data sets at the
  3.5σ C.L., independent of astrophysical considerations. We use improved
  calculations of solar model fluxes, neutrino absorption cross sections
  and energy spectra, and a detailed evaluation of regeneration effects.

---------------------------------------------------------
Title: Globular Cluster Photometry with the Hubble Space
    Telescope. VII. Color Gradients and Blue Stragglers in the Central
    Region of M30 from Wide Field Planetary Camera 2 Observations
Authors: Guhathakurta, Puragra; Webster, Zodiac T.; Yanny, Brian;
   Schneider, Donald P.; Bahcall, John N.
1998AJ....116.1757G    Altcode: 1998astro.ph..5361G
  We present F555W (V), F439W (B), and F336W (U) photometry of 9507 stars
  in the central 2' of the dense, post-core-collapse cluster M30 (NGC
  7099) derived from Hubble Space Telescope Wide Field Planetary Camera
  2 images. These data are used to study the mix of stellar populations
  in the central region of the cluster. Forty-eight blue straggler stars
  are identified; they are found to be strongly concentrated toward the
  cluster center. The specific frequency of blue stragglers, F_BSS =
  N(BSS)/N(V &lt; V_HB + 2), is 0.25 +/- 0.05 in the inner region of
  M30 (r &lt; 20"), significantly higher than the frequency found in
  other clusters: F_BSS = 0.05-0.15. The shape of M30's blue straggler
  luminosity function resembles the prediction of the collisional
  formation model, and is inconsistent with the binary merger model
  of Bailyn &amp; Pinsonneault. An unusually blue star (B = 18.6,
  B-V = -0.97), possibly a cataclysmic variable based on its color,
  is found about 1.2" from the crowded cluster center; the photometric
  uncertainty for this star is large, however, because of the presence
  of a very close neighbor. Bright red giant stars (B &lt; 16.6) appear
  to be depleted by a factor of 2-3 in the inner r &lt; 10" relative
  to fainter giants, subgiants, and main-sequence turnoff stars (95%
  significance). We confirm that there is a radial gradient in the color
  of the overall cluster light, going from B-V ~ 0.82 at r ~ 1' to B-V ~
  0.45 in the central 10". The central depletion of the bright red giants
  is responsible for about half of the observed color gradient; the rest
  of the gradient is caused by the relative underabundance of faint red
  main-sequence stars near the cluster center (presumably a result of
  mass segregation). The luminosity function of M30's evolved stars does
  not match the luminosity function shape derived from standard stellar
  evolutionary models: the ratio of the number of bright giants to the
  number of turnoff stars in the cluster is 30% higher than predicted
  by the model (3.8 sigma effect), roughly independent of red giant
  brightness over the range M_V = -2 to +2. Based on observations with
  the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope
  Science Institute, which is operated by the Association of Universities
  for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Lick
  Observatory Bulletin No. 1377.

---------------------------------------------------------
Title: The Hubble Space Telescope Quasar Absorption Line Key
    Project. XIV. The Evolution of Lyα Absorption Lines in the Redshift
    Interval z = 0-1.5
Authors: Weymann, Ray J.; Jannuzi, Buell T.; Lu, Limin; Bahcall,
   John N.; Bergeron, Jacqueline; Boksenberg, Alec; Hartig, George F.;
   Kirhakos, Sofia; Sargent, W. L. W.; Savage, Blair D.; Schneider,
   Donald P.; Turnshek, David A.; Wolfe, Arthur M.
1998ApJ...506....1W    Altcode: 1998astro.ph..6123W
  We present the results of an analysis of the rate of evolution of the
  Lyα absorption lines in the redshift interval 0.0 to ~1.5 based upon
  a sample of 987 Lyα absorption lines identified in the spectra of 63
  QSOs obtained with the Faint Object Spectrograph (FOS) of the Hubble
  Space Telescope (HST). These spectra were obtained as part of the QSO
  Absorption Line Survey, an HST Key Project during the first four years
  of observations with the telescope. Fits to the evolution of the number
  of absorbers per unit redshift (dN/dz) of the form dN/dz = A × (1 +
  z)<SUP>γ</SUP> continue to yield values of γ in the range 0.1-0.3,
  decidedly flatter than results from ground-based data pertaining
  to the redshift range z &gt; 1.7. These results are consistent with
  our previous results based on a much smaller sample of lines, but the
  uncertainties in the fit have been greatly reduced. The combination of
  the HST and ground-based data suggest a marked transition in the rate
  of evolution of the Lyα lines at a redshift of about 1.7. The 19 Lyα
  lines from an additional higher redshift QSO from our sample for which
  tentative line identifications are available (UM 18; z<SUB>em</SUB>
  = 1.89) support the suggestion of a rapid increase at around this
  redshift. We derive the cumulative distribution of the full sample of
  Lyα lines and show that the distribution in redshift can indeed be
  well represented by a power law of the form (1 + z)<SUP>γ</SUP>. For
  this same sample, the distribution of equivalent widths of the Lyα
  absorbers above a rest equivalent width of 0.1 Å is fit quite well
  by an exponential. Comparing samples of Lyα lines, one set of which
  has redshifts the same as, or very near to, the redshifts of ions from
  heavy elements and another set in which no ions from heavy elements
  have been identified, we find that the Lyα systems with heavy element
  detections have a much steeper slope than the high rest equivalent
  width portion of the Lyman-only sample. We argue that this result is
  not likely to be due to either line misidentification or incomplete
  spectral coverage. Considering the insensitivity of the equivalent width
  to large changes in the column density for saturated lines, we suggest
  that this result is probably attributable to rapid evolution of the
  very highest column density systems, rather than real differences in
  metallicity. We find evidence that the rate of evolution increases with
  increasing equivalent width. We compare our results for the variation
  of line density with redshift to recent numerical simulations of Lyα
  absorbers, in particular, to those of Riediger, Petitjean, &amp; Mucket,
  which extend to zero redshift. We find fairly good agreement between
  these simulations and our results, though the rapid evolution we find
  in the Lyα systems containing heavy element ions is not predicted
  in their models. We speculate that these heavy element-containing
  Lyα systems involve those clouds closely associated with galaxies,
  whose column densities are too high and whose sizes are too small to be
  included in the Riediger et al. simulations. Our results for Lyα lines
  at the high end of our equivalent width distribution are compatible
  with the recent analysis of the absorber-galaxy correlation by Chen et
  al. For the weaker lines, however, our results suggest that whatever
  association exists between absorbers and galaxies is different from that
  for the stronger lines. We conclude with some suggestions for further
  observations. <P />Based on observations with the NASA/ESA Hubble
  Space Telescope, obtained at the Space Telescope Science Institute,
  which is operated by the Association of Universities for Research in
  Astronomy, Inc., under NASA contract NAS 5-26555.

---------------------------------------------------------
Title: Solar fusion cross sections
Authors: Adelberger, Eric G.; Austin, Sam M.; Bahcall, John N.;
   Balantekin, A. B.; Bogaert, Gilles; Brown, Lowell S.; Buchmann, Lothar;
   Cecil, F. Edward; Champagne, Arthur E.; de Braeckeleer, Ludwig; Duba,
   Charles A.; Elliott, Steven R.; Freedman, Stuart J.; Gai, Moshe;
   Goldring, G.; Gould, Christopher R.; Gruzinov, Andrei; Haxton,
   Wick C.; Heeger, Karsten M.; Henley, Ernest; Johnson, Calvin W.;
   Kamionkowski, Marc; Kavanagh, Ralph W.; Koonin, Steven E.; Kubodera,
   Kuniharu; Langanke, Karlheinz; Motobayashi, Tohru; Pandharipande,
   Vijay; Parker, Peter; Robertson, R. G.; Rolfs, Claus; Sawyer, R. F.;
   Shaviv, N.; Shoppa, T. D.; Snover, K. A.; Swanson, Erik; Tribble,
   Robert E.; Turck-Chièze, Sylvaine; Wilkerson, John F.
1998RvMP...70.1265A    Altcode: 1998astro.ph..5121A
  We review and analyze the available information on the nuclear-fusion
  cross sections that are most important for solar energy generation and
  solar neutrino production. We provide best values for the low-energy
  cross-section factors and, wherever possible, estimates of the
  uncertainties. We also describe the most important experiments and
  calculations that are required in order to improve our knowledge of
  solar fusion rates.

---------------------------------------------------------
Title: Screening in Thermonuclear Reaction Rates in the Sun
Authors: Gruzinov, Andrei V.; Bahcall, John N.
1998ApJ...504..996G    Altcode: 1998astro.ph..1028G
  We evaluate the effect of electrostatic screening by ions and electrons
  on low-Z thermonuclear reactions in the Sun. We use a mean field
  formalism and calculate the electron density of the screening cloud
  using the appropriate density matrix equation of quantum statistical
  mechanics. Because of well-understood physical effects that are included
  for the first time in our treatment, the calculated enhancement of
  reaction rates does not agree with the frequently used interpolation
  formulae. Our result does agree, within small uncertainties, with
  Salpeter's weak screening formula. If weak screening is used instead
  of the commonly employed screening prescription of Graboske et al.,
  the predicted <SUP>8</SUP>B neutrino flux is increased by 7% and the
  predicted chlorine rate is increased by 0.4 SNU.

---------------------------------------------------------
Title: The Hubble Space Telescope Quasar Absorption Line Key
    Project. XIII. A Census of Absorption-Line Systems at Low Redshift
Authors: Jannuzi, Buell T.; Bahcall, John N.; Bergeron, Jacqueline;
   Boksenberg, Alec; Hartig, George F.; Kirhakos, Sofia; Sargent,
   W. L. W.; Savage, Blair D.; Schneider, Donald P.; Turnshek, David A.;
   Weymann, Ray J.; Wolfe, Arthur M.
1998ApJS..118....1J    Altcode: 1998astro.ph..5148J
  We present a catalog of absorption lines obtained from the analysis
  of the ultraviolet spectra of 66 quasars. The data were acquired with
  the Faint Object Spectrograph of the Hubble Space Telescope (HST)
  as part of the Quasar Absorption Line Survey, a Key Project for the
  first four cycles of HST observations. This is the third of a series
  of catalogs of absorption lines produced from the survey and increases
  the number of quasars whose higher resolution (R = 1300) spectra we
  have published from 17 to 83. The general properties and execution of
  the survey are reviewed, including descriptions of the final sample
  of observed objects and the algorithmic processes used to construct
  the catalog. This database is suitable for a wide variety of studies
  of gaseous systems in the nearby universe. This third catalog includes
  2594 absorption lines and brings the total number of absorption lines in
  the combined catalog to 3238. The third catalog has 878 identified Lyα
  lines, 27 extensive metal line systems (detected absorption lines from
  four or more metal ions), 88 C IV systems, and 34 O VI systems. The
  combined catalog contains the following numbers of extragalactic
  absorption lines: 1129 Lyα lines, 107 C IV systems, 41 O VI systems,
  16 Lyman limit systems, and one damped Lyα system (in the spectrum
  of PG 0935+416). In addition, there are 25 pairs of identified Lyα
  lines that are candidate C IV doublets. Of the 122 identified C IV and
  candidate C IV systems in the completely identified sample of absorption
  lines, 24 +/- 5 are expected to be chance coincidences of other lines
  (based upon Monte Carlo simulations). The detection of a single damped
  Lyα system in a path length of Δz = 49 yields an observed number of
  damped systems per unit redshift of (dN/dz)<SUB>damp</SUB>(z = 0.58)
  = 0.020 with 95% confidence boundaries of 0.001-0.096 systems per unit
  redshift. <P />We include notes on our analysis of each of the observed
  quasars and the absorption systems detected in each spectrum. Some
  especially interesting systems include low-redshift Lyα absorbers
  suitable for extensive follow-up observations (e.g., in the spectra
  of TON 28 and PG 1216+069), possibly physically associated pairs of
  extensive metal line absorption systems (e.g., in the spectrum of PG
  0117+213), and systems known to be associated with galaxies (e.g.,
  in the spectrum of 3C 232). <P />The spectra of five broad absorption
  line (BAL) quasars (UM 425, PG 1254+047, PG 1411+442, PG 1700+518, and
  PG 2112+059) can be found in this third catalog, bringing the total
  number of BAL quasars in the combined catalog to six (including PG
  0043+039). <P />Based on observations with the NASA/ESA Hubble Space
  Telescope, obtained at the Space Telescope Science Institute, which is
  operated by the Association of Universities for Research in Astronomy,
  Inc., under NASA contract NAS 5-26555.

---------------------------------------------------------
Title: Do hep neutrinos affect the solar neutrino energy spectrum?
Authors: Bahcall, John N.; Krastev, Plamen I.
1998PhLB..436..243B    Altcode: 1998hep.ph....7525B
  If the low energy cross section for
  <SUP>3</SUP>He+p--&gt;<SUP>4</SUP>He+e<SUP>+</SUP>+ν<SUB>e</SUB>, the
  `hep' reaction, is &gt;~20 times larger than the best (but uncertain)
  theoretical estimates, then this reaction could significantly influence
  the electron energy spectrum produced by solar neutrino interactions
  and measured in the SuperKamiokande, SNO, and ICARUS experiments. We
  compare predicted energy spectra for different assumed hep fluxes
  and different neutrino oscillation scenarios with the observed
  SuperKamiokande spectrum. The spectra with enhanced hep contributions
  provide better fits to the SuperKamiokande data.

---------------------------------------------------------
Title: Spheroid Luminosity and Mass Functions from Hubble Space
    Telescope Star Counts
Authors: Gould, Andrew; Flynn, Chris; Bahcall, John N.
1998ApJ...503..798G    Altcode: 1997astro.ph.11263G
  We analyze 166 spheroid subdwarfs (6.5 &lt; M<SUB>V</SUB> &lt; 14.5)
  found in 53 fields observed with the Wide Field Planetary Camera on
  the Hubble Space Telescope. The fields cover 221 arcmin<SUP>2</SUP>
  over a wide range of directions. The spheroid luminosity function (LF)
  is inconsistent at about the 3 σ level with the local spheroid LF of
  Dahn et al. even when the normalization of the latter is corrected to
  take account of the latest data on spheroid kinematics. The difference
  may reflect systematic errors in one of the two studies or features
  of the spheroid spatial distribution that are not included in the
  simplest models. The mass function, which shows no obvious structure,
  can be represented by a power law, dN/d ln M ~ M<SUP>α</SUP>, with
  α = 0.25 +/- 0.32 over the mass range 0.71 M<SUB>⊙</SUB> &gt; M
  &gt; 0.09 M<SUB>⊙</SUB>. The spheroid therefore does not contribute
  significantly to microlensing unless the mass function changes slope
  dramatically in the substellar range. The total local mass density
  of spheroid stars (including remnants and unseen binary companions)
  is ρ ~ 6.4 × 10<SUP>-5</SUP> M<SUB>⊙</SUB> pc<SUP>-3</SUP>, with
  an uncertainty of about 50%. The power-law indices α = 0.25 for the
  spheroid and α = 0.44 for the disk (both uncorrected for binaries) are
  similar to those of globular clusters of moderate-to-high metallicity.

---------------------------------------------------------
Title: Electron-screening correction for the proton-proton reaction
Authors: Bahcall, John N.; Chen, Xuelei; Kamionkowski, Marc
1998PhRvC..57.2756B    Altcode: 1996astro.ph.12209B
  We test the Salpeter formalism for the electron screening of the solar
  proton-proton fusion reaction by solving numerically the relevant
  Schrödinger equation. We evaluate exactly the square of the overlap
  integral of the two-proton wave function and the deuteron wave function
  and compare with the usual analytic approximation. The usual WKB
  solution agrees with the numerical result to O(10<SUP>-4</SUP>). The
  WKB approximation should be even more precise for the other nuclear
  fusion reactions in the pp chain and CNO cycles.

---------------------------------------------------------
Title: Hans Bethe Prize Recipient: Solar Neutrinos: from Darwin to
    Bethe to Superkamiokande and SNO
Authors: Bahcall, John
1998APS..APR..I104B    Altcode:
  The nineteenth century debate on the origin of stellar energy
  generation was resolved theoretically by Hans Bethe in the late
  1930's and experimentally by Ray Davis in the 1970's. Kamiokande
  showed conclusively in the 1990s that the observed neutrinos come
  from the sun. Five beautiful experiments (chlorine, Kamiokande,
  GALLEX, SAGE, and Superkamiokande) have by now detected solar
  neutrinos, which have approximately the fluxes and energies
  predicted by calculations of nuclear fusion rates in standard solar
  models. Quantitative discrepancies between the standard model
  predictions (which assume that nothing happens to the neutrinos
  after they are created) and the measurements provide evidence that
  physics beyond the standard electroweak model may be manifested in
  solar neutrino experiments. Recent helioseismological measurements
  strengthen this inference. I will summarize the current status of &lt;A
  HREF=http://www.sns.ias.edu/ jnb/&gt;solar neutrino research&lt;/A&gt;
  and review the prospects for discovering “smoking-gun” evidence for
  new physics with the Superkamiokande, SNO, and BOREXINO detectors.

---------------------------------------------------------
Title: Solar neutrinos: where we are, what we need
Authors: Bahcall, John
1998NuPhA.631...29B    Altcode: 1998nucl.th...2050B
  This talk compares standard model predictions for solar neutrino
  experiments with the results of actual observations. Here `standard
  model' means the combined standard model of minimal electroweak
  theory plus a standard solar model. I emphasize the importance of
  recent analyses in which the neutrino fluxes are treated as free
  parameters, independent of any constraints from solar models, and
  the stunning agreement between the predictions of standard solar
  models and helioseismological measurements. In order to interpret
  solar neutrino experiments more accurately in terms of fundamental
  physics and astronomy, we need improved improved nuclear physics
  data. I describe the five most important nuclear physics problems
  whose solution is required for understanding the precise implications
  of solar neutrino experiments. Relevant preprints and references
  to other solar neutrino papers, as well as links to solar neutrino
  experiments, software, and numerical data are available at my Web site:
  http://www.sns.ias.edu/~jnb. This Web site also contains a series of
  solar neutrino viewgraphs, with explanations, that can be downloaded.

---------------------------------------------------------
Title: How uncertain are solar neutrino predictions?
Authors: Bahcall, John N.; Basu, Sarbani; Pinsonneault, M. H.
1998PhLB..433....1B    Altcode: 1998astro.ph..5135B; 1998PhLB..433..128B
  Solar neutrino fluxes and sound speeds are calculated using a systematic
  reevaluation of nuclear fusion rates. The largest uncertainties are
  identified and their effects on the solar neutrino fluxes are estimated.

---------------------------------------------------------
Title: Solar Neutrinos: Where We Are
Authors: Bahcall, J.
1998tsra.conf...99B    Altcode: 1997astro.ph..2057B
  This talk compares standard model predictions for solar neutrino
  experiments with the results of actual observations. Here `standard
  model' means the combined standard model of minimal electroweak
  theory plus a standard solar model. I emphasize the importance of
  recent analyses in which the neutrino fluxes are treated as free
  parameters, independent of any constraints from solar models, and the
  stunning agreement between the predictions of standard solar models
  and helioseismological measurements.

---------------------------------------------------------
Title: Gallium solar neutrino experiments: Absorption cross sections,
    neutrino spectra, and predicted event rates
Authors: Bahcall, John N.
1997PhRvC..56.3391B    Altcode: 1997hep.ph...10491B
  Neutrino absorption cross sections for <SUP>71</SUP>Ga are calculated
  for all solar neutrino sources with standard energy spectra, and
  for laboratory sources of <SUP>51</SUP>Cr and <SUP>37</SUP>Ar; the
  calculations include, where appropriate, the thermal energy of fusing
  solar ions and use improved nuclear and atomic data. The ratio, R, of
  measured (in GALLEX and SAGE) to calculated <SUP>51</SUP>Cr capture rate
  is R=0.95+/-0.07 (expt)+<SUP>+0.04</SUP><SUB>-0.03</SUB> (theor). Cross
  sections are also calculated for specific neutrino energies chosen so
  that a spline fit determines accurately the event rates in a gallium
  detector even if new physics changes the energy spectrum of solar
  neutrinos. Theoretical uncertainties are estimated for cross sections
  at specific energies and for standard neutrino energy spectra. Standard
  energy spectra are also presented for pp and CNO neutrino sources in the
  appendix. Neutrino fluxes predicted by standard solar models, corrected
  for diffusion, have been in the range 120 SNU to 141 SNU since 1968.

---------------------------------------------------------
Title: The Standard Solar Model
Authors: Bahcall, John
1997snns.confE...1B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Space Interferometry: the Next Frontier?
Authors: Bahcall, J. N.
1997AAS...191.2301B    Altcode: 1997BAAS...29.1249B
  The Decade Survey for Astronomy and Astrophysics in the 1990s
  recommended the development of an interferometric mission to
  “...achieve a 1000 fold improvement in our ability to measure
  celestial positions.” The design goal was to measure positions of
  widely separated objects to visual magnitude 20 with an accuracy of
  30 microarcseconds. Our futuristic hope was that the mission might
  achieve 3 microacrseconds. The design concept adopted by the NASA
  for the Space Interferometry Mission (SIM) brilliantly fulfills these
  scientific goals. The precision provided by SIM promises to open up
  a vast new frontier of scientific problems.

---------------------------------------------------------
Title: What Have We Learned from the Decade Survey for the 1990s?
Authors: Bahcall, J.
1997AAS...191.6101B    Altcode: 1997BAAS...29.1308B
  I will summarize the principal lessons that we learned in carrying
  out the Decade Survey for the 1990s and describe the most important
  objectives that were (or were not) achieved.

---------------------------------------------------------
Title: Gallium solar neutrino experiments
Authors: Bahcall, J.
1997AAS...191.2601B    Altcode: 1997BAAS...29.1253B
  Neutrino absorption cross sections for (71Ga) are calculated for
  all solar neutrino sources with standard energy spectra, and for
  laboratory sources of (51Cr) and (37Ar) ; the calculations include,
  where appropriate, the thermal energy of decaying solar ions and
  use improved nuclear and atomic data. The ratio, R, of measured
  (in GALLEX and SAGE) to calculated (51Cr) capture rate is R = 0.95
  +/- 0.07 (exp) + (+0.04}_{-0.03) (theory). Cross sections are also
  calculated for specific neutrino energies chosen so that a spline fit
  determines accurately the event rates in a gallium detector even if new
  physics changes the energy spectrum of solar neutrinos. Theoretical
  uncertainties are estimated for cross sections at specific energies
  and for standard neutrino energy spectra. Standard energy spectra are
  presented for pp and CNO neutrino sources in the appendices. Neutrino
  fluxes predicted by standard solar models, and minimal standard
  electroweak theory, when corrected for diffusion, have been in the range
  120 SNU to 141 SNU since 1968. The measured rate is 70.5 +/- 7 SNU.

---------------------------------------------------------
Title: Solar Neutrinos: News About SNUs
Authors: Bahcall, J.; Haxton, W.; Langacker, P.; Robertson, H.;
   Totsuka, Y.
1997snns.conf.....B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: An Introduction To Solar Neutrino Research
Authors: Bahcall, John
1997hep.ph...11358B    Altcode:
  The first lecture describes the conflicts between the combined
  standard model (minimal electroweak and solar) predictions and the
  results of solar neutrino experiments. The second lecture discusses
  the possibilities for detecting with solar neutrinos “smoking gun”
  indications of departures from minimal electroweak theory. Viewgraphs
  and related data are available at http://www.sns.ias.edu/~jnb .

---------------------------------------------------------
Title: Does the Sun appear brighter at night in neutrinos?
Authors: Bahcall, J. N.; Krastev, P. I.
1997PhRvC..56.2839B    Altcode: 1997hep.ph....6239B
  We calculate accurately the number of solar neutrino events expected
  as a function of solar zenith angle, with and without neutrino
  oscillations, for detectors at the locations of Super-Kamiokande, SNO,
  and the Gran Sasso National Laboratory. Using different Earth models
  to estimate geophysical uncertainties, and different solar models to
  estimate solar uncertainties, we evaluate distortions predicted by
  the Mikheyev-Smirnov-Wolfenstein (MSW) effect in the zenith angle
  distributions of solar neutrino events. The distortions are caused
  by oscillations and by ν-e interactions in the Earth that regenerate
  ν<SUB>e</SUB> from ν<SUB>μ</SUB> or ν<SUB>τ</SUB>. We show that the
  first two moments of the zenith-angle distribution are more sensitive
  to the small mixing angle MSW solution than the conventionally studied
  day-night asymmetry. We present iso-σ contours that illustrate the
  potential of Super-Kamiokande, SNO, BOREXINO, ICARUS, and HERON/HELLAZ
  for detecting the Earth regeneration effect at their actual locations
  (and at the equator). MSW solutions favored by the four pioneering
  solar neutrino experiments predict characteristic distortions for
  Super-Kamiokande, SNO, BOREXINO, and ICARUS that range from being
  unmeasurably small to &gt;5σ (stat) after only a few years of
  observations.

---------------------------------------------------------
Title: The <SUP>7</SUP>Be Electron Capture Rate in the Sun
Authors: Gruzinov, Andrei V.; Bahcall, John N.
1997ApJ...490..437G    Altcode: 1997astro.ph..2065G
  For solar conditions, we numerically integrate the density matrix
  equation for a thermal electron in the field of a <SUP>7</SUP>Be ion
  and other plasma ions and smeared-out electrons. With this technique, we
  can calculate the capture rate without either assuming the existence of
  bound states or requiring fluctuations to be spherical. Our results
  are in agreement with previous calculations that are based on a
  different physical picture, a picture that postulates the existence of
  distinct continuum and bound-state orbits for electrons. The density
  matrix calculation of the electron capture rate is independent of the
  nature of electron states in the solar plasma. To within 1% accuracy,
  the effects of screening can be described at high temperatures by a
  Salpeter-like factor of exp (-Ze<SUP>2</SUP>/kTR<SUB>D</SUB>), which can
  be derived from the density matrix equation. We show that nonspherical
  fluctuations change the reaction rate by less than 1%. The total
  theoretical uncertainty in the electron capture rate is about +/-2%.

---------------------------------------------------------
Title: ^8B Solar Neutrinos
Authors: Bahcall, John N.
1997APS..DNP..BB01B    Altcode:
  Solar neutrino astronomy began because of the expectation that the
  ^8B neutrino flux from the Sun is large enough to be measured at the
  Earth. The newest neutrino detectors, Super-Kamiokande and the soon
  to be commissioned SNO detector, will make a detailed study of the
  energy spectrum of ^8B neutrinos. In this talk, I will review the
  status of the solar neutrino problems and then focus on the state of
  our knowledge about the critical part of the solar neutrino spectrum
  coming from ^8B decay.

---------------------------------------------------------
Title: Obituaries: Lyman Spitzer, Jr.
Authors: Bahcall, John N.; Ostriker, Jeremiah P.
1997PhT....50j.123B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Localized Helioseismic Constraints on Solar Structure
Authors: Bahcall, John N.; Basu, Sarbani; Kumar, Pawan
1997ApJ...485L..91B    Altcode: 1997astro.ph..2075B
  Localized differences between the real Sun and standard solar models
  are shown to be small. The sound speeds of the real and the standard
  model Suns typically differ by less than 0.3% for regions of radial
  width ~=0.1 R<SUB>solar</SUB> in the solar core.

---------------------------------------------------------
Title: M Dwarfs from Hubble Space Telescope Star Counts. III. The
    Groth Strip
Authors: Gould, Andrew; Bahcall, John N.; Flynn, Chris
1997ApJ...482..913G    Altcode: 1996astro.ph.11157G
  We analyze the disk M dwarfs found in 31 new fields observed with
  the Wide Field Camera 2 (WFC2) on the Hubble Space Telescope,
  together with the sample previously analyzed from 22 WFC2 fields
  and 162 prerepair Planetary Camera 1 fields. The new observations,
  which include the 28 high-latitude fields comprising the Large Area
  Multi-Color Survey (Groth Strip), increase the total sample to 337
  stars, and more than double the number of late M dwarfs (M<SUB>V</SUB>
  &gt; 13.5) from 23 to 47. The mass function changes slope at M ~
  0.6 M<SUB>⊙</SUB>, from a near-Salpeter power-law index of α =
  -1.21 to α = 0.44. In both regimes, the mass function at the Galactic
  plane is given by (d<SUP>2</SUP>N)/(d log MdV)=8.1×10<SUP>-2</SUP>
  pc<SUP>-3</SUP>(M/(0.59 M<SUB>solar</SUB>))<SUP>α</SUP> . The
  correction for secondaries in binaries changes the low-mass index
  from α = 0.44 to α ~ 0.1. If the Salpeter slope continued to the
  hydrogen-burning limit, we would expect 500 stars in the last four
  bins (14.5 &lt; M<SUB>V</SUB> &lt; 18.5), instead of the 25 actually
  detected. The explanation of the observed microlensing rate toward the
  Galactic bulge requires either a substantial population of bulge brown
  dwarfs or that the disk and bulge mass functions are very different
  for stars with M &lt;~ 0.5 M<SUB>⊙</SUB>.

---------------------------------------------------------
Title: Hubble Space Telescope Images of a Sample of 20 Nearby
    Luminous Quasars
Authors: Bahcall, John N.; Kirhakos, Sofia; Saxe, David H.; Schneider,
   Donald P.
1997ApJ...479..642B    Altcode: 1996astro.ph.11163B
  Observations with the Wide-Field Camera of the Hubble Space Telescope
  (HST) are presented for a representative sample of 20 intrinsically
  luminous quasars with redshifts smaller than 0.30. These observations
  show that luminous quasars occur in diverse environments that include
  ellipticals as bright as the brightest cluster galaxies (two),
  apparently normal ellipticals (10), apparently normal spirals with H
  II regions (three), complex systems of gravitationally interacting
  components (three), and faint surrounding nebulosity (two). The
  quasar host galaxies are centered on the quasar to the accuracy of our
  measurements, 400 pc. There are more radio-quiet quasars in galaxies
  that appear to be ellipticals (seven) than in spiral hosts (three),
  contrary to expectations. However, three, and possibly five, of the
  six radio-loud quasars have detectable elliptical hosts, in agreement
  with expectations. The luminous quasars studied in this paper occur
  preferentially in luminous galaxies. The average absolute magnitude
  of the hosts is 2.2 mag brighter than expected for a field galaxy
  luminosity function. <P />The superb optical characteristics of the
  repaired HST make possible the detection of close galactic companions;
  we detect eight companion galaxies within projected distances of 10
  kpc from quasar nuclei. The presence of very close companions, the
  images of current gravitational interactions, and the higher density of
  galaxies around the quasars suggest that gravitational interactions
  play an important role in triggering the quasar phenomenon. <P
  />Based on observations with the NASA/ESA Hubble Space Telescope,
  obtained at the Space Telescope Science Institute, which is operated
  by the Association of Universities for Research in Astronomy, Inc.,
  under NASA contract NAS 5-26555.

---------------------------------------------------------
Title: Prioritizing Science: A Story of the Decade Survey for
    the 1990s
Authors: Bahcall, John N.
1997astro.ph..4255B    Altcode:
  This article summarizes the process by which astronomers and
  astrophysicists reached a consensus view as to what are the highest
  priority scientific projects for the decade of the 1990s. I also review
  the remarkable success of these recommendations.

---------------------------------------------------------
Title: Recent Highlights of Hubble Space Telescope Observations
Authors: Bahcall, John
1997APS..APR..C601B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: High Energy Neutrinos from Cosmological Gamma-Ray Burst
    Fireballs
Authors: Waxman, Eli; Bahcall, John
1997PhRvL..78.2292W    Altcode: 1997astro.ph..1231W
  Observations suggest that γ-ray bursts (GRBs) are produced by the
  dissipation of the kinetic energy of a relativistic fireball. We show
  that a large fraction, &gt;=10%, of the fireball energy is expected to
  be converted by photomeson production to a burst of ~10<SUP>14</SUP>
  eV neutrinos. A km<SUP>2</SUP> neutrino detector would observe at
  least several tens of events per year correlated with GRBs, and test
  for neutrino properties (e.g., flavor oscillations, for which upward
  moving τ's would be a unique signature, and coupling to gravity) with
  an accuracy many orders of magnitude better than is currently possible.

---------------------------------------------------------
Title: The proton-proton reaction, solar neutrinos, and a relativistic
    field theoretic model of the deuteron
Authors: Bahcall, John N.; Kamionkowski, Marc
1997NuPhA.625..893B    Altcode: 1997astro.ph..7320B
  In a series of recent papers, Ivanov et al. and Oberhummer et
  al. have calculated the rate for the p + p -&gt; d + e<SUP>+</SUP>
  + v<SUB>e</SUB> reaction with a zero-range four-fermion effective
  interaction and find a result 2.9 times higher than the standard value
  calculated from non-relativistic potential theory. Their procedure
  is shown to give a wrong answer because their assumed interaction
  disagrees with low-energy pp scattering data.

---------------------------------------------------------
Title: Globular Cluster Photometry with the Hubble Space
    Telescope.VI.WF/PC-I Observations of the Stellar Populations in the
    Core of M13 (NGC 6205)
Authors: Cohen, Randi L.; Guhathakurta, Puragra; Yanny, Brian;
   Schneider, Donald P.; Bahcall, John N.
1997AJ....113..669C    Altcode: 1996astro.ph.11151C
  We study the dense core of the globular cluster Messier 13 (NGC 6205)
  using pre-refurbishment Planetary Camera-I images obtained with the
  Hubble Space Telescope. Short exposures (60 s) through the F555W and
  F785LP filters (similar to Johnson V and I, respectively) have been used
  to obtain V and I photometry of 2877 stars brighter than V ~ 20 in a
  1.25 arcmin(2) region of the cluster including its core and extending
  out to r ~ 66(”) (2.3 pc) from its center. The sample is complete to
  V =~ 18.3 (the main sequence turnoff) and the 1sigma photometric error
  is about 0.1 mag. We find 15 blue straggler star candidates and 10 other
  possible blue stragglers in this region of M13. Their specific frequency
  is in the range F_BSS=0.04-0.07, comparable to what is observed near the
  centers of other dense clusters. A comparison between M13's observed
  V band stellar luminosity function and a theoretical model (Bergbusch
  &amp; Vandenberg 1992) for the luminosity function of an old, metal-poor
  cluster shows that the model predicts too few of the brightest red
  giants (V ~ 12.5-15) by a factor of two relative to subgiants/turnoff
  stars (&gt;6sigma effect). The radial distributions of the red giants,
  blue stragglers, and subgiants are consistent with one another, and
  are well fit by a King profile of core radius r_core=38(”}+/-6({”))
  (90% confidence limits) or 1.3 pc. Stars in the blue horizontal branch
  of M13, however, appear to be centrally depleted relative to other
  stellar types. We combine data from three dense `King model clusters',
  M13, M3, and 47 Tuc, and two post core collapse clusters, M30 and M15,
  and compare the distributions of various stellar types as a function
  of (r/r_half light) and (r/r_core). The horizontal branch stars in the
  combined sample appear to be centrally depleted relative to the giants
  (97% significance)--this depletion is only a 1sigma -2sigma effect in
  each of the clusters taken individually. The blue stragglers in the
  combined sample are centrally concentrated relative to the giants.

---------------------------------------------------------
Title: What can be learned by measuring the fluxes of the
    <SUP>7</SUP>Be and the pep solar neutrino lines?
Authors: Bahcall, J. N.; Krastev, P. I.
1997PhRvC..55..929B    Altcode: 1996astro.ph..7013B
  Measurements of the interaction rates of the solar neutrino lines
  of <SUP>7</SUP>Be and pep can be used, independent of solar models,
  to test whether electron flavor is conserved, to determine survival
  probabilities of electron-type neutrinos at specific energies,
  and to test for the existence of sterile neutrinos. We present
  analytic descriptions of these tests. We also illustrate by numerical
  simulations, assuming matter-enhanced and vacuum neutrino oscillations,
  what measurements of solar neutrino lines can teach us about neutrino
  masses and mixing angles.

---------------------------------------------------------
Title: Are Standard Solar Models Reliable?
Authors: Bahcall, John N.; Pinsonneault, M. H.; Basu, Sarbani;
   Christensen-Dalsgaard, J.
1997PhRvL..78..171B    Altcode: 1996astro.ph.10250B
  The sound speeds of solar models that include element diffusion
  agree with helioseismological measurements to a rms discrepancy
  of better than 0.2% throughout almost the entire Sun. Models that
  do not include diffusion, or in which the interior of the Sun is
  assumed to be significantly mixed, are effectively ruled out by
  helioseismology. Standard solar models predict the measured properties
  of the Sun more accurately than is required for applications involving
  solar neutrinos.

---------------------------------------------------------
Title: Neutrino oscillations and moments of electron spectra
Authors: Bahcall, J. N.; Krastev, P. I.; Lisi, E.
1997PhRvC..55..494B    Altcode: 1996nucl.ex..10010B
  We show that the effects of neutrino oscillations on <SUP>8</SUP>B solar
  neutrinos are described well by the first two moments (the average
  and the variance) of the energy distribution of scattered or recoil
  electrons. For the SuperKamiokande and the Sudbury Neutrino Observatory
  experiments, the differences between the moments calculated with
  oscillations and the standard, no-oscillation moments are greater than
  three standard deviations for a significant fraction of the neutrino
  mass-mixing (Δm<SUP>2</SUP>,sin<SUP>2</SUP>2θ) parameter space.

---------------------------------------------------------
Title: HST Images of Twenty Nearby Luminous Quasars
Authors: Bahcall, J. N.; Kirhakos, S.; Schneider, D. P.
1997quho.conf...37B    Altcode: 1996quho.conf...37B
  No abstract at ADS

---------------------------------------------------------
Title: Solar neutrinos: solved and unsolved problems.
Authors: Bahcall, J. N.
1997upa..conf..195B    Altcode:
  This paper answers a series of questions. Why study solar
  neutrinos? What does the combined standard model (solar plus
  electroweak) predict for solar neutrinos? Why are the calculations of
  neutrino fluxes robust? What are the three solar neutrino problems? What
  have we learned in the first 30 years of solar neutrino research? For
  the next decade, what are the most important solvable problems in
  the physics of solar neutrinos? What are the most important solvable
  problems in the astrophysics of solar neutrinos?

---------------------------------------------------------
Title: Hubble Space Telescope Images of a Sample of Twenty Nearby
    Luminous Quasars
Authors: Bahcall, J. N.; Kirhakos, S.; Saxe, D. H.; Schneider, D. P.
1997hsth.conf..387B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Unsolved Problems in Astrophysics
Authors: Bahcall, John N.; Ostriker, Jeremiah P.
1997upa..conf.....B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: How well do standard solar models describe the results of
    solar neutrino experiments?
Authors: Bahcall, J. N.
1997MmSAI..68..361B    Altcode: 1996astro.ph..6161B
  The neutrino fluxes calculated from the 14 standard solar models
  published recently in refereed journals are inconsistent with the
  results of the 4 pioneering solar neutrino experiments if nothing
  happens to the neutrinos after they are created in the solar
  interior. The calculated fluxes and the experimental results are in
  good agreement if neutrino oscillations occur.

---------------------------------------------------------
Title: Is H_0 Well Defined?
Authors: Bahcall, John N.
1996PASP..108.1097B    Altcode:
  As moderator, I very much enjoyed the high level of scientific
  discussion and wondered if the residual disagreement might be caused
  by different operational definitions of H_0. (SECTION: A Debate on
  The Scale of the Universe)

---------------------------------------------------------
Title: Helioseismology, Solar Models, and Solar Neutrinos
Authors: Bahcall, J. N.; Pinsonneault, M. H.
1996AAS...189.5601B    Altcode: 1996BAAS...28.1346B
  We compare with helioseismological measurements the sound speeds
  computed from solar models that we have developed to calculate
  solar neutrino fluxes. The agreement is spectacularly good throughout
  essentially the entire sun. Solar models that do not include diffusion,
  or in which the interior of the sun is assumed to be significantly
  mixed, are ruled out by helioseismology. Standard solar models predict
  the measured properties of the sun more accurately than is required
  for applications involving solar neutrinos. These results strengthen
  the case that the discrepancies between observed and predicted solar
  neutrino fluxes are due to new physics.

---------------------------------------------------------
Title: Tests of electron flavor conservation with the Sudbury
    Neutrino Observatory
Authors: Bahcall, John N.; Lisi, Eligio
1996PhRvD..54.5417B    Altcode: 1996hep.ph....7433B
  We analyze tests of electron flavor conservation that can be performed
  at the Sudbury Neutrino Observatory (SNO). These tests, which utilize
  <SUP>8</SUP>B solar neutrinos interacting with deuterium, measure
  (1) the shape of the recoil electron spectrum in charged-current (CC)
  interactions (the CC spectrum shape), and (2) the ratio of the number
  of charged-current to neutral current (NC) events (the CC/NC ratio). We
  determine standard model predictions for the CC spectral shape and for
  the CC/NC ratio, together with realistic estimates of their errors and
  the correlations between errors. We consider systematic uncertainties
  in the standard neutrino spectrum and in the charged-current and
  neutral current cross sections, the SNO energy resolution and absolute
  energy scale, and the SNO detection efficiencies. Assuming that either
  matter-enhanced or vacuum neutrino oscillations solve the solar neutrino
  problems, we calculate the confidence levels with which electron flavor
  nonconservation can be detected using either the CC spectrum shape or
  the CC/NC ratio, or both. If the SNO detector works as expected, the
  neutrino oscillation solutions that best fit the results of the four
  operating solar neutrino experiments can be distinguished unambiguously
  from the standard predictions of electron flavor conservation.

---------------------------------------------------------
Title: Status of Solar Models
Authors: Bahcall, John N.; Pinsonneault, Marc H.
1996hep.ph...10542B    Altcode:
  The neutrino fluxes calculated from 14 standard solar models published
  recently in refereed journals are inconsistent with the results of
  the 4 pioneering solar neutrino experiments if nothing happens to the
  neutrinos after they are created in the solar interior. The sound speeds
  calculated from standard solar models are in excellent agreement with
  helioseismological measurements of sound speeds. Some statements made
  by Dar at Neutrino 96 are answered here.

---------------------------------------------------------
Title: The Hubble Space Telescope Quasar Absorption Line Key
Project: The Unusual Absorption-Line System in the Spectrum of PG
    2302+029---Ejected or Intervening?
Authors: Jannuzi, B. T.; Hartig, G. F.; Kirhakos, S.; Sargent,
   W. L. W.; Turnshek, D. A.; Weymann, R. J.; Bahcall, J. N.; Bergeron,
   J.; Boksenberg, A.; Savage, B. D.; Schneider, D. P.; Wolfe, A. M.
1996ApJ...470L..11J    Altcode: 1996astro.ph..8080J
  We report the discovery of a high-ionization broad absorption line
  system at a redshift of zabs = 0.695 in the spectrum of the zem = 1.052
  radio-quiet quasar PG 2302+029. Broad absorption with FWHM from 3000
  to 5000 km s-1 is detected from C IV, N V, and O VI in Hubble Space
  Telescope (HST) Faint Object Spectrograph spectra of the quasar. A
  narrow-line system (FWHM ~ 250 km s-1) at zabs = 0.7016 is resolved
  from the broad blend and includes absorption by Ly alpha and the C IV,
  N V, and O VI doublets. No absorption by low-ionization metal species
  (e.g., Si II and Mg II) is detected in the HST or ground-based spectra
  for either the broad or the narrow system. The centroids of the broad
  system lines are displaced by ~56,000 km s-1 to the blue of the quasar's
  broad emission lines. The reddest extent of the broad-line absorption is
  more than 50,000 km s-1 from the quasar. The properties of this system
  are unprecedented, whether it is an intervening or an ejected system.

---------------------------------------------------------
Title: Neutrino astronomy: the Sun and beyond.
Authors: Bahcall, J.; Halzen, F.
1996PhyW....9...41B    Altcode:
  Neutrinos might be difficult to detect, but a new generation of
  experiments and telescopes could open new areas of particle physics
  and regions of the universe that cannot be seen with photons.

---------------------------------------------------------
Title: Galaxy Clustering around Nearby Luminous Quasars
Authors: Fisher, Karl B.; Bahcall, John N.; Kirhakos, Sofia; Schneider,
   Donald P.
1996ApJ...468..469F    Altcode: 1996astro.ph..2078F
  We examine the clustering of galaxies around a sample of 20 luminous low
  redshift ( z &lt;~ 0.30) quasars observed with the Wide Field Camera-2
  on the Hubble Space Telescope (HST). The HST resolution makes possible
  galaxy identification brighter than V = 24.5 and as close as 1" or 2"
  to the quasar. We find a significant enhancement of galaxies within a
  projected separation of &lt;~ 100 h^-1^ kpc of the quasars. If we model
  the QSO/galaxy correlation function as a power law with a slope given by
  the galaxy/galaxy correlation function, we find that the ratio of the
  QSO/galaxy to galaxy/galaxy correlation functions is 3.8 +/- 0.8. The
  galaxy counts within r &lt; 15 h^-1^ kpc of the quasars are too high
  for the density profile to have an appreciable core radius (~&gt;100
  h^-1^ kpc). Our results reinforce the idea that low redshift quasars
  are located preferentially in groups of 10-20 galaxies rather than
  in rich clusters. We see no significant difference in the clustering
  amplitudes derived from radio-loud and radio-quiet subsamples.

---------------------------------------------------------
Title: Hubble Deep Field Constraint on Baryonic Dark Matter
Authors: Flynn, Chris; Gould, Andrew; Bahcall, John N.
1996ApJ...466L..55F    Altcode: 1996astro.ph..3035F
  We use a new technique to search for faint red stars in the Hubble deep
  field. We distinguish unambiguously between stars and galaxies to I =
  26.3. Our results place strong and general constraints on the I-band
  luminosity of the constituents of the Galactic dark halo.

---------------------------------------------------------
Title: Solar Neutrinos: Where We Are, Where We Are Going
Authors: Bahcall, John N.
1996ApJ...467..475B    Altcode: 1995hep.ph...12285B
  This paper answers a series of questions: Why study solar
  neutrinos? What does the combined standard model (solar plus
  electroweak) predict for solar neutrinos? Why are the calculations of
  neutrino fluxes robust? What are the three solar neutrino problems? What
  have we learned in the first 30 years of solar neutrino research? For
  the next decade, what are the most important solvable problems in
  the physics of solar neutrinos? What are the most important solvable
  problems in the astrophysics of solar neutrinos?

---------------------------------------------------------
Title: Disk M Dwarf Luminosity Function from Hubble Space Telescope
    Star Counts
Authors: Gould, Andrew; Bahcall, John N.; Flynn, Chris
1996ApJ...465..759G    Altcode: 1995astro.ph..5087G
  We study a sample of 257 Galactic disk M dwarfs (8 ≤ M<SUB>v</SUB>
  ≤ 18.5) found in images obtained using the Hubble Space Telescope
  (HST). These include 192 stars in 22 fields imaged with the repaired
  Wide Field Camera (WFC2) with mean limiting mag I = 23.7 and 65 stars
  in 162 fields imaged with the prerepair Planetary Camera (PC 1)
  with mean limiting mag V = 21.3. We find that the disk luminosity
  function (LF) drops sharply for M<SUB>v</SUB> &gt; 12 (M &lt; 0.25
  M<SUB>sun</SUB>), decreasing by a factor ≥ 3 by M<SUB>v</SUB> ∼
  14 (M ∼ 0.14 M<SUB>sun</SUB>). This decrease in the LF is in good
  agreement with the ground-based photometric study of nearby stars by
  Stobie, Ishida, &amp; Peacock, and in mild conflict with the most recent
  LF measurements based on local parallax stars by Reid, Hawley, &amp;
  Gizis. The local LF of the faint Galactic disk stars can be transformed
  into a local mass function using an empirical mass-M<SUB>v</SUB>
  relation. The mass function can be represented analytically over
  the mass range 0.1 M<SUB>sun</SUB> &lt; M &lt; 1.6 M<SUB>sun</SUB>
  by log (φ) = -1.35 - 1.33 log (M/M<SUB>sun</SUB>) - 1.82[log
  (M/M<SUB>sun</SUB>)]<SUP>2</SUP>, where φ is the number density
  per logarithmic unit of mass. The total column density of M stars
  is only Σ<SUB>M</SUB> = 12.4±1.9 M<SUB>sun</SUB> pc<SUP>-2</SUP>,
  implying a total "observed" disk column density of Σ<SUB>obs</SUB>
  ≃ 40 M<SUB>sun</SUB> pc<SUP>-2</SUP>, lower than previously believed,
  and also lower than all estimates with which we are familiar of the
  dynamically inferred mass of the disk. The measured scale length for
  the M-star disk is 3.0±0.4 kpc. The optical depth to microlensing
  toward the Large Magellanic Cloud (LMC) by the observed stars in
  the Milky Way disk is τ ≤ 1 x 10<SUP>-8</SUP>, compared to the
  observed optical depth found in ongoing experiments τ<SUB>obs</SUB>
  ∼ 10<SUP>-7</SUP>. The M-stars show evidence for a population
  with characteristics intermediate between thin disk and spheroid
  populations. Approximating what may be a continuum of populations
  by two separate components, we find a vertical density profile v(z)
  ∝ 0.80 sech<SUP>2</SUP> (z/323 pc) + 0.20 exp (- |z|/656 pc). If
  we combine the HST data with ground-based measurements of the local
  density of M dwarfs, then a traditional double-exponential vertical
  density profile is strongly excluded.

---------------------------------------------------------
Title: Solar neutrino experiments: The next generation
Authors: Bahcall, John N.; Calaprice, Frank; McDonald, Arthur B.;
   Totsuka, Yoji
1996PhT....49g..30B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Standard neutrino spectrum from <SUP>8</SUP>B decay
Authors: Bahcall, John N.; Lisi, E.; Alburger, D. E.; de Braeckeleer,
   L.; Freedman, S. J.; Napolitano, J.
1996PhRvC..54..411B    Altcode: 1996nucl.th...1044B
  We present a systematic evaluation of the shape of the neutrino energy
  spectrum produced by beta decay of <SUP>8</SUP>B. We place special
  emphasis on determining the range of uncertainties permitted by existing
  laboratory data and theoretical ingredients (such as forbidden and
  radiative corrections). We review and compare the available experimental
  data on the <SUP>8</SUP>B(β<SUP>+</SUP>)<SUP>8</SUP>Be(2α) decay
  chain. We analyze the theoretical and experimental uncertainties
  quantitatively. We give a numerical representation of the best-fit
  (standard-model) neutrino spectrum, as well as two extreme deviations
  from the standard spectrum that represent the total (experimental and
  theoretical) effective +/-3σ deviations. Solar neutrino experiments
  that are currently being developed will be able to measure the shape
  of the <SUP>8</SUP>B neutrino spectrum above about 5 MeV. An observed
  distortion of the <SUP>8</SUP>B solar neutrino spectrum outside the
  range given in the present work could be considered as evidence, at an
  effective significance level greater than three standard deviations,
  for physics beyond the standard electroweak model. We use the most
  recent available experimental data on the Gamow-Teller strengths in the
  A=37 system to calculate the <SUP>8</SUP>B neutrino absorption cross
  section on chlorine: σ<SUB>Cl</SUB>=(1.14+/-0.11)×10<SUP>-42</SUP>
  cm<SUP>2</SUP> (+/-3σ errors). The chlorine cross section
  is also given as a function of the neutrino energy. The
  <SUP>8</SUP>B neutrino absorption cross section in gallium is
  σ<SUB>Ga</SUB>=(2.46<SUP>+2.1</SUP><SUB>-1.1</SUB>)×10<SUP>-42</SUP>
  cm<SUP>2</SUP> (+/-3σ errors).

---------------------------------------------------------
Title: Solar Neutrinos: Where We Are, Where We Are Going
Authors: Bahcall, John N.
1996NuPhS..48..309B    Altcode:
  This talk answers the following questions. Why study solar
  neutrinos? What does the combined standard model (solar plus
  electroweak) predict for solar neutrinos? Why are the calculations of
  neutrino fluxes robust? What are the three solar neutrino problems? What
  have we learned in the first thirty years of solar neutrino research?

---------------------------------------------------------
Title: How well do we (and will we) know solar neutrino fluxes and
    oscillation parameters\?
Authors: Bahcall, J. N.; Krastev, P. I.
1996PhRvD..53.4211B    Altcode: 1995hep.ph...12378B
  Individual neutrino fluxes are not well determined by the four
  operating solar neutrino experiments. Assuming neutrino oscillations
  occur, the pp electron neutrino flux is uncertain by a factor of 2,
  the <SUP>8</SUP>B flux by a factor of 5, and the <SUP>7</SUP>Be
  flux by a factor of 45. For matter-enhanced oscillation (MSW)
  solutions, the range of allowed differences of squared neutrino
  masses, Δm<SUP>2</SUP>, varies between 4×10<SUP>-6</SUP>
  eV<SUP>2</SUP> and 1×10<SUP>-4</SUP> eV<SUP>2</SUP>, while
  4×10<SUP>-3</SUP>&lt;=sin<SUP>2</SUP>2θ&lt;=1.5×10<SUP>-2</SUP>
  or 0.5&lt;=sin<SUP>2</SUP>2θ&lt;=0.9. For vacuum oscillations,
  Δm<SUP>2</SUP> varies between 5×10<SUP>-11</SUP>
  eV<SUP>2</SUP> and 1×10<SUP>-10</SUP> eV<SUP>2</SUP>, while
  0.7&lt;=sin<SUP>2</SUP>2θ&lt;=1.0. The inferred ranges of
  neutrino parameters depend only weakly on which standard solar
  model is used. Calculations of the expected results of future
  solar neutrino experiments (SuperKamiokande, SNO, BOREXINO, ICARUS,
  HELLAZ, and HERON) are used to illustrate the extent to which these
  experiments will restrict the range of the allowed neutrino mixing
  parameters. For example, the double ratio (observed ratio divided
  by standard model ratio) of neutral current to charged current
  event rates to be measured in the SNO experiment varies, at 95%
  confidence limit, over the range 1.0 (no oscillations into active
  neutrinos), 3.1<SUP>+1.8</SUP><SUB>-1.3</SUB> (small mixing angle
  MSW), 4.4<SUP>+2.0</SUP><SUB>-1.4</SUB> (large mixing angle MSW), and
  5.2<SUP>+5.6</SUP><SUB>-2.9</SUB> (vacuum oscillations). We present an
  improved formulation of the “luminosity constraint” and show that at
  95% confidence limit, this constraint establishes the best available
  limits on the rate of creation of pp neutrinos in the solar interior
  and provides the best upper limit to the <SUP>7</SUP>Be neutrino
  flux. The actual rate of creation of solar neutrinos in the solar
  interior to the rate predicted by the standard solar model can vary
  (while holding the CNO neutrino flux constant) between 0.55 and 1.08
  for pp neutrinos and between 0.0 and 6.35 for <SUP>7</SUP>Be neutrinos.

---------------------------------------------------------
Title: Temperature dependence of solar neutrino fluxes
Authors: Bahcall, John N.; Ulmer, Andrew
1996PhRvD..53.4202B    Altcode: 1996astro.ph..2012B
  By comparing neutrino fluxes and central temperatures calculated from
  1000 detailed numerical solar models, we derive improved scaling laws
  which show how each of the neutrino fluxes depends upon the central
  temperature (flux ~T<SUP>m</SUP>) we also estimate uncertainties
  for the temperature exponents. With the aid of a one-zone model of
  the Sun, we derive expressions for the temperature exponents of
  the neutrino fluxes. For the most important neutrino fluxes, the
  exponents calculated with the one-zone model agree to within 20%
  or better with the exponents extracted from the detailed numerical
  models. The one-zone model provides a physical understanding of the
  temperature dependence of the neutrino fluxes. For the pp neutrino flux,
  the one-zone model explains the (initially surprising) dependence of
  the flux upon a negative power of the temperature and suggests a new
  functional dependence. This new function makes explicit the strong
  anticorrelation between the <SUP>7</SUP>Be and pp neutrino fluxes. The
  one-zone model also predicts successfully the average linear relations
  between neutrino fluxes, but cannot predict the appreciable scatter in
  a Δφ<SUB>i</SUB>/φ<SUB>i</SUB> versus Δφ<SUB>j</SUB>/φ<SUB>j</SUB>
  diagram.

---------------------------------------------------------
Title: Improved limit on charge conservation derived from
    <SUP>71</SUP>Ga solar neutrino experiments
Authors: Norman, Eric B.; Bahcall, John N.; Goldhaber, Maurice
1996PhRvD..53.4086N    Altcode:
  The reported counting rates of the SAGE and GALLEX
  solar neutrino detectors have been used to establish
  an improved limit on the charge-nonconserving decay
  <SUP>71</SUP>--&gt;<SUP>71</SUP>Ge+neutrals. The 1σ lower limit on
  the lifetime against such decays is 3.5×10<SUP>26</SUP> yr. This
  result can be used to establish a 1σ upper limit on the ratio
  of the charge-nonconserving to the normal weak interaction decay
  width of the neutron, Γ(n--&gt;p+ν<SUB>e</SUB>+ν¯<SUB>e</SUB>)/Γ
  (n--&gt;p+e<SUP>-</SUP>+ν¯<SUB>e</SUB>)&lt;=8×10<SUP>-27</SUP>. This
  result represents by far the most stringent limit yet derived for
  charge-nonconserving decays involving baryons.

---------------------------------------------------------
Title: The Apparently Normal Galaxy Hosts for Two Luminous Quasars
Authors: Bahcall, John N.; Kirhakos, Sofia; Schneider, Donald P.
1996ApJ...457..557B    Altcode: 1995astro.ph..9031B
  HST images (with WFPC2) of PHL 909 (z = 0.171) and PG 0052+251 (z =
  0.155) show that these luminous radio-quiet quasars each occur in
  an apparently normal host galaxy. The host galaxy of PHL 909 is an
  elliptical galaxy (∼E4), and the host of PG 0052+251 is a spiral
  (∼Sb). Both host galaxies are several tenths of a magnitude brighter
  than L<SUP>*</SUP>, the characteristic Schechter luminosity of field
  galaxies. <P />The images of PHL 909 and PG 0052+251, when compared with
  HST images of other objects in our sample of 20 luminous, small-redshift
  (z ≤ 0.30) quasars, show that luminous quasars occur in a variety of
  environments. The local environments of the luminous quasars range from
  luminous ellipticals to apparently normal host galaxies, to complex
  systems of interacting components, to faint (and as yet undetected)
  hosts. <P />The bright H II regions of the host galaxy of PG 0052+251
  provide an opportunity to measure directly the metallicity of the
  host of a luminous quasar, to establish an upper limit to the mass
  of the nuclear AGN (i.e., the putative black hole source), and to
  test stringently the cosmological hypothesis that the galaxy and the
  quasar are both at the distance indicated by the quasar redshift. <P
  />The moderately luminous host galaxies of PHL 909 and PG 0052+251 are
  obvious on the HST images. Normalizing the limits of detectability using
  short exposures in which the host galaxies of PHL 909 and PG 0052+251
  are easily observed, we estimate that we could have detected similar
  host galaxies as faint as 0.5 magnitudes less than L<SUP>*</SUP> in the
  longer exposure HST images that have not yet shown host galaxies. The
  details of the PSF subtraction are unimportant for the determination
  of the host galaxy morphologies and luminosities; the major and minor
  axes measured by subtracting very different stellar PSFs are the same
  to ±5% and the host galaxy magnitudes are the same to ±0.1 mag.

---------------------------------------------------------
Title: How does the sun shine?
Authors: Bahcall, J. N.; Fukugita, M.; Krastev, P. I.
1996PhLB..374....1B    Altcode: 1996astro.ph..2065B
  Assuming that MSW neutrino oscillations occur and ignoring all solar
  physics except for the constraint that nuclear fusion produces the
  solar luminosity, we show that new solar neutrino experiments are
  required to rule out empirically the hypothesis that the sun shines
  via the CNO cycle.

---------------------------------------------------------
Title: Observational Searches for Solar g-Modes: Some Theoretical
    Considerations
Authors: Kumar, Pawan; Quataert, Eliot J.; Bahcall, John N.
1996ApJ...458L..83K    Altcode: 1995astro.ph.12091K
  We argue that the solar g-modes are unlikely to have caused the discrete
  peaks in the power spectrum of the solar wind flux observed by Thomson
  et al (1995). The lower limit to the energy of individual g-modes,
  using the amplitudes given by Thomson et al., is estimated to be at
  least 1036 ergs for low-order g-modes; the resulting surface velocity
  amplitude is at least 50 cm s-1, larger than the observational upper
  limit (5 cm s-1). We suggest that the most likely source for the
  excitation of solar g-modes is turbulent stresses in the convection
  zone. The surface velocity amplitude of low-degree and low-order
  g-modes resulting from this process is estimated to be of order 10-2 cm
  s-1. This amplitude is interestingly close to the detection threshold of
  the SOHO satellite. The long lifetime of g-modes (~106 yr for low-order
  modes) should be helpful in detecting these small-amplitude pulsations.

---------------------------------------------------------
Title: Preliminary Study of the Stellar Populations and Density
    Profile of NGC 6624 Using LIST
Authors: Guhathakurta, P.; Yanny, B.; Bahcall, J. N.; Schneider, D. P.
1996IAUS..174..333G    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Hubble Space Telescope Studies of the Dense Central Regions
    of Globular Clusters
Authors: Guhathakurta, P.; Yanny, B.; Schneider, D. P.; Bahcall, J. N.
1996IAUS..174...19G    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Hubble Space Telescope Quasar Absorption Line Key
    Project. VII. Absorption Systems at Z abs &lt;= 1.3
Authors: Bahcall, John N.; Bergeron, Jacqueline; Boksenberg, Alec;
   Hartig, George F.; Jannuzi, Buell T.; Kirhakos, Sofia; Sargent,
   W. L. W.; Savage, Blair D.; Schneider, Donald P.; Turnshek, David A.;
   Weymann, Ray J.; Wolfe, Arthur M.
1996ApJ...457...19B    Altcode: 1995astro.ph..6124B
  We present evidence that clumps of Lyα lines are physically associated
  with about half of the extensive metal-line systems (absorption systems
  with four or more observed metal-line species) found in this paper,
  demonstrate that all four Lyman-limit systems discussed here correspond
  to extensive metal-line absorption systems, and present an extraordinary
  pair of extensive metal-line absorption systems within 2000 km s^-1^
  of each other at z = 0.95 that are probably an early manifestation of
  large-scale structure. These results are obtained using ultraviolet
  spectra, taken with the higher resolution gratings of the Faint Object
  Spectrograph of the Hubble Space Telescope (HST) for four quasars
  with emission-line redshifts between 1.0 and 1.3. We also determine
  the evolution of Lyα absorption lines at redshifts less than 1.3 by
  combining the results for 13 smaller redshift quasars discussed in Paper
  I of this series with the results for the four moderate redshift quasars
  analyzed in the present paper. Absorption lines were selected, measured,
  and identified algorithmically using software tested by Monte Carlo
  simulations. A total of 291 absorption lines, all with a statistical
  significance above a specified high threshold level, were selected and
  measured. A total of 145 lines are identified as extragalactic Lyα
  absorption lines. Ten of the Lyα absorption lines are found at the same
  redshifts as metal-line systems. Monte Carlo simulations with pseudo-C
  IV or O VI doublets were carried out to determine the probability that
  a pair of absorption lines might accidentally have the appropriate
  separation to be identified as either a C IV or an O VI absorption
  doublet. The average number of pseudo-C IV doublets found in the real
  (observed) spectra varies from 0.05 to 2.4 per spectrum within the Lyα
  forest and is negligible outside the Lyα forest. For z_abs_ &lt;= 1.3,
  the density of Lyα lines with equivalent widths greater than 0.24
  A is adequately fitted by dN/dz = (dN/dz)_0_(1 + z)<SUP>gamma</SUP>^
  with (dN/dz)_0_ = 24.3 +/- 6.6 Lyα lines per unit redshift, and γ
  = 0.58 +/- 0.50 (1 σ uncertainties). This rate of evolution at low
  redshifts is less than the evolutionary rate inferred from several
  different ground-based data samples that pertain to high redshifts,
  although neither the available HST data nor the ground-based data
  are sufficiently extensive to establish whether this change occurs
  abruptly or gradually. The four Lyman-limit systems that are present
  in the spectra analyzed here all correspond to extensive metal-line
  systems. This result provides further circumstantial evidence that
  many Lyman-limit systems (like many metal-line absorption systems)
  are associated with galaxies. Eight extensive metal-line systems with
  between five and 15 strong metal lines are identified. An approximate
  estimate for the frequency of such systems is dN/dz ~ 2.5(1 + z)^0.5^
  systems per unit redshift of dN/dz ~ 2.0(1 + z)^1.0^ systems per unit
  redshift. About half of the extensive metal-line systems are accompanied
  by clumps of neighboring (in redshift space) Lyα absorption lines,
  corresponding to velocity dispersions of 600-1400 km s^-1^. In addition,
  two of the extensive metal systems, found in the spectrum PKS 0122-00
  at z = 0.9667 and z = 0.9531, are probably physically associated,
  since they are separated by only 2000 km s^-1^. We suggest that the
  metal-line systems with associated clumps of Lyα lines and the linked
  pair of metal-line systems seen in the spectrum of PKS 0122-00, may
  correspond to clusters, or possibly superclusters, of galaxies. The
  observed gaseous structures at redshifts of 0.5-1.0 with velocity
  dispersions of 6 x 102 to 1.4 x 10- km ski (or velocity spans of 1.2 x
  10- to 3 x 10- km ~/1) constitute a constraint on cosmological models
  of structure formation. The local mean free path (the reciprocal of
  the number density times radius squared) for the clumps of Ly(alpha)
  absorptions and metal-line systems is 10^-4^ Mpc^-1^. The clumps
  of Lyα absorption lines clustered about metal-line systems and the
  inferred rate of evolution of low and moderate redshift Lyα absorption
  lines more clearly resemble the properties of galaxies and of metal
  containing absorption line systems than they do the properties of
  the high-redshift Lyα forest lines. These results are consistent
  with two different populations of Lyα absorption lines, with type 1
  being closely associated with galaxies and evolving slowly and type
  2 being relative unclustered, evolving more rapidly, and dominating
  the observations at large redshift.

---------------------------------------------------------
Title: Galaxy Clustering Around Nearby Luminous Quasars
Authors: Fisher, Karl B.; Bahcall, John N.; Kirhakos, Sofia; Schneider,
   Donald P.
1996STIN...9621450F    Altcode:
  We examine the clustering of galaxies around a sample of 20 luminous
  low redshift (z approximately less than 0.30) quasars observed with the
  Wide Field Camera-2 on the Hubble Space Telescope. The HST resolution
  makes possible galaxy identification brighter than V = 24.5 and as
  close as 2 arc-seconds to the quasar. We find a significant enhancement
  of galaxies within a projected separation of approximately less than
  100 (h exp -1)kpc of the quasars. The galaxy distribution around
  the quasars inconsistent with the observed slope of the galaxy/galaxy
  correlation function, but has an amplitude 3.8 +/- 0.8 times larger. The
  galaxy counts within r less than 15 (h exp -1)kpc of the quasars are
  too high for the density profile to have an appreciable core radius
  (approximately greater than 100 (h exp -1)kpc). Our results reinforce
  the idea that low redshift quasars are located preferentially in groups
  of 10-20 galaxies rather than in rich clusters. We see no significant
  difference in the clustering amplitudes derived from radio-loud and
  radio-quiet subsamples.

---------------------------------------------------------
Title: Monte Carlo Exploration of Mikheyev-Smirnov-Wolfenstein
    Solutions to the Solar Neutrino Problem
Authors: Shi, X.; Schramm, D. N.; Bahcall, J. N.
1996bboe.book..701S    Altcode:
  We explore the impact of astrophysical uncertainties on the
  Mikheyev-Smirnov-Wolfenstein (MSW) solution by calculating the allowed
  MSW solutions for 1000 different solar models with a Monte Carlo
  selection of solar model input parameters, assuming a full three-family
  MSW mixing. Applications are made to the chlorine, gallium, Kamiokande,
  and Borexino experiments. The initial GALLEX result limits the mixing
  parameters to the upper diagonal and the vertical regions of the MSW
  triangle. We also calculate the expected event rates in the Borexino
  experiment assuming the MSW solutions implied by GALLEX.

---------------------------------------------------------
Title: Solar interior and solar neutrinos.
Authors: Bahcall, J. N.
1996stsu.conf..279B    Altcode:
  The following topics were dealt with: nuclear fusion reactions in the
  Sun; the chlorine solar neutrino experiment; chlorine versus Kamiokande;
  GALLEX and SAGE.

---------------------------------------------------------
Title: Globular Cluster Photometry With the Hubble Space
    Telescope. V. WFPC Study of M15's Central density Cusp
Authors: Guhathakurta, Puragra; Yanny, Brian; Schneider, Donald P.;
   Bahcall, John N.
1996AJ....111..267G    Altcode: 1995astro.ph.12015G
  We describe images of the center of the dense globular cluster M15
  (NGC 7078) obtained with the Hubble Space Telescope Wide Field
  and Planetary Camera 2 (WFPC2). Data taken in the F336W, F439W,
  and F555W filters (approximately U, B, and V) are used to study
  the surface density distribution of the ∼3×10<SUP>4</SUP> stars
  detected in a 5 arcmin<SUP>2</SUP> region within r&lt;2' (6.7 pc)
  of the cluster center. Realistic simulated images have been used to
  estimate photometric errors and incompleteness in the star counts,
  which are strong functions of stellar brightness and radius. We have
  used a combination of point-spread-function fitting and aperture
  photometry, a technique that yields more accurate photometry than
  either method alone on the undersampled WFPC2 images of crowded
  star fields. The error in photometry is 1σ∼0.05 mag for stars
  with V&lt;18; this increases to 1σ∼0.2 mag at V=20.5, which is
  1.5 mag fainter than the main-sequence turnoff. The surface density
  of stars in M15 (after correction for the effects of incompleteness
  and photometric bias/scatter) is well represented by a power law in
  radius: N(r)∼r<SUP>-0.82±0.12,</SUP>, over the radial range 0:3
  (0.017 pc) to 6". The observed power law is remarkably similar to
  what is expected if the center of the cluster harbors a massive black
  hole. Nonparametric estimates of the density profile show a monotonic
  rise with decreasing radius all the way in to r=0".3, the smallest
  radius at which the density can be reliably measured; there is no
  indication that the profile flattens at smaller radii. Any flat core
  of radius larger than 2" (0.11 pc) in the stellar distribution is
  ruled out at the ≳9S% significance level. The star count profile
  is consistent with that expected from core-collapse models or with
  the predicted distribution around a massive (few times 10<SUP>3</SUP>
  M<SUB>sun</SUB>) black hole. The close triplet of bright stars, AC 214,
  is within 0".5 (1.5σ) of the cluster centroid position. The projected
  density distribution of stars within the central 15" of M15 departs from
  circular symmetry at the 95% level, with an ellipticity e=0.05±0.04
  (90% confidence limits) at a position angle of +60°±25°, consistent
  with the rotation measured by Gebhardt et al. (1995) in this region
  of the cluster.

---------------------------------------------------------
Title: PKS 2349-014: A Luminous Quasar with Thin Wisps, a Large
Off-Center Nebulosity, and a Close Companion Galaxy: Erratum
Authors: Bahcall, John N.; Kirhakos, Sofia; Schneider, Donald P.
1995ApJ...454L.175B    Altcode:
  In the Letter "PKS 2349-014: A Luminous Quasar with Thin Wisps,
  a Large Off-Center Nebulosity, and a Close Companion Galaxy,"
  by John N. Bahcall, Sofia Kirhakos, and Donald P. Schneider (ApJ,
  447, L1 [1995]), there is an error in the next to last paragraph
  (before the acknowledgments), second sentence. An exponent is given
  incorrectly. The sentence should read: "If we suppose that we have
  observed ... the required number density of black holes to be ~10-4
  Mpc-3 R^{-2}<SUB>20</SUB> ...." (The superscript -1 has been changed
  to a -4.)

---------------------------------------------------------
Title: Hubble Space Telescope and MERLIN Observations of the Jet in
    3C 273
Authors: Bahcall, J. N.; Kirhakos, S.; Schneider, D. P.; Davis, R. J.;
   Muxlow, T. W. B.; Garrington, S. T.; Conway, R. G.; Unwin, S. C.
1995ApJ...452L..91B    Altcode: 1995astro.ph..9028B
  We present red and blue images of the jet of the quasar 3C 273 obtained
  with the WFPC2 on the Hubble Space Telescope as well as a new radio
  map made with the MERLIN array. The images are of significantly better
  quality than those of previous data. The two maps are aligned to an
  accuracy of 0."020; this accuracy is achieved because both the quasar
  and the jet are contained in both the radio and optical images. The
  start of the optical jet is marked by an elongated knot which appears
  identical at radio and optical wavelengths. Other knots in the optical
  jet correspond to narrow oblique features within the radio outline. The
  total width of the smooth emission in the optical jet is 0."7; the
  FWHM of the optical knots is 0."3. The knots may trace the current
  location of a narrow, perhaps helical jet lying within the outlines
  of the older radio cocoon.

---------------------------------------------------------
Title: Solar models with helium and heavy-element diffusion
Authors: Bahcall, John N.; Pinsonneault, M. H.; Wasserburg, G. J.
1995RvMP...67..781B    Altcode: 1995hep.ph....5425B
  Helium and heavy-element diffusion are both included in precise
  calculations of solar models. In addition, improvements in the input
  data for solar interior models are described for nuclear reaction rates,
  the solar luminosity, the solar age, heavy-element abundances, radiative
  opacities, helium and metal diffusion rates, and neutrino interaction
  cross sections. The effects on the neutrino fluxes of each change in
  the input physics are evaluated separately by constructing a series of
  solar models with one additional improvement added at each stage. The
  effective 1 σ uncertainties in the individual input quantities are
  estimated and used to evaluate the uncertainties in the calculated
  neutrino fluxes and the calculated event rates for solar neutrino
  experiments. The calculated neutrino event rates, including all of
  the improvements, are 9.3<SUP>+1.2</SUP><SUB>-1.4</SUB> SNU for the
  <SUP>37</SUP>Cl experiment and 137<SUP>+8</SUP><SUB>-7</SUB> SNU for
  the <SUP>71</SUP>Ga experiments. The calculated flux of <SUP>7</SUP>Be
  neutrinos is 5.1 (1.00<SUP>+0.06</SUP><SUB>-0.07</SUB>)×10<SUP>9</SUP>
  cm<SUP>-2</SUP> s<SUP>-1</SUP> and the flux of <SUP>8</SUP>B
  neutrinos is 6.6(1.00<SUP>+0.14</SUP><SUB>-0.17</SUB>)×10<SUP>6</SUP>
  cm<SUP>-2</SUP> s<SUP>-1</SUP>. The primordial helium abundance found
  for this model is Y=0.278. The present-day surface abundance of the
  model is Y<SUB>s</SUB>=0.247, in agreement with the helioseismological
  measurement of Y<SUB>s</SUB>=0.242+/-0.003 determined by Hernandez
  and Christensen-Dalsgaard (1994). The computed depth of the
  convective zone is R=0.712R<SUB>solar</SUB>, in agreement with
  the observed value determined from p-mode oscillation data of
  R=0.713+/-0.003R<SUB>solar</SUB> found by Christensen-Dalsgaard et
  al. (1991). Although the present results increase the predicted event
  rate in the four operating solar neutrino experiments by almost 1 σ
  (theoretical uncertainty), they only slightly increase the difficulty
  of explaining the existing experiments with standard physics (i.e.,
  by assuming that nothing happens to the neutrinos after they are
  created in the center of the sun). For an extreme model in which
  all diffusion (helium and heavy-element diffusion) is neglected,
  the event rates are 7.0<SUP>+0.9</SUP><SUB>-1.0</SUB> SNU for the
  <SUP>37</SUP>Cl experiment and 126<SUP>+6</SUP><SUB>-6</SUB> SNU
  for the <SUP>71</SUP>Ga experiments, while the <SUP>7</SUP>Be
  and <SUP>8</SUP>B neutrino fluxes are, respectively,
  4.5(1.00<SUP>+0.06</SUP><SUB>-0.07</SUB>)×10<SUP>9</SUP>
  cm<SUP>-2</SUP> s<SUP>-1</SUP> and
  4.9(1.00<SUP>+0.14</SUP><SUB>-0.17</SUB>)×10<SUP>6</SUP>
  cm<SUP>-2</SUP> s<SUP>-1</SUP>. For the no-diffusion model, the computed
  value of the depth of the convective zone is R=0.726R<SUB>solar</SUB>,
  which disagrees with the observed helioseismological value. The
  calculated surface abundance of helium, Y<SUB>s</SUB>=0.268, is also
  in disagreement with the p-mode measurement. The authors conclude that
  helioseismology provides strong evidence for element diffusion and
  therefore for the somewhat larger solar neutrino event rates calculated
  in this paper.

---------------------------------------------------------
Title: Hubble Space Telescope Images of Nearby Luminous
    Quasars. II. Results for Eight Quasars and Tests of the Detection
    Sensitivity
Authors: Bahcall, John N.; Kirhakos, Sofia; Schneider, Donald P.
1995ApJ...450..486B    Altcode: 1995astro.ph..1018B
  Observations with the Wide-Field Camera of the Hubble Space Telescope
  (HST) are presented for eight intrinsically luminous quasars with
  redshifts between 0.16 and 0.29. These observations, when combined
  with a similar HST study of the quasar PKS 2349-014, show that luminous
  nearby quasars exist in a variety of environments. <P />Seven companion
  galaxies brighter than M<SUB>v</SUB> = -16.5 (H<SUB>0</SUB> = 100 km
  s<SUP>-1</SUP> Mpc<SUP>-1</SUP>, Ω<SUB>0</SUB> = 1.0) lie within a
  projected distance of 25 kpc of the quasars; three of the companions
  are located closer than 3" (6 kpc projected distance) from the quasars,
  well within the volume that would be enclosed by a typical L<SUP>*</SUP>
  host galaxy. The observed association of quasars and companion galaxies
  is statistically significant and may be an important element in the
  luminous-quasar phenomenon. <P />Apparent host galaxies are detected
  for three of the quasars: PG 1116+215, 3C 273, and PG 1444+407; the
  hosts have an average absolute magnitude of about 0.6 mag brighter than
  L<SUP>*</SUP>. The agreement between the previously published major-axis
  directions in ground-based images and in the present HST images of
  3C 273 and PG 1444+407 constitutes important evidence supporting the
  reality of these candidate host galaxies. <P />Upper limits are placed
  on the visual-band brightnesses of representative galactic hosts
  for all the quasars. These limits are established by placing galaxy
  images obtained with HST underneath the quasars and measuring at what
  faintness level the known galaxies are detected. On average, the HST
  spirals would have been detected if they were as faint as 1 mag below
  L<SUP>*</SUP>, and the early-type galaxies could have been detected
  down to a brightness level of about L<SUP>*</SUP>, where L<SUP>*</SUP>
  is the Schechter characteristic luminosity of field galaxies. Smooth,
  featureless galaxy models (exponential disks or de Vaucouleurs profiles)
  are fitted to the residual light after a best-fitting point source is
  subtracted from the quasar images. The results show that smooth spiral
  galaxies brighter than, on average, about L<SUP>*</SUP>, would have been
  detected. These upper limits, or possible detections, are consistent
  with, for example, the eight luminous quasars studied in this paper,
  occurring in host galaxies that have a Shechter luminosity function
  with a lower cutoff of in the range 0.01-0.1L<SUP>*</SUP>. <P />Tests
  are performed to determine if our failure to detect, in some cases,
  luminous host galaxies could be an artifact caused by our analysis
  procedures. These tests include comparing the measured point-spread
  function (PSF) for our HST observations with the PSFs used in previous
  ground-based studies of host galaxies, measuring the fluctuations
  in the sky signals that were subtracted from the quasar images,
  evaluating empirically the effects of using different stellar PSFs in
  the analysis, carrying out the subtraction of the stellar (nuclear)
  source in different ways, creating and analyzing artificial active
  galactic nuclei (AGNs) with known surface brightnesses, and fitting
  the observed quasar light to an analytic model that includes a host
  galaxy. Our analysis procedures successfully pass all these tests.

---------------------------------------------------------
Title: Solar neutrinos and the principle of equivalence
Authors: Bahcall, J. N.; Krastev, P. I.; Leung, C. N.
1995PhRvD..52.1770B    Altcode: 1994hep.ph...10353B
  We study the proposed solution of the solar neutrino problem which
  requires a flavor nondiagonal coupling of neutrinos to gravity. We
  adopt a phenomenological point of view and investigate the consequences
  of the hypothesis that the neutrino weak interaction eigenstates
  are linear combinations of the gravitational eigenstates which
  have slightly different couplings to gravity, f<SUB>1</SUB>G and
  f<SUB>2</SUB>G, ||f<SUB>1</SUB>-f<SUB>2</SUB>||&lt;&lt;1, corresponding
  to a difference in redshift between electron and muon neutrinos,
  Δz/(1+z)~||f<SUB>1</SUB>-f<SUB>2</SUB>||. Our χ<SUP>2</SUP>
  analysis of the available solar neutrino data on observed event
  rates rules out most of the relevant parameter space, allowing
  only ||f<SUB>1</SUB>-f<SUB>2</SUB>||~3×10<SUP>-14</SUP>
  for small values of the mixing angle
  [2×10<SUP>-3</SUP>&lt;~sin<SUP>2</SUP>(2θ<SUB>G</SUB>)&lt;~10<SUP>-2</SUP>]
  and
  10<SUP>-16</SUP>&lt;~||f<SUB>1</SUB>-f<SUB>2</SUB>||&lt;~10<SUP>-15</SUP>
  for large mixing [0.6&lt;~sin<SUP>2</SUP>(2θ<SUB>G</SUB>)&lt;~0.9]. We
  show that the recoil-electron spectrum measured by the Kamiokande
  II Collaboration can be used to exclude part of the allowed regions
  obtained above. We analyze the prospects of using future spectral
  measurements of solar neutrinos to distinguish the oscillation
  mechanism due to the violation of the equivalence principle from more
  conventional mechanisms which require neutrinos to have nondegenerate
  masses. We find that, for small mixing angles, the flavor nondiagonal
  coupling to gravity leads to predictions regarding the shape of the
  <SUP>8</SUP>neutrino spectrum which will be distinguishable in the
  upcoming SNO and Super-Kamiokande experiments and which are independent
  of solar models.

---------------------------------------------------------
Title: PKS 2349-014: A Luminous Quasar with Thin Wisps, a Large
    Off-Center Nebulosity, and a Close Companion Galaxy
Authors: Bahcall, John N.; Kirhakos, Sofia; Schneider, Donald P.
1995ApJ...447L...1B    Altcode: 1995astro.ph..4076B
  Hubble Space Telescope (HST) images (WFC2) of PKS 2349-014 show that
  this luminous nearby quasar is interacting with diffuse (presumably
  galactic) material. Two thin wisps that have a total extent of about
  20 kpc (for H0 = 100 km s-1 Mpc-1 and Omega 0 = 1.0) are observed to
  approximately surround the quasar. One of the wisps appears to pass
  through a companion galaxy that is located at a projected distance
  of 3 kpc from the center of the quasar light. The companion galaxy,
  if located at the distance of PKS 2349-014, has an intrinsic size and
  luminosity similar to the Large Magellanic Cloud. A faint extended
  nebulosity, which is detected over a region of 35 kpc x 50 kpc and is
  centered about 5 kpc from the quasar nucleus, overlaps the wisps. The
  immediate environment of PKS 2349-014 is different from the environments
  of the other eight luminous quasars that we have studied previously
  with HST. If the multiple light components of the HST images are fit
  to a single de Vaucouleurs profile, as was done in previous analyses of
  ground-based data, then the result obtained for the total luminosity of
  the model galaxy is in agreement with the earlier ground-based studies.

---------------------------------------------------------
Title: Host Galaxies of Luminous Nearby Quasars
Authors: Bahcall, John
1995hst..prop.5849B    Altcode: 1995hst..prop.2322B
  The imaging of nearby quasars in oder to measure the characteristics
  of theirpresumed bright host galaxies was one of the scientific goals
  used to setperformance standards during the design and development
  of the HST. Thesurprising first results from our systematic program
  to determine host-galaxycharacteristics are not consistent with the
  standard picture, assumed in thedesign standards, that quasars occur
  in well-developed, luminous (L^* orbrighter) galaxies. No bright
  host galaxies were found for any of the 8luminous quasars we have
  studied. For this proposal, 4-orbit exploratoryexposures will be taken
  of the "cleanest" quasar for which the only candidatenebulosity detected
  in Cycle 4 was extremely faint. These observations willdetect or set
  limits on host galaxies about as faint as the LMC. For 3 otherquasars,
  the reality of possible faint nebulosity, including three candidatefaint
  host galaxies, will be tested using single-orbit observations at
  rollangles different from those used in Cycle 4; these observations
  will measurethe absolute magnitudes, the sizes, and the shapes of
  any host galaxy materialfound. The proposed observations will also
  determine the projected spacedensity of companion galaxies near (but
  physically distinct from) the quasars.

---------------------------------------------------------
Title: The Ultraviolet Emission Properties of 13 Quasars
Authors: Laor, Ari; Bahcall, John N.; Jannuzi, Buell T.; Schneider,
   Donald P.; Green, Richard F.
1995ApJS...99....1L    Altcode:
  We analyze the ultraviolet (UV) emission properties of a sample
  of 13 quasars studied with the Hubble Space Telescope (HST). The
  quasars redshifts are in the range 0.165 &lt;= z &lt;= 2.06, and
  their absolute magnitudes are in the range -30.1 &lt;= M_v_ &lt;=
  -24.4. The data were obtained with the Faint Object Spectrograph and
  have a spectral resolution of ~1300 and a signal-to-noise ratio S/N ~
  20 per resolution element. We include in the analysis optical spectra
  covering Hβ and the narrow [O III] λλ4959, 5007 doublet for 7 of
  the 13 quasars. We find that the profile of the O VI + Lyβ blend can
  be reproduced well using a "symmetric Lyα" template. The remarkable
  similarity of the Lyα and O VI profiles rules out significant line
  emission from a high-velocity and high ionization level component inner
  to the broad line region (the very broad line region, VBLR), suggested
  in a number of earlier studies of active galactic nuclei. The Hβ line
  profile is in most cases different from the Lyα and C IV profiles,
  which indicates that Hβ and the bulk of the UV lines are not produced
  by the same distribution of clouds in the broad line region (BLR). The
  following previously unobserved emission features were found in our
  spectra: (1) λ ~ 832 A, most likely OII λ 833 + O III λλ833,835
  emission.(2)λ ~ 1070 A, most likely an Fe II multiplet. (3)λ ~ 1175
  A, probably due to C III^*^. Possible implications of these features
  are briefly mentioned. The narrow [O III]-like components in both Lyα
  and C III] are generally significantly weaker than expected based on
  the observed [O III] λ5007 flux. This result is consistent with the
  1993 finding of Wills et al. and implies that the narrow line region
  (NLR) in quasars produces weaker UV /optical emission line ratios
  compared with the NLR in Seyfert 2 galaxies. A study of a combined
  sample of 18 quasars observed with HST(including Paper I) suggests
  that the equivalent widths of all lines, excluding N V, decreases
  with increasing continuum luminosity. The slopes of the EW versus
  luminosity relations for the different lines do not clearly favor
  explanations which invoke either a decrease in ionization parameter,
  or softening of the ionizing continuum, with increasing luminosity,
  as the single physical mechanism producing this effect. We verify with
  our larger sample the conclusions of Paper 1 concerning the presence
  of N III λ991, C III λ977, and Lyβ, the similarity of the C IV
  λ1549 and Lyα profiles, and the generally small velocity shifts
  of the broad line peaks relative to the peak of [O III] λ5007. In
  particular, we find a very small average shift for O VI (120 +/-
  270 km s^-1^ relative to Lyα), which does not support the suggestion
  made in earlier studies that the line peak velocity shift increases
  systematically with ionization level. The software developed for the
  line profile fitting and template deblending is available upon request.

---------------------------------------------------------
Title: Two solar neutrino problems
Authors: Bahcall, John N.
1995NuPhS..43...41B    Altcode:
  Twelve recently-published solar models give <SUP>7</SUP>Be
  neutrino fluxes that lie within a range of ±10% of the average
  value, a convergence that is independent of uncertainties in the
  measured laboratory rate of the <SUP>7</SUP>Be( p, γ) <SUP>8</SUP>B
  reaction. If nothing happens to solar neutrinos after they are created
  ( a la standard electroweak theory) and the operating solar neutrino
  experiments are correct, then the <SUP>7</SUP>Be solar neutrino flux
  must be less than 50% of the solar model value. At least three of
  the four existing solar neutrino experiments must be wrong if: (1)
  standard electroweak theory is correct, and (2) the true <SUP>7</SUP>Be
  neutrino flux lies within the range predicted by standard solar models.

---------------------------------------------------------
Title: Solar neutrinos: Radiative corrections in neutrino-electron
    scattering experiments
Authors: Bahcall, John N.; Kamionkowski, Marc; Sirlin, Alberto
1995PhRvD..51.6146B    Altcode: 1995astro.ph..2003B
  Radiative corrections to the electron recoil-energy spectra and to
  total cross sections are computed for neutrino-electron scattering
  by solid neutrinos. Radiative corrections change monotonically the
  electron recoil spectrum for incident <SUP>8</SUP>B neutrinos, with
  the relative probability of observing recoil electrons being reduced by
  about 4% at the highest electron energies. For p-p and <SUP>7</SUP>Be
  neutrinos, the recoil spectra are not affected significantly. Total
  cross sections for solar neutrino-electron scattering are reduced by
  about 2% compared to previously computed values. We also calculate
  the recoil spectra from <SUP>13</SUP>N and <SUP>15</SUP>O neutrinos
  including radiative corrections.

---------------------------------------------------------
Title: Progress and prospects in neutrino astrophysics
Authors: Bahcall, John N.; Lande, K.; Lanou, R. E.; Learned, J. G.;
   Robertson, R. G. H.; Wolfenstein, L.
1995Natur.375...29B    Altcode: 1995astro.ph..3047B
  Four separate experiments to detect neutrinos from the Sun have now
  confirmed a deficit in the flux relative to the predictions of standard
  theories of nuclear physics. Future experiments with new neutrino
  detectors promise to reveal the explanation for this shortfall. The
  planned detectors may also engender a new field of astronomy, based
  on the observation of neutrino emission from distant, energetic
  astrophysical sources.

---------------------------------------------------------
Title: The Hubble Space Telescope Quasar Absorption Line Key
    Project. V. Redshift Evolution of Lyman Limit Absorption in the
    Spectra of a Large Sample of Quasars
Authors: Stengler-Larrea, Erik A.; Boksenberg, Alec; Steidel, Charles
   C.; Sargent, W. L. W.; Bahcall, John N.; Bergeron, Jacqueline; Hartig,
   George F.; Jannuzi, Buell T.; Kirhakos, Sofia; Savage, Blair D.;
   Schneider, Donald P.; Turnshek, David A.; Weymann, Ray J.
1995ApJ...444...64S    Altcode:
  Using a sample of 119 QSOs, containing objects we have selected
  having previously available high quality ground-based and IUE spectral
  observations, together with Hubble Space Telescope (HST) observations
  of 26 QSOs from Bahcall et al. (1993, 1995) and Impey et al. (1995) and
  new optical observations of 41 objects by Steidel &amp; Sargent (1995),
  we study the redshift evolution of Lyman limit absorption systems
  (LLSs; τ &gt; 1.0) over the redshift range 0.32 &lt;= Z_LLS_ &lt;=
  4.11. The HST observations significantly improve the determination of
  the low redshift (0.4 &lt;= Z_LLS_ &lt;= 1.4) distribution. We find
  the effect which may have been responsible for the apparent strong
  evolution at Z_LLS_ =&gt; 2.5 found by Lanzetta (1991), which led him to
  consider a broken, not single, power law as a better description of the
  redshift distribution of LLSs. After removing objects which may bias
  our sample, leaving a total of 169 QSOs, we find the distribution is
  well described by a single power law, and obtain for the number density
  as a function of redshift the form N(z) = N_0_(1 + z)<SUP>gamma</SUP>^
  with γ = 1.50 +/- 0.39 and N_0_ = 0.25_+0.17_^-0.10^, consistent with
  a constant comoving density of absorbers in a Friedmann universe with
  q_0_ = 0 but indicating evolution if q_0_ = 1/2.

---------------------------------------------------------
Title: What causes a quasar?
Authors: Bahcall, J. N.
1995STSIN..12....1B    Altcode:
  Most of the pre-launch expectations that we had of what HST would reveal
  around luminous, nearby quasars have not been confirmed. Instead, the
  HST pictures show a richer variety of apparently normal galaxies, of
  complex systems of interacting material, and of undetected (presumably)
  faint host galaxies.

---------------------------------------------------------
Title: Star Counts from the HST Snapshot Survey. II. Wide Binaries
Authors: Gould, Andrew; Bahcall, John N.; Maoz, Dan; Yanny, Brian
1995ApJ...441..200G    Altcode:
  We report on a study of the first sample of wide binaries whose members
  are primarily in the old component of the Galactic disk. The binaries
  were discovered in 446 fields imaged with the Hubble Space Telescope
  (HST) Planetary Camera to an average magnitude limit of V = 2.13,
  as part of the Snapshot Survey for gravitational lenses. Most of the
  fields are at moderate to high Galactic latitude. Their total area is
  0.15 deg squared. Because of the relatively faint magnitude limit,
  the observations are sensitive primarily to binaries in the old
  disk with heights above the Galactic plane of 500-1500 pc, absolute
  magnitudes of M<SUB>v</SUB> = 6-11, and physical separations of
  130-4000 AU. By contrast, most previous surveys have been sensitive
  to binaries composed of earlier-type stars lying closer to the plane,
  that is, to a younger population. We find that 4% of the disk stars
  in the Snapshot sample have fainter companions within 1.5 mag, and
  separations in the range 0.13 sec is less than theta which is less than
  4.0 sec. The distribution of angular separations can be fitted to a
  power law F(theta) is proportional to theta<SUP>-l</SUP>, where l =
  1.2 +/- 0.4, in agreement with most previous studies. The binaries
  in the Snapshot sample have bluer colors than would be expected for
  random pairs of field stars.

---------------------------------------------------------
Title: Detection of Compact Ultraviolet Nuclear Emission in LINER
    Galaxies
Authors: Maoz, Dan; Filippenko, Alexei V.; Ho, Luis C.; Rix,
   Hans-Walter; Bahcall, John N.; Schneider, Donald P.; Macchetto,
   F. Duccio
1995ApJ...440...91M    Altcode: 1994astro.ph..8042M
  Low-ionization nuclear emission-line regions (LINERs), which exist in
  a large fraction of galaxies, may be the least luminous manifestation
  of quasar activity. As such, they may make possible the study of
  the AGN phenomenon in the nearest galaxies. The nature of LINERs
  has, however, remained controversial because an AGN-like nonstellar
  continuum source has not been directly observed in them. We report
  the detection of bright (~&gt;2 x 10^-16^ ergs s^-1^ cm^-2^ A^-1^),
  unresolved (FWHM &lt;~ 0.1") point sources of UV (2300A) emission in
  the nuclei of nine nearby galaxies. The galaxies were imaged using the
  Faint Object Camera on the Hubble Space Telescope (HST), and seven of
  them are from a complete sample of 110 nearby galaxies that was observed
  with HST. Ground-based optical spectroscopy reveals that five of the
  nuclei are LINERs, three are starburst nuclei, and one is a Seyfert
  nucleus. The observed UV flux in each of the five LINERs implies an
  ionizing flux that is sufficient to account to the observed emission
  lines through photoionization. The detection of a strong UV continuum in
  the LINERs argues against shock excitation as the source of the observed
  emission lines, and supports the idea that photoionization excites
  the lines in at least some objects of this class. We have analyzed
  ground-based spectra for most of the northern- hemisphere galaxies in
  the HST sample and find that 26 of them are LINERs, among which only
  the above five LINERs have a detected nuclear UV source. There are
  no obvious differences in the optical line intensity ratios between
  the UV-bright and UV-dark LINERs. If all LINERs are photoionized,
  then the continuum source is unobscured along our line of sight in
  5/26 ~ 20% of LINERs. Alternatively, it can be argued that spectrally
  similar LINERs are produced by various excitation mechanisms, and that
  photoionization is responsible in only ~20% of the cases. The high
  angular resolution allows us to set upper limits, typically several
  parsecs, on the physical size of the compact star cluster or AGN-type
  continuum source that is emitting the UV light in these objects.

---------------------------------------------------------
Title: Limits on electron-neutrino oscillations from the GALLEX
    <SUP>51</SUP>Cr source experiment
Authors: Bahcall, J. N.; Krastev, P. I.; Lisi, E.
1995PhLB..348..121B    Altcode: 1994hep.ph...11414B
  The recent result from the chromium source experiment carried
  out by the GALLEX collaboration implies interesting limits on the
  parameters Δm<SUP>2</SUP> and sin<SUP>2</SUP>2θ describing neutrino
  oscillations. Values of Δm<SUP>2</SUP> &gt; 0.17 eV<SUP>2</SUP> for
  maximal mixing and of sin<SUP>2</SUP>2θ &gt; 0.38 for Δm<SUP>2</SUP>
  &gt; 1 eV<SUP>2</SUP> are ruled out at 90% C.L. This result improves
  by more than an order of magnitude previous limits on Δm<SUP>2</SUP>
  derived from electron-neutrino oscillation experiments at accelerators.

---------------------------------------------------------
Title: Solar neutrinos: what we have learned.
Authors: Bahcall, J. N.
1995LNP...458...19B    Altcode: 1993astro.ph.12002B
  Four solar neutrino experiments are currently taking data. The results
  of these experiments confirm the hypothesis that the energy source for
  solar luminosity is hydrogen fusion. However, the measured rate for
  each of the four solar neutrino experiments differs significantly (by
  factors of 2.0 to 3.5) from the corresponding theoretical prediction
  that is based upon the standard solar model and the simplest version
  of the standard electroweak theory (zero-neutrino masses, no flavor
  mixing). If standard electroweak theory is correct, the energy spectrum
  for <SUP>8</SUP>B neutrinos created in the solar interior must be
  the same (to one part in 10<SUP>5</SUP>) as the known laboratory
  <SUP>8</SUP>B neutrino energy spectrum. A direct comparison of the
  chlorine and the Kamiokande experiments, both of which are sensitive
  to <SUP>8</SUP>B neutrinos, suggests that the discrepancy between
  theory and observations depends upon neutrino energy, in conflict with
  standard expectations. Monte Carlo studies with 1000 implementations of
  the standard solar model indicate that the chlorine and the Kamiokande
  experiments cannot be reconciled unless new weak interaction physics
  changes the shape of the <SUP>8</SUP>B neutrino energy spectrum. The
  boundary conditions that the solar model luminosity equals the current
  observed photon luminosity and that the solar model must be consistent
  with helioseismological measurements are two of the strongest reasons
  that the predictions of the standard solar model are robust. The
  results of the two gallium solar neutrino experiments strengthen the
  conclusion that new physics is required and help determine a relatively
  small allowed region for the MSW neutrino parameters. New experiments
  that will start in 1996 will test - independent of solar models -
  the inference that physics beyond the standard electroweak model is
  required to resolve the solar neutrino problem.

---------------------------------------------------------
Title: How Many Solar Neutrino Experiments Are Wrong?
Authors: Bahcall, John N.
1995NuPhS..38...98B    Altcode:
  Ten recently-published solar models give <SUP>7</SUP>Be neutrino fluxes
  that lie within a range of ±10% of the average value, a convergence
  that is independent of uncertainties in the measured laboratory rate of
  the <SUP>7</SUP>Be( p, γ) <SUP>8</SUP>B reaction. If nothing happens
  to solar neutrinos after they are created ( a la standard electroweak
  theory) and the operating solar neutrino experiments are correct,
  then the <SUP>7</SUP>Be solar neutrino flux must be less than 50%
  of the solar model value. At least three of the four existing solar
  neutrino experiments must be wrong if: (1) standard electroweak theory
  is correct, and (2) the true <SUP>7</SUP>Be neutrino flux lies within
  the range predicted by standard solar models.

---------------------------------------------------------
Title: Solar Modeling
Authors: Balantekin, A. B.; Bahcall, John N.
1995somo.conf.....B    Altcode: 1995QB539.S65S63...
  No abstract at ADS

---------------------------------------------------------
Title: Two Solar Neutrino Problems
Authors: Bahcall, J. N.
1995fras.conf..151B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Has a Standard Model Solution to the Solar Neutrino Problem
    been Found?
Authors: Bahcall, John N.; et al.
1995somo.conf..121B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Neutrinos: Where we are, where we are going
Authors: Bahcall, John N.
1995somo.conf....1B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: How Many Solar Neutrino Experiments Are Wrong?
Authors: Bahcall, J. N.
1995psc..conf..271B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: HST WFPC2 Study of the Density Profile and Stellar Populations
    in M15
Authors: Guhathakurta, P.; Yanny, B.; Schneider, D. P.; Bahcall, J. N.
1994AAS...18510414G    Altcode: 1994BAAS...26Q1490G
  We describe images of the center of the dense globular cluster M15
  (NGC 7078) obtained with HST's WFPC2 instrument. Data taken in
  the F336W, F439W, and F555W filters (UBV) yield a color--magnitude
  diagram of ~ 3*E(4) stars in a 5 arcmin(2) region within r&lt;2'
  (6.7pc) of the cluster center. Realistic simulated images have been
  used to estimate photometric error and incompleteness in the star
  counts. The measurement error in color is 1sigma la0 .05 mag for stars
  with V&lt;18, increasing to 1sigma ~ 0.2 mag at V=20.5, which is 1.5
  mag fainter than the main sequence turnoff. The larger number of stars
  detected with WFPC2 (compared to WF/PC-1) result in smaller Poisson
  errors in the determination of the star count profile. The projected
  radial distribution of stars (after correction for incompleteness
  and photometric bias/error) is well represented by a power law: N(r)
  ~ {r}(alpha ) , with slope alpha =-0.7+/-0.15, into radii less than
  0\farcs3 (0.015pc). Any flat core of radius larger than 1” (0.05pc)
  in the stellar distribution is ruled out at the 99% level. Only 30
  blue straggler candidates are identified from the UBV data within
  rla30 ”, and we use the simulations to correct for contamination by
  subgiant and turnoff stars. The specific frequency of blue straggler
  stars (relative to red giant branch [RGB] and subgiant stars) in the
  central region of M15 is f_BSS=0.05+/-0.02 which is significantly
  lower than in other dense clusters. The incompleteness-corrected
  radial distribution of 19&lt;V&lt;21 main sequence stars is consistent
  with that of faint RGB/subgiant stars; there is no evidence for mass
  segregation among stars in the mass interval 0.6--0.8M_sun over the
  radial range 5”--2'. As noted previously, the ratio of bright RGB
  stars (V&lt;16) to to fainter RGB and subgiant stars is lower in the
  inner 5” of the cluster compared to further out (99% significance
  level). Stars in the blue extension of the horizontal branch are
  marginally centrally depleted relative to redder horizontal branch,
  faint RGB, and subgiant stars.

---------------------------------------------------------
Title: What Have We Learned About Solar Neutrinos?
Authors: Bahcall, John
1994AAS...18510001B    Altcode: 1994BAAS...26Q1482B
  The principal lessons learned from the first 30 years of solar neutrino
  research will be summarized. The results from the four operating solar
  neutrino experiments will be reviewed and compared with theoretical
  predictions based upon standard solar models and standard electroweak
  theory (zero neutrino masses, no flavor mixing). The implications of
  p-mode helioseismological measurements for the neutrino problems will
  be discussed. New solar neutrino experiments that are currently being
  constructed will be described.

---------------------------------------------------------
Title: Host and Companion Galaxies of Luminous, Nearby Quasars
Authors: Bahcall, John
1994AAS...185.9302B    Altcode: 1994BAAS...26.1473B
  The Cycle 4 HST results for the host galaxies and companions of nearby
  luminous quasars will be reviewed.

---------------------------------------------------------
Title: Solar Neutrinos: Sensitivity to Pre--Main-Sequence Evolution
    and to the Depth of the Convective Zone
Authors: Bahcall, John N.; Glasner, Ami
1994ApJ...437..485B    Altcode: 1994astro.ph..6039B
  Predicted rates for solar neutrino experiments that are obtained with
  a modified stellar evolution code originally developed to study the
  advanced stages of stellar evolution are shown to be in agreement with
  other recently-calculated precise solar models to about 2% (0.2 SNU
  for the chlorine experiment). Different scenarios for pre-main sequence
  evolution are explored and are found to change the predicted rates for
  solar neutrino experiments by less than or of order 1%. The influence of
  the depth of the solar convective zone on the predicted solar neutrino
  fluxes is established by direct calculation. It is shown that a change
  in the calculated depth of the convective zone that is five times larger
  than the quoted helioseismological measurement uncertainty determined
  by Christensen-Dalsgaard, Gough, &amp; Thompson causes a change in
  the predicted $^8$B neutrino flux of less than 7% and a change in the
  $^7$Be neutrino flux of less than 4%. Additionally, it is shown that the
  radiative opacities near the depth of the convective zone cannot differ
  from the standard OPAL values by more than about 12% without causing
  the calculated and measured depths of the convective zone to differ
  by more than five times the helioseismological measurement uncertainty.

---------------------------------------------------------
Title: M Dwarfs, Microlensing, and the Mass Budget of the Galaxy
Authors: Bahcall, John N.; Flynn, Chris; Gould, Andrew; Kirhakos, Sofia
1994ApJ...435L..51B    Altcode: 1994astro.ph..6019B
  We show that faint red stars do not contribute significantly to the
  mass budget of the Galaxy or to microlensing statistics. Our results
  are obtained by analyzing two long exposures of a high-latitude
  field taken with the Wide Field Camera on the newly repaired {\it
  Hubble Space Telescope}. Stars are easily distinguished from galaxies
  essentially to the limiting magnitudes of the images. We find five
  stars with $2.0&lt;V-I&lt;3.0$ and $I&lt;25.3$ and no stars with
  $V-I&gt;3.0$. Therefore, main-sequence stars with $M_I&gt;10$ that
  are above the hydrogen-burning limit in the dark halo or the spheroid
  contribute $&lt;6%$ of the unseen matter. Faint red disk stars,
  M-dwarfs, contribute at most $ 15%$ to the mass of the disk. We
  parameterize the faint end of the cumulative distribution of stars,
  $\Phi$, as a function of luminosity $L_V$, $d\Phi/d \ln L_V \propto
  L_V^{-\gamma}$. For spheroid stars, $\gamma&lt;0.32$ over the range
  $6&lt;M_V&lt;17$, with 98% confidence. The disk luminosity function
  falls, $\gamma&lt;0$, for $15\lsim M_V\lsim 19$. Faint red stars in
  the disk or thick disk, and stars with $M_V&lt;16$ in the spheroid
  contribute $\tau&lt; 10^{-8}$ to the optical depth to microlensing
  toward the Large Magellanic Cloud.

---------------------------------------------------------
Title: HST Images of Nearby Luminous Quasars
Authors: Bahcall, John N.; Kirhakos, Sofia; Schneider, Donald P.
1994ApJ...435L..11B    Altcode: 1994astro.ph..9028B
  Strong upper limits are placed on the visual-band brightnesses
  of galactic hosts for four luminous, radio-quiet quasars with
  redshifts between 0.16 and 0.24 that were studied with the HST's
  Wide Field/Planetary Camera 2 (WFPC2). Typical upper limits on the
  luminosities of galactic hosts are ~1.4 mag fainter than L^*^ for
  spirals and ~0.5 mag fainter than L^*^ for ellipticals. The galactic
  hosts of the quasars are more than a magnitude and a half fainter than
  the median integrated absolute magnitude of Seyfert galaxies. If the
  detection limits are determined using featureless simulated galaxies
  instead of observed galaxy images, then the detection limits for spirals
  are 0.5-1.0 mag less stringent. These results are consistent with the
  hypothesis that the quasar phenomenon corresponds to the early stages
  of galaxy formation, before extensive star formation occurs.

---------------------------------------------------------
Title: WFPC2 Observations of the Globular Cluster M30
Authors: Yanny, Brian; Guhathakurta, Puragra; Schneider, Donald P.;
   Bahcall, John N.
1994ApJ...435L..59Y    Altcode:
  We describe images of the center of the dense globular cluster M30
  (NGC 7099) obtained with the Hubble Space Telescope Wide Field/Planetary
  Camera 2 (HST WFPC2). Data taken in the F336W, F439W, and F555W filters
  (approximately U, B, and V) yield a color-magnitude diagram with
  photometric errors of 1 sigma = 0.05 mag for stars with V less than
  17.5, and 1 sigma approximately 0.1 mag at V = 20, which is 1.5 mag
  fainter than the main-sequence turnoff. Simulations show that the star
  identifications are essentially complete for stars with V less than
  19.5, even in the densest regions of the cluster. The projected radial
  distribution of stars can be represented by a power law distribution:
  N(r) approximately r<SUP>alpha</SUP>, with slope alpha = -0.4 +/- 0.15,
  into radii less than 0.4 sec (0.015 pc). The radial profile is also
  consistent with a flat core of any radius smaller than approximately
  1.5 sec (0.05 pc), but inconsistent with any core radius larger than
  2.5 sec (0.09 pc). A total of 30 blue straggler candidates within 20
  sec of the cluster center have been identified from the three-color
  data. Their radial distribution is strongly centrally concentrated when
  compared to the horizontal branch, red giant branch, or main-sequence
  stars in the cluster. The abundance of blue stragglers (relative to
  red giants and subgiants) within r approximately less than 20 sec of
  the center of M30 is f<SUB>BS</SUB> = 0.19 =/- 0.04, about twice as
  high as in other dense clusters.

---------------------------------------------------------
Title: Globular Clusters Photometry With the Hubble Space
    Telescope. III. Blue Stragglers and Variable Stars in the Core of M3
Authors: Guhathakurta, P.; Yanny, B.; Bahcall, J. N.; Schneider, D. P.
1994AJ....108.1786G    Altcode:
  This paper describes Hubble Space Telescope (HST)/Planetary
  Camera-I images of the core of the dense globular cluster M3 (NGC
  5272). Stellar photometry in the F555W (V) and F785LP (I) bands,
  with a 1-sigma photometric accuracy of about 0.1 mag, has been used
  to construct color-magnitude diagrams of about 4700 stars above
  the main-sequence turnoff within r less than or approximately equal
  to 1 min of the cluster center. We have also analyzed archival HST
  F336W (U) images of M3 obtained by the Wide Field/Planetary Camera-I
  Instrument Definition Team. The UVI data are used to identify 28 blue
  straggler (BS) stars within the central 0.29 sq. arcmin. The specific
  frequency of BSs in this region of M3, N<SUB>BS</SUB>/N<SUB>V less
  than (V(HB</SUB>+2)) = 0.094 +/- 0.019, is about a factor of 2 -
  3 higher than that found by Bolte et al. in a recent ground-based
  study of the same region, but comparable to that seen in the sparse
  outer parts of the same cluster and in HST observations of the core
  of the higher density cluster 47 Tuc. The BSs in M3 are slightly more
  centrally concentrated than red giant branch stars while horizontal
  branch stars are somewhat less concentrated red giants. The radial
  distribution of V-selected subgiant and turnoff stars is well fit by
  a King model with a core radius r<SUB>core</SUB> = 28 arcmin +/- 2
  arcmin (90% confidence limits), which corresponds to 1.4 pc. Red giant
  and horizontal branch stars selected in the ultraviolet data (U less
  than 18) have a somewhat more compact distribution (r<SUB>core</SUB>
  = 22.5 arcmin). The HST U data consist of 17 exposures acquired over
  a span of three days. We have used these data to isolate 40 variable
  stars for which relative astrometry, brightnesses, colors, and light
  curves are presented. A Kolmogorov-Smirnov test indicates that,
  typically, the variability for each star is significant at the 95%
  level. We identify two variable BS candidates (probably of the SX Phe
  type), out of a sample of approximately 25 BSs in which variability
  could have been detected. Most of the variables are RR Lyrae stars
  on the horizontal branch. All of them have periods P greater than or
  approximately equal 8 h.

---------------------------------------------------------
Title: The Hubble Space Telescope Quasar Absorption Line Key
    Project. VI. Properties of the Metal-rich Systems
Authors: Bergeron, Jacqueline; Petitjean, Patrick; Sargent, W. L. W.;
   Bahcall, John N.; Boksenberg, Alec; Hartig, George F.; Jannuzi,
   Buell T.; Kirhakos, Sofia; Savage, Blair D.; Schneider, Donald P.;
   Turnshek, David A.; Weymann, Ray J.; Wolfe, Arthur M.
1994ApJ...436...33B    Altcode:
  We present an analysis of the properties of a sample of 18
  metal-rich, low-redshift z_abs_ &lt; z_em_ absorbers seen in low- and
  medium-resolution spectra obtained for the Quasar Absorption Line Key
  Project with the Hubble Space Telescope Faint Object Spectrograph. For
  most of the C IV and Lyman-limit systems, observations in the optical
  wavelength range of the expected associated Mg II absorption are
  available. As at high redshift (z ~ 2), there are two subclasses of
  absorbers which are characterized by the presence or absence of Mg
  II absorption. However, some low-redshift Mg II and Fe II absorptions
  originate from regions optically thin to UV ionizing photons and thus,
  at low redshift, the low- ionization systems do not always trace
  high opacities, as is the case at high redshift. This implies that
  the mean ionization state of metal-rich, optically thin absorbing
  clouds falls with decreasing redshift, which is consistent with
  the hypothesis that the gas is photoionized by the metagalactic UV
  background radiation field. Two main constraints are derived from
  the analysis of the Lyman-limit sample, assuming photoionization
  models are valid. First, a low opacity to ionizing photons (τ_LL_
  &lt;~ 1), as observed for several Mg II-Fe II systems at z ~ 0.5,
  sets limits on the ionization level of hydrogen, thus on the total
  hydrogen column density and the heavy element abundances, [Z/H] ~
  -0.5 to -0.3. Second, the dimensions of individual Mg II clouds are
  smaller than at high redshift by a factor 3-10. At z &gt;~ 0.6, the O
  VI absorption doublet is detected in four of the five z_abs_ &lt; z_em_
  systems for which the O VI wavelength range has been observed, whereas
  the associated N V doublet is detected in only two cases. This suggests
  that the presence of a high-ionization O VI phase is a general property
  of z ~ 0.6-1 absorption systems, as is also probably the case at high
  redshift. These O VI absorbers can be ionized by the UV metagalactic
  field if their density is low, n_H_ &lt;~ 3 x 10^-4^ cm^-3^. The O VI
  phase would then be a homogeneous region of large extent, r ~&gt; 50
  kpc. A detailed photoionization model of the z_abs_ = 0.791 absorber
  toward PKS 2145 + 06 confirms the properties derived from the Mg II,
  C IV, O VI, and Lyman-limit samples. The galaxy causing this extensive
  metal-line absorption system has been identified, and its possible
  contribution to the UV ionizing flux does not substantially modify
  the value of the derived parameters. The heavy element abundances are
  about half the solar values. The O VI region has a density about 20
  times lower than the Mg II clouds and a size of ~70 kpc. Alternatively,
  the high-ionization phase could be collisionally ionized and trace gas
  associated with a possible group of galaxies at the absorber redshift.

---------------------------------------------------------
Title: Two solar neutrino problems
Authors: Bahcall, John N.
1994PhLB..338..276B    Altcode: 1994PhLB..338..276N; 1994astro.ph..7048B
  It is shown that there are two solar neutrino problems:
  (1) the incompatibility of the chlorine and Kamiokande solar
  neutrino experiments; and (2) the low counting rates in the gallium
  experiments. Eleven recently-published solar models give <SUP>7</SUP>Be
  neutrino fluxes that lie within a range of +/-10% of the average
  value, a convergence that is independent of uncertainties in the
  measured laboratory rate of the <SUP>7</SUP>Be(p,γ)<SUP>8</SUP>B
  reaction. If nothing happens to solar neutrinos after they are created
  (à la standard electroweak theory) and the operating solar neutrino
  experiments are correct, then the <SUP>7</SUP>Be solar neutrino flux
  must be less than 50% of the solar model value. At least three of
  the four existing solar neutrino experiments must be wrong if. (1)
  standard electroweak theory is correct, and (2) the true <SUP>7</SUP>Be
  neutrino flux lies within the range predicted by standard solar models.

---------------------------------------------------------
Title: Has a standard model solution to the solar neutrino problem
    been found?
Authors: Bahcall, J. N.; Barnes, C. A.
1994STIN...9520490B    Altcode:
  The claim by Dar and Shaviv that they have found a standard model
  solution to the solar neutrino problem is based upon an incorrect
  assumption made in extrapolating nuclear cross sections and the
  selective use of a small fraction of the nuclear physics and of the
  neutrino data. In addition, five different solar model codes show that
  the rate obtained for the chlorine experiment using the Dar- Shaviv
  stated parameters differs by a least 14(sigma) from the observed rate.

---------------------------------------------------------
Title: The HST Quasar Absorption Line Key Project VIII. CCD Imaging
    of Hubble Space Telescope Quasar Fields
Authors: Kirhakos, Sofia; Sargent, W. L. W.; Schneider, Donald P.;
   Bahcall, John N.; Jannuzi, Buell T.; Maoz, Dan; Small, Todd A.
1994PASP..106..646K    Altcode: 1994PASP..106..646P
  We present an analysis of CCD images of more than 100 quasars; many
  of the objects have been or will be observed in the HST Key Project
  Quasar Absorption Line Survey. The data set consists of B, g, and i
  photometry of 117 quasars and deeper g (limiting magnitude of ~22)
  images of 101 quasar fields. Positions accurate to ~1", measured with
  the Space Telescope Science Institute's Astrometric Support Program,
  are listed for all of the quasars in this study. Positions, magnitudes,
  and classifications of stars and galaxies located within ~100" of the
  quasars are given for all of the dep g data. The positions of the stars
  and galaxies relative to the quasar are accurate to ~0.5". The results
  presented here can be used to prepare spectroscopic programs designed to
  obtain redshifts of galaxies in the fields of these quasars. (SECTION:
  Quasars and Active Galactic Nuclei)

---------------------------------------------------------
Title: Globular Cluster Photometry With The Hubble Space
    Telescope. II. U,V, And I Measurements of M15
Authors: Yanny, Brian; Guhathakurta, Puragra; Bahcall, John N.;
   Schneider, Donald P.
1994AJ....107.1745Y    Altcode:
  The projected density distribution of resolved stars near the center
  of M15 is shown to be consistent with either a power-law cusp N(r)
  approximately r<SUP>alpha</SUP>, with alpha approximately -0.85 +/-
  0.2, or with a King model with a core of radius approximately less than
  2 sec. The inferred slope is in agreement with the theoretical value,
  alpha = -0.75, calculated by Bahcall and Wolf for the distribution
  of equal-mass stars surrounding a massive black hole and is also
  consistent with the radial profile expected from core collapse without
  a central black hole. The object AC 214 is a candidate for the central
  density cusp. Analysis of Monte Carlo simulations of the diffuse light
  indicates that, using current analysis techniques and available data,
  the residual light is not a reliable indicator of the true density
  distribution. This is contrary to earlier work. Photometric measurements
  in V and I of more than 5 x 10<SUP>3</SUP> stars (and in U, V, and
  I of approximately greater than 1500 stars) are used to construct
  color-magnitude diagrams in the central 1 min of M15. Fourteen blue
  straggler candidates are identified in the inner 20 sec. The central
  color gradient noticed by previous researchers is caused by a central
  depletion of bright red giant stars rather than an excess of blue
  stragglers or blue horizontal branch stars.

---------------------------------------------------------
Title: Solar Neutrinos: Where We Are, Where We Are Going
Authors: Bahcall, John N.
1994astro.ph..4070B    Altcode:
  There are four important facts about solar neutrinos. They are listed
  in order of importance in this abstract and discussed more in the
  text of the talk. First, solar neutrinos have been detected in four
  experiments with approximately the energies and fluxes predicted by the
  standard solar model, confirming the hypothesis that the energy source
  for the solar luminosity is the fusion of light elements. Second,
  the measured event rates are significantl less than the event rates
  predicted by the combined standard solar and electroweak models in all
  four experiments. Third, a comparison of the event rates measured in
  the chlorine experiment (threshold 0.8 Mev) and the neutrino-electron
  scattering experiment (Kamiokande II, threshold 7.5 MeV) indicates
  that the deficiency of electron-type neutrinos at the earth is energy
  dependent, if the rates and the uncertainties in both experiments
  have been correctly understood. The inference that the deficiency
  is energy-dependent conflicts with the simplest version of standard
  electroweak theory. Fourth, experiments are being constructed that
  have the capabilities to determine conclusively if new neutrino physics
  is required.

---------------------------------------------------------
Title: Distantly detecting deuterium
Authors: Bahcall, John N.
1994Natur.368..584B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Has A Standard Model Solution to the Solar Neutrino Problem
    Been Found?
Authors: Bahcall, John N.
1994astro.ph..4002B    Altcode:
  The claim by Dar and Shaviv that they have found a standard model
  solution to the solar neutrino problem is based upon an incorrect
  assumption made in extrapolating nuclear cross sections and the
  selective use of a small fraction of the nuclear physics and of the
  neutrino data. In addition, five different solar model codes show that
  the rate obtained for the chlorine experiment using the Dar-Shaviv
  stated parameters differs by at least $14 \sigma$ from the observed
  rate.

---------------------------------------------------------
Title: <SUP>7</SUP>Be solar neutrino line: A reflection of the
    central temperature distribution of the Sun
Authors: Bahcall, John N.
1994PhRvD..49.3923B    Altcode: 1994astro.ph..1024B
  A precise test of the theory of stellar evolution can be performed by
  measuring the average difference in energy between the neutrino line
  produced by <SUP>7</SUP>Be electron capture in the solar interior
  and the corresponding neutrino line produced in a terrestrial
  laboratory. This energy shift is calculated to be 1.29 keV (to an
  accuracy of a few percent) for the dominant ground-state to ground-state
  transition. The energy shift is approximately equal to the average
  temperature of the solar core, computed by integrating the temperature
  over the solar interior with a weighting factor equal to the locally
  produced <SUP>7</SUP>Be neutrino emission. Therefore, a measurement
  of the energy shift is a measurement of the central temperature
  distribution of the Sun. The energy profile of the <SUP>7</SUP>Be line
  is derived analytically and is evaluated numerically. The line shape
  is asymmetric: on the low-energy side, the line shape is Gaussian with
  a half-width at half-maximum of 0.6 keV and, on the high-energy side,
  the line shape is exponential with a half-width at half-maximum of 1.1
  keV. The effective temperature of the high-energy exponential tail is
  15×10<SUP>6</SUP> K. The energy profile of the <SUP>7</SUP>Be neutrino
  line should be taken into account in calculations of vacuum neutrino
  oscillations and of the absorption cross section for <SUP>7</SUP>Be
  solar neutrinos incident on <SUP>7</SUP>Li nuclei. The characteristic
  modulation of the <SUP>7</SUP>Be line shape that would be caused
  by either vacuum neutrino oscillations or by matter-enhanced (MSW)
  neutrino oscillations is shown to be small. Other frequently discussed
  weak interaction solutions to the solar neutrino problem are also not
  expected to change significantly the line profile.

---------------------------------------------------------
Title: Microlensing Events: Thin Disk, Thick Disk, or Halo?
Authors: Gould, Andrew; Miralda-Escude, Jordi; Bahcall, John N.
1994ApJ...423L.105G    Altcode:
  The three recently announced candidate microlensing events toward the
  Large Magellanic Cloud (LMC) could arise from compact objects in a thin
  disk, a thick disk, or a halo. We discuss five observations that could
  among these possibilities: (1) The optical depth to the LMC, which can
  be measured from the rate and duration of events. The ratios of upper
  limits to the optical depths are 1:2.5:15 for the thin disk, thick disk,
  and halo models, so a large optical depth can rule out the thin disk
  and thick disk models, (2) The ratios of the optical depths to the SMC
  and LMC for the three models: 0.6, 0.6, and 1-1.5. (3) Deviations from
  the normal shape of the microlensing light curve, caused by parallax
  effects. The ratios of the fraction of events with detectable parallax
  effects are 70:15:1. If events are identified in real time and are
  observed with high-precision relative photometry (~0.02 mag), then
  parallax effects can be measured for most thin-disk events and ~15%
  of thick-disk events. (4) The characteristic masses inferred from
  the mean duration of events. These are in the ratio of 1.2:1:1.5,
  so this can be at most a marginal test of the three models. (5) The
  ratios of optical depths to the bulge (in excess of that produced by
  known stars) and to the LMC. These are 45, 5.5, and 1 for a thin disk,
  a thick disk, and a halo. At present the observations favor a thick-disk
  or halo origin of the lenses, or similar contributions from more than
  one structure, but do not exclude the thin disk as the main contributor.

---------------------------------------------------------
Title: Is large lepton mixing excluded\?
Authors: Smirnov, Alexei Yu.; Spergel, David N.; Bahcall, John N.
1994PhRvD..49.1389S    Altcode: 1993hep.ph....5204S
  The original ν¯<SUB>μ</SUB>- (or ν¯<SUB>τ</SUB>-) energy
  spectrum from the gravitational collapse of a star has a
  larger average energy than the spectrum for ν¯<SUB>e</SUB>
  since the opacity of ν¯<SUB>e</SUB> exceeds that of
  ν¯<SUB>μ</SUB> (or ν<SUB>τ</SUB>). Flavor neutrino conversion
  ν¯<SUB>e</SUB>⇆ν¯<SUB>μ</SUB> induced by lepton mixing
  results in partial permutation of the original ν¯<SUB>e</SUB>
  and ν¯<SUB>μ</SUB> spectra. An upper bound on the permutation
  factor p&lt;=0.35 (99% C.L.) is derived using the data from SN
  1987A and a range of models of the neutrino emission. The relation
  between the permutation factor and the vacuum mixing angle is
  established, which leads to the upper bound on this angle. The upper
  bound sin<SUP>2</SUP>2θ&gt;0.7-0.9 excludes the large mixing angle
  solutions of the solar neutrino problem: “just-so” and, partly, MSW,
  as well as part of the region of the ν<SUB>e</SUB>-ν<SUB>μ</SUB>
  oscillation space which could be responsible for the atmospheric muon
  neutrino deficit. These limits are sensitive to the predicted neutrino
  spectrum and can be strengthened as supernova models improve.

---------------------------------------------------------
Title: VizieR Online Data Catalog: Positions of high-redshift luminous
    quasars (Schneider+ 1992)
Authors: Schneider, D. P.; Bahcall, J. N.; Saxe, D. H.; Bahcall,
   N. A.; Doxsey, R.; Golombek, D.; Krist, J.; McMaster, M.; Meakes,
   M.; Lahav, O.
1994yCat.7149....0S    Altcode:
  The non-proprietary HST Snapshot Survey produced Planetary Camera
  images of high-redshift, luminous quasars. The aim of the program is to
  determine the frequency of multiple imaged QSOs down to angular scales
  of 0.15". Detailed descriptions of the program are given in Bachall et
  al. (1992ApJ...387...56B) and Maoz et al. (1992ApJ...394...51M). The
  sample was taken from the 3rd and 4th editions of the catalog of
  Veron-Cetty and Veron (1987ESOSR...5....1V, 1989ESOSR...7....1V). The
  target positions taken from these catalogs were fed to GASP, the
  STSci Guide Star Astrometric Support Program, to generate revised
  positions from regions extracted from the STSci's digitized sky
  survey. The printed version of the catalog does not contain the Veron
  1950 coordinates nor the difference between these and the GASP derived
  1950 coordinates that are contained in this version. <P />(1 data file).

---------------------------------------------------------
Title: Element Diffusion in the Solar Interior
Authors: Thoul, Anne A.; Bahcall, John N.; Loeb, Abraham
1994ApJ...421..828T    Altcode: 1993astro.ph..4005T
  We study the diffusion of helium and other heavy elements in the solar
  interior by solving exactly the set of flow equations developed by
  Burgers for a multi-component fluid, including the residual heat-flow
  terms. No approximation is made concerning the relative concentrations
  and no restriction is placed on the number of elements considered. We
  give improved diffusion velocities for hydrogen, helium, oxygen
  and iron, in the analytic form derived previously by Bahcall and
  Loeb. These expressions for the diffusion velocities are simple to
  program in stellar evolution codes and are expected to be accurate
  to $\sim 15\%$. Our complete treatment of element diffusion can be
  directly incorporated in a standard stellar evolution code by means
  of an exportable subroutine, but, for convenience, we also give simple
  analytical fits to our numerical results.

---------------------------------------------------------
Title: Electron Capture and Nuclear Matrix Elements of Be<SUP>7</SUP>
Authors: Bahcall, J. N.
1994snft.book..198B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Termination of the Proton-Proton Chain in Stellar Interiors
Authors: Parker, P. D.; Bahcall, J. N.; Fowler, W. A.
1994snft.book..212P    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Standard Solar Models, With and Without Helium Diffusion,
    and the Solar Neutrino Problem
Authors: Bahcall, J. N.; Pinsonneault, M. H.
1994snft.book...60B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Rate of the Proton-Proton Reaction
Authors: Kamionkowski, Marc; Bahcall, John N.
1994ApJ...420..884K    Altcode: 1993astro.ph..5020K
  We re-evaluate the matrix element for the proton-proton reaction
  which is important for stellar-evolution calculations and for the
  solar-neutrino problem. We self-consistently determine the effect
  of vacuum polarization on the matrix element by first correcting the
  low-energy scattering data to account for vacuum polarization. We then
  calculate the proton-proton wave function by integrating the Schrodinger
  equation with vacuum polarization included. We use improved data
  for proton-proton scattering and for the deuteron wave function. We
  evaluate the uncertainties that are due to experimental error and
  estimate those that are due to theoretical inadequacies. We estimate the
  theoretical uncertainty by using six different deuteron potentials and
  five different proton-proton potentials. Vacuum polarization decreases
  the calculated value by $0.6_{-0.4}^{+0.1}$\%. The complete result is
  $\Lambda^2=6.92\times(1\pm0.002^{+0.014}_{-0.009})$ where the first
  uncertainty is due to experimental errors and the second uncertainty
  is due to theoretical uncertainties. Our value of $\Lambda^2$ is 2\%
  smaller than the value obtained in 1969 by Bahcall and May. The improved
  calculations of the rate of the $pp$ reaction described here increase
  slightly the predicted event rates for the chlorine and the Kamiokande
  solar-neutrino experiments.

---------------------------------------------------------
Title: Vacuum-polarization corrections to solar-fusion rates
Authors: Kamionkowski, Marc; Bahcall, John N.
1994PhRvC..49..545K    Altcode: 1993astro.ph..6024K
  The vacuum-polarization (VP) corrections to rates for nuclear-fusion
  reactions in the pp chain and in the CNO cycle are calculated. For
  the reactions of particular importance to the solar-neutrino
  problem, the <SUP>3</SUP>He(<SUP>3</SUP>He,2p)<SUP>4</SUP>He,
  <SUP>3</SUP>He(α,γ)<SUP>7</SUP>Be, <SUP>7</SUP>Be(p,γ)<SUP>8</SUP>B,
  and <SUP>14</SUP>N(p,γ)<SUP>15</SUP>O reactions, we find the magnitude
  of the effect to be less than 2%. The effect of VP on all the other
  reaction rates is expected to be of a similar order of magnitude. We
  discuss how these results affect the predicted fluxes of solar
  neutrinos.

---------------------------------------------------------
Title: The Stellar Density Distributions in the Centers of Galactic
Globular Clusters: Cycle 4 Observations
Authors: Bahcall, John
1994hst..prop.5603B    Altcode: 1994hst..prop.2044B
  A single exposure in the F336W filter will be made of M30 using the
  PC CCD of the WFPC2.

---------------------------------------------------------
Title: The <SUP>7</SUP>Be Electron-Capture Rate
Authors: Bahcall, J. N.; Moeller, C. P.
1994snft.book..222B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Standard Solar Models and the Uncertainties in Predicted
    Capture Rates of Solar Neutrinos
Authors: Bahcall, J. N.; Huebner, W. F.; Lubow, S. H.; Parker, P. D.;
   Ulrich, R. K.
1994snft.book...57B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Are Neutrinos Stable Particles?
Authors: Bahcall, J. N.; Cabibbo, N.; Yahil, A.
1994snft.book..285B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Neutrinos. I. Theoretical
Authors: Bahcall, J. N.
1994snft.book....9B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Neutrino Flux
Authors: Bahcall, J. N.; Fowler, W. A.; Iben, I., Jr.; Sears, R. L.
1994snft.book...30B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Rate of the Proton-Proton Reaction
Authors: Bahcall, J. N.; May, R. M.
1994snft.book..218B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Stellar Density Distributions in the Centers of Galactic
    Globular Clusters
Authors: Bahcall, John
1994hst..prop.5687B    Altcode: 1994hst..prop.2128B
  Short exposures will be made of all galactic globular clusters
  with distance moduli less than 15.5 mag and galactic latitude
  above or below 15 degrees. A search will be made for cusps
  in the stellar density distributions and the colors will be
  measured for the brightest stars in the cores of the clusters. ST
  observations are required in order to reach the innermost regions
  of the clusters with sufficient resolution to separate individual
  stars. ********************************************************** This
  program contains only the exposures that were not completed prior to
  the first HST servicing mission.

---------------------------------------------------------
Title: Do Solar-Neutrino Experiments Imply New Physics?
Authors: Bahcall, J. N.; Bethe, H. A.
1994snft.book...65B    Altcode: 1993astro.ph..7013B
  Physics beyond the simplest version of the standard electroweak
  model is required to reconcile the results of the chlorine and the
  Kamiokande solar neutrino experiments. None of the 1000 solar models
  in a full Monte Carlo simulation is consistent with the results of
  the chlorine or the Kamiokande experiments. Even if the solar models
  are forced articficially to have a ${}^8 B$ neutrino flux in agreement
  with the Kamiokande experiment, none of the fudged models agrees with
  the chlorine observations. This comparison shows that consistency of
  the chlorine and Kamiokande experiments requires some physical process
  that changes the shape of the ${}^8 B$ neutrino energy spectrum. The
  GALLEX and SAGE experiments, which currently have large statistical
  uncertainties, differ from the predictions of the standard solar model
  by $2 \sigma$ and $3 \sigma$, respectively. The possibility that the
  neutrino experiments are incorrect is briefly discussed.

---------------------------------------------------------
Title: Solar Neutrino Experiments
Authors: Bahcall, J. N.
1994snft.book...29B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Neutrino-Spectroscopy of the Solar Interior
Authors: Bahcall, J. N.
1994snft.book..113B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Present Status of the Theoretical Predictions for the
    <SUP>37</SUP>Cl Solar-Neutrino Experiment
Authors: Bahcall, J. N.; Bahcall, N. A.; Shaviv, G.
1994snft.book...45B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Imaging and Spectroscopy of a Complete Sample of Bright Nearby
Quasars: I. Imaging
Authors: Bahcall, John
1994hst..prop.5099B    Altcode: 1994hst..prop.1611B
  A sample of 7 Palomar Green quasars will be imaged with the WFC. The
  morphology of the host galaxies is not discernible - in the presence of
  a bright center source (quasar) - with ground based observations, but
  will be determined with ST unless the galaxies are unexpectedly faint.

---------------------------------------------------------
Title: Lepton Non-Conservation and Solar Neutrinos
Authors: Bahcall, J. N.; Frautschi, S. C.
1994snft.book..277B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Neutrinos
Authors: Bahcall, J. N.
1994snft.book...23B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Proposed Solar-Neutrino Experiment Using <SUP>71</SUP>Ga
Authors: Bahcall, J. N.; Cleveland, B. T.; Davis, R., Jr.; Dostrovsky,
   I.; Evans, J. C., Jr.; Frati, W.; Friedlander, G.; Lande, K.; Rowley,
   J. K.; Stoenner, R. W.; Weneser, J.
1994snft.book..116B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Sensitivity of the Solar-Neutrino Fluxes
Authors: Bahcall, J. N.; Bahcall, N. A.; Ulrich, R. K.
1994snft.book...54B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Predictions for a Liquid Argon Solar Neutrino Detector
Authors: Bahcall, J. N.; Baldo-Ceolin, M.; Cline, D. B.; Rubbia, C.
1994snft.book..123B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On the Problem of Detecting Solar Neutrinos
Authors: Bahcall, J. N.; Davis, R., Jr.
1994snft.book...42B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Neutrinos: A Scientific Puzzle
Authors: Bahcall, J. N.; Davis, R., Jr.
1994snft.book..141B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: WFC Imaging of Nearby Bright Quasars
Authors: Bahcall, John
1994hst..prop.5343B    Altcode: 1994hst..prop.1789B
  We will obtain deep WFPC2 images of bright, nearby quasars to
  investigate the optical morphology of their host galaxies. The high
  angular resolution of HST will allow one to perform a number of
  quantitative measurements of the morphology and luminosities of host
  galaxies. The proposed HST observations will reveal the relationship
  between the properties of the host galaxy and quasar luminosity (both
  optical and radio), and how quasar host galaxies differ from field or
  cluster galaxies. The sample consists of 13 quasars with z &lt; 0.3,
  M_V &lt; -23 (Ho = 100), and |b| &gt; 35. Each quasar will be imaged in
  a Wide Field Camera CCD through the F606W filter. The objects in this
  proposal span a range of quasar luminosities (up to M_V of -24.5; Ho =
  100) and redshifts (0.09 &lt; z &lt; 0.265). Three of the 13 quasars
  are radio-loud; the combined GTO/GO sample of 22 objects contains six
  radio-loud quasars.

---------------------------------------------------------
Title: Quasar Absorption Line Survey - Cycle 4 High
Authors: Bahcall, John
1994hst..prop.5664B    Altcode: 1994hst..prop.2105B
  The Absorption Line Survey of bright quasars provides a homogeneous
  data base for studying fundamental questions about the origin and
  evolution of gaseous systems in the universe. The initial results
  determine at small redshifts the number densities of Ly-ALPHA systems,
  of metal-lines and extragalactic halos, of Lyman-limit systems,
  of associated absorption systems, and the shapes and intensities of
  quasar emission lines and spectral energy distributions. The survey
  reveals that much of the sky is covered by high or very high velocity
  metal-line clouds present in the Galactic halo. A larger sample, which
  includes the requested Cycle 3 observations, is required to answer many
  important questions. For example, what is the correlation function
  of Ly-ALPHA systems at small redshifts? What fraction of the metal,
  the Ly-ALPHA, and the Ly-limit systems are associated with galaxies
  and what are the characteristic sizes of the outer gaseous regions of
  different types of galaxies? Do absorbing systems show evidence of the
  large-scale structure seen with galaxies and clusters of galaxies? The
  observations requested in Cycle 3 will extend the region of coverage
  of the Key Project sample from the redshift range of z = 0.0 to 1.0
  (Cycles 1&amp; 2) to z = 0.0 to 1.6 (Cycles 1-3). THIS FILE CONTAINS
  THE HIGH PRIORITY OBSERVATIONS FROM CYCLES 2 and 3 WHICH WERE NOT
  COMPLETED IN THOSE CYCLES.

---------------------------------------------------------
Title: Standard Model Expectations: Introduction
Authors: Bahcall, John N.
1994snft.book....3B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Neutrino Opacity. I. Neutrino-Lepton Scattering
Authors: Bahcall, J. N.
1994snft.book...18B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Models, Neutrino Experiments, and Helioseismology
Authors: Bahcall, J. N.; Ulrich, R. K.
1994snft.book...58B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar neutrinos. The first thirty years.
Authors: Bahcall, J. N.; Davis, R., Jr.; Parker, P.; Smirnov, A.;
   Ulrich, R.
1994snft.book.....B    Altcode: 1994FrPhy..92.....B; 1994QB539.S65S64...
  The editors have selected a representative collection of papers that
  they believe to be important in the development of solar neutrino
  research. They chose to begin their selection of papers in the year
  1964 when it first became apparent that a practical experiment to
  detect solar neutrinos was possible.

---------------------------------------------------------
Title: The Ultraviolet Emission Properties of Five Low-Redshift Active
    Galactic Nuclei at High Signal-to-Noise Ratio and Spectral Resolution
Authors: Laor, Ari; Bahcall, John N.; Jannuzi, Buell T.; Schneider,
   Donald P.; Green, Richard F.; Hartig, George F.
1994ApJ...420..110L    Altcode: 1993astro.ph..5026L
  We analyze the ultraviolet (UV) emission line and continuum properties
  of five low-redshift active galactic nuclei (four luminous quasars:
  PKS 0405 - 123, H1821 +643, PG 0953+414, and 3C 273, and one bright
  Seyfert 1 galaxy: Mrk 205). The HST spectra have higher signal-to-noise
  ratios (typically ~60 per resolution element) and spectral resolution
  (A = 1300) than all previously published UV spectra used to study
  the emission characteristics of active galactic nuclei. We include in
  the analysis ground-based optical spectra covering Hβ and the narrow
  [O III] λλ4959,5007 doublet. The following new results are obtained:
  Lyβ/Lyα = 0.03-0.12 for the four quasars, which is the first accurate
  measurement of the long-predicted Lyβ intensity in QSOs. The cores of
  Lyα and C IV are symmetric to an accuracy of better than 2.5% within
  about 2000 km s^-1^ of the line peak. This high degree of symmetry
  of Lyα argues against models in which the broad line cloud velocity
  field has a significant radial component. The observed smoothness of the
  Lyα and C IV line profiles requires at least ~10^4^ individual clouds
  if bulk velocity is the only line-broadening mechanism. The overall
  similarity of the Lyα and C IV λ1549 profiles rules out models for the
  broad-line region (BLR) with a radial distribution of virialized clouds
  having an ionization parameter U is proportional to Radius^-1^. The
  measured high values of O VI λ1034/Lyα and low values of C III λ977/O
  VI λ1034 imply a BLR component with U ~ 1. The red-wing flux in O
  VI relative to Lyα suggests the presence of an inner, high-velocity,
  optically thin component with U &gt; 1 in the BLR. The N V/Lyα ratio
  is 0.135 +/- 0.01 for the four quasars, which may be an indication of
  higher than solar N abundance and metallicity. The maximum contribution
  of a narrow ([O III]-like) component is about 3%-6% of the total
  broad-line flux; this limit is generally highest for C III]. This
  result constrains the covering factor of the narrow line region or
  indicates the presence of dust. An unresolved component having full
  width at half-maximum less than 230 km s^-1^ typically contributes
  less than 0.5% of the observed broad lines flux. The HST data permit
  the first relatively accurate measurements of the Lyγ, C III λ977,
  S VI λλ933, 945, and the N III λ991 emission lines, as well as the
  measurement of a number of other weak or strongly blended lines at λ
  &gt; 1216 A. In agreement with observations of high-redshift quasars,
  the peaks of Lyα, C IV, and C III] are blueshifted by ~200 km s^-1^
  relative to [O III] λ5007, while He II λ1640 is shifted by about
  500 km s^-1^. The low ionization lines, Mg II, Hβ, and O I λ1304,
  are in most cases only marginally shifted to the red.

---------------------------------------------------------
Title: The centers of two very dense Globular Clusters
Authors: Yanny, Brian; Guhathakurta, Puragra; Schneider, Donald P.;
   Bahcall, John
1993AAS...183.2402Y    Altcode: 1993BAAS...25.1329Y
  We present Hubble Space Telescope Planetary Camera imaging observations
  of the centers of very dense globular clusters. We discuss the radial
  profile of stars in the central 2 arcsec of these clusters and compare
  with predictions of theories of post core collapse cluster profiles. We
  discuss the appearance of various negative power law stellar density
  slopes in the center of a cluster under typical observing conditions
  and compare with the HST observations. We find we cannot rule out
  a cusp of slope -0.8 in projected stellar density as a function of
  radius in the center of the cluster M15 (NGC 7078).

---------------------------------------------------------
Title: A Very Large Array Search for Emission From HI Associated
    With Nearby Lyman alpha Absorption
Authors: van Gorkom, J. H.; Bahcall, J. N.; Jannuzi, B. T.; Schneider,
   D. P.
1993AJ....106.2213V    Altcode: 1993ApJS...89.2213V
  We present a sensitive VLA search for H I emission from the vicinity of
  the Lyman α clouds in the Virgo Cluster, which were recently discovered
  with HST in absorption toward the nearest quasar 3C 273. We searched
  an area of 40 by 40 arcmin centered on 3C 273, covering a velocity
  range from 840 to 1840 km s^-1^. The bandpass was self- calibrated
  on 3C 273 leading to a spectral dynamic range of better than 10^5^ to
  1. No H I was detected. The rms noise in the final images corresponds
  to a 3σ column density sensitivity of 2.8 x 10^19^ cm^- 2^ on scales
  of a few kpc. Small H I clouds could have been detected down to a
  few times 10^6^ M_sun_. Our failure to detect H I in emission at the
  higher column densities sets a lower limit to the radius of the Lyman
  α clouds of 3.9 kpc, assuming a spherical geometry.

---------------------------------------------------------
Title: The Effects of Helium Diffusion on Solar p-Mode Frequencies
Authors: Guenther, D. B.; Pinsonneault, M. H.; Bahcall, J. N.
1993ApJ...418..469G    Altcode:
  Precise solar models are computed with and without including helium
  diffusion. We show that the inclusion of helium diffusion according
  to the Bahcall-Loeb prescription causes systematic shifts of order
  1-5 μHz in the predicted p-mode oscillation frequencies. Calculations
  with the diffusion coefficients multiplied and divided by two show that
  the inferred effects are linearly proportional to the magnitude of the
  diffusion. Relative to a model that does not include helium diffusion,
  the models with diffusion increase the frequencies of low-l modes and
  decrease the frequencies of high-l modes. The effect on the frequencies
  of intermediate-l modes depends on whether or not the modes penetrate
  significantly below the convection zone. Future observations may reveal
  this characteristic signature of diffusion. Unfortunately, systematic
  discrepancies of order 10 μHz out of 3000 μHz prevent, at present,
  a direct test of the signature of helium diffusion. Improvements in
  the treatment of nonadiabatic effects and in the opacity and equation
  of state may remove the largest discrepancies and permit measurements
  that are specifically sensitive to helium diffusion.

---------------------------------------------------------
Title: Central temperature of the Sun can be measured via the
    <SUP>7</SUP>Be solar neutrino line
Authors: Bahcall, John N.
1993PhRvL..71.2369B    Altcode: 1993hep.ph....9292B
  A precise test of the theory of stellar evolution can be performed
  by measuring the difference in average energy between the neutrino
  line produced by <SUP>7</SUP>Be electron capture in the solar
  interior and the corresponding neutron line produced in a terrestrial
  laboratory. The high temperatures in the center of the Sun broaden the
  line asymmetrically, FWHM =1.6 keV, and cause an average energy shift
  of 1.3 keV. The width of the <SUP>7</SUP>Be neutrino line should be
  taken into account in calculations of vacuum neutrino oscillations.

---------------------------------------------------------
Title: Star Counts from the Hubble Space Telescope Snapshot
    Survey. I. Galactic Models
Authors: Gould, A.; Bahcall, J. N.; Maoz, D.
1993ApJS...88...53G    Altcode:
  We report on a photometric study of stars from 450 fields at high
  Galactic latitudes that were observed in the Hubble Space Telescope
  Snapshot Survey to an average limiting apparent magnitude of V =
  21.4. There are 166 fields that contain quasars selected in radio,
  X-ray, and color-excess surveys. This sample of 273 stars is free of
  selection bias with respect to the density of stars. To within the
  Poisson errors, the total counts and magnitude distribution of this
  unbiased sample are in agreement with the Bahcall-Soneira model. The
  angular distribution of the faint stars favors, at the 2 σ level,
  a somewhat steeper disk luminosity function and a smaller spheroid
  main-sequence normalization than given by the model. The sample does not
  have enough statistical power to distinguish between the two-component
  Bahcall-Soneira model and the three-component model first proposed
  by Gilmore &amp; Reid, which contains a thick disk. The statistical
  power of the survey would increase ~15 fold if colors were obtained
  for the stars: the data probe the main sequences of the disk, thick
  disk, and spheroid and these three components are well separated in
  color. Models with and without a thick disk could then be distinguished
  at the 6 sigma level. The HST Snapshot Survey includes an additional
  284 fields, 279 of which are centered on quasars that were selected by
  objective-prism surveys. These 279 fields are expected to show and do
  exhibit bias against bright stars, making them unsuitable for testing
  Galactic models. There is a zone of avoidance surrounding quasars
  identified by objective-prism techniques which should be taken into
  account when determining the distribution properties of these quasars.

---------------------------------------------------------
Title: The Hubble Space Telescope Quasar Absorption Line Key
    Project. III. First Observational Results on Milky Way Gas
Authors: Savage, Blair D.; Lu, Limin; Bahcall, John N.; Bergeron,
   Jacqueline; Boksenberg, Alec; Hartig, George F.; Jannuzi, Buell T.;
   Kirhakos, Sofia; Lockman, Felix J.; Sargent, W. L. W.; Schneider,
   Donald P.; Turnshek, David; Weymann, Ray J.; Wolfe, Arthur M.
1993ApJ...413..116S    Altcode:
  We report on absorption by Milky Way disk and halo gas seen in Quasar
  Absorption Line Key Project measurements of 15 quasars obtained with
  the Faint Object spectrograph (FOS) of the Hubble Space Telescope
  (HST). The measurements extend from 1150 to 3270 A for four objects
  and from 1600 to 3270 A for 11 objects and have a velocity resolution
  (FWHM) of 220-240 km s^-1^ and signal-to-noise ratio of typically 25
  per resolution element. The data processing techniques are presented in
  Key Project Papers I and II. Milky Way absorption lines comprise 44%
  of all absorption lines found in the first group of 13 Key Project
  spectra. The Milky Way lines observed in the highest quality data
  for 3C 273 and H 1821+643 include lines from H I, C II, C II^*^,
  C IV, O I, N I, Mg I, Mg II, Al II, Al III, Si II, Si III, Si IV,
  S II, Mn II, Fe II, and Zn II. Strong singly ionized metal lines of
  Fe II λλ2600.17 and 2586.65 and Mg II λλ2796.35 and 2803.53 are
  detected in all the spectra. High-quality H I 21 cm emission spectra
  are used to make small adjustments to the FOS wavelength scale to
  bring the UV data onto an LSR velocity system. The strong metal lines
  of Fe II and Mg II permit a sensitive search for metal-line analogs
  to the high-velocity clouds seen in H I 21 cm emission. Toward three
  quasars we detect resolved, very high negative velocity (v &lt; -
  250 km s^-1^) metal-line absorption. Toward four quasars we detect
  blended high negative velocity absorption (-250 km s^-1^ &lt; v &lt;
  - 100 km s^-1^). Therefore, seven of 15 sight lines observed in this
  limited sample exhibit high-velocity or very high velocity metal-line
  absorption. Lower limits to the Mg-to-H abundance ratio of 0.059,0.12,
  and 0.32 times the solar abundance are obtained for the three detections
  of very high velocity Mg II absorption toward PKS 2251 + 11, PG
  0043 + 039, and 3C 454.3, respectively. However, cloud clumping may
  influence this result, since the H I reference column density from 21
  cm emission measurements is obtained with a 21' beam. The sight-line
  to PG 1259 + 593 reveals absorptions in the lines of Mg II, Fe II,
  C II, and Si II which are in part due to high-velocity cloud Complex
  C III. Two sight lines (H1821 + 643 and 3C 351) which extend through
  the warped outer Galaxy exhibit strong absorption by singly ionized
  metals (C II, Si II, Fe II, Mg II) and highly ionized gas (C IV) at
  velocities corresponding to absorption in the outer Galaxy. Combining
  our measurements of C IV with data from the literature, we derive
  a Galactic C IV exponential scale height of 4.9 kpc and a midplane
  density of 7.1 x 10^-9^ atoms cm^-3^. However, the C IV distribution is
  so patchy that the measurements are found to be equally well fitted by
  a spherical halo model with a Galactocentric exponential scale length
  of 6.9 kpc. A comparison of absorption in high-redshift damped Lyα
  systems with the absorption produced by the Milky Way shows that an
  appreciable fraction of the damped Lyα absorption-line systems have
  mixed ionization absorption-line characteristics roughly similar to that
  found for six sight lines through the Milky Way disk and halo. Since
  the low-ionization lines are highly saturated, this similarity does
  not imply similar abundances in the neutral and weakly ionized gas but
  instead probably suggests a similarity in the kinematical behavior of
  the different absorbing media.

---------------------------------------------------------
Title: Hydrogen and Metal Absorption Lines in PKS 0405-123 From the
    Halos of Low Redshift Galaxies
Authors: Spinrad, Hyron; Filippenko, Alexei V.; Yee, H. K.; Ellingson,
   Erica; Blades, J. C.; Bahcall, John N.; Jannuzi, Buell T.; Bechtold,
   Jill; Dobrzycki, Adam
1993AJ....106....1S    Altcode:
  Hubble Space Telescope ultraviolet spectra and ground-based optical
  spectra of the bright quasar PKS 0405 - 123 are used to identify two
  absorption-line systems probably produced by the halos of foreground
  galaxies. The quasar lies in a rich galaxy field. Loose groups
  of galaxies are present in the field at &lt;z_1_&gt; = 0.1669 and
  &lt;z_2_&gt; = 0.3519. Ly α, C IV λ1549, and probably Mg II λ2798
  resonance lines are detected in an absorption system at z = 0.1670. An
  absorption system consisting of only Ly α is observed at z = 0.3516. We
  cannot be completely certain which foreground galaxy is responsible
  for the metal line absorption system at z_1_. A likely candidate is
  a large, luminous, early-type spiral 40" (projected distance 78h^-1^
  kpc) to the east of the quasar. However, the origin of the z_1_ system
  could possibly be a small, undetected galaxy more precisely aligned
  along our line of sight to PKS 0405 - 123, or a very faint galaxy
  whose redshift has not yet been measured.

---------------------------------------------------------
Title: The Hubble Space Telescope Quasar Absorption Line Key
    Project. II. Data Calibration and Absorption-Line Selection
Authors: Schneider, Donald P.; Hartig, George F.; Jannuzi, Buell T.;
   Kirhakos, Sofia; Saxe, David H.; Weymann, Ray J.; Bahcall, John N.;
   Bergeron, Jacqueline; Boksenberg, Alec; Sargent, W. L. W.; Savage,
   Blair D.; Turnshek, David A.; Wolfe, Arthur M.
1993ApJS...87...45S    Altcode:
  We present the observational and data processing aspects of the Hubble
  Space Telescope Quasar Absorption Line Key Project. Topics discussed
  include the observational technique, calibration of the data, software
  that simulates the data, the automated procedure used to identify and
  characterize the absorption features, and the determination of the
  sensitivity limits of the survey.

---------------------------------------------------------
Title: The Hubble Space Telescope Quasar Absorption Line Key
    Project. I. First Observational Results, Including Lyman-Alpha and
    Lyman-Limit Systems
Authors: Bahcall, John N.; Bergeron, Jacqueline; Boksenberg, Alec;
   Hartig, George F.; Jannuzi, Buell T.; Kirhakos, Sofia; Sargent,
   W. L. W.; Savage, Blair D.; Schneider, Donald P.; Turnshek, David A.;
   Weymann, Ray J.; Wolfe, Arthur M.
1993ApJS...87....1B    Altcode:
  We present spectra for a total of 37 quasars with small and
  moderate redshifts; the quasars were observed with the Faint Object
  Spectrograph of the Hubble Space Telescope. The spectra are obtained
  either at a resolution of R = 1300 (hereafter "higher resolution")
  or a resolution of r = 180 (hereafter "lower resolution"). We report
  new higher resolution measurements of the absorption lines in the
  ultraviolet spectra of 11 quasars with emission-line redshifts that
  lie between 0.3 and 1.0. Improved reductions are provided for higher
  resolution observations of two additional small-redshift quasars
  observed as part of the Guaranteed Time observational program. These
  observations cover all or part of the wavelength range 1180-3270 A in
  the observed frame. In addition, we present lower dispersion spectra
  (R = 180, wavelength range 1150-2430 A) obtained for 24 objects with
  redshifts between 0.5 and 1.4. Calibrated spectra and continuum fits
  are shown for each object. A well-defined sample of absorption lines
  was constructed algorithmically from all of the higher resolution data;
  the detection limit is expressed in terms of a limiting equivalent width
  as a function of wavelength. A total of 358 lines are selected by the
  software in the higher resolution spectra. Time-dependent flat-field
  features represent the most serious and difficult-to-quantify source
  of systematic errors. The identifications of interstellar and of
  extragalactic lines were made in the higher resolution spectra with
  the aid of software that utilizes the detection limit as a function of
  wavelength and the known atomic properties of cosmologically abundant
  ions. A total of 104 extragalactic Lyα systems are identified, of
  which nine are found at the same redshifts as metal-line systems. The
  absorption lines that are not identified Galactic interstellar features
  or extragalactic metal lines are not uniformly distributed; their
  line density is more than 10 times larger within (rather than outside)
  the region accessible to extragalactic hydrogen absorption, providing
  statistical support for the identifications of Lyα systems. The local
  number density of Lyα systems with rest equivalent widths larger
  than 0.32 A and without detected metal lines is (dN/dz)_0_~15.1 +/- 2
  Lyα systems per unit redshift, if the local Lyα systems are members
  of the same population as the previously observed large-redshift
  Lyα lines (i.e., the evolutionary parameter is fixed at γ = 0.75,
  and the assumed exponential distribution of equivalent widths is
  characterized by W^*^ = 0.32 A). If γ and W^*^ are allowed to vary,
  then (dN/dz)_0_~ 17.7 +/- 4.3 Lyα systems per unit redshift with γ =
  0.30 +/- 0.62 and W^*^ = 0.22 +/- 0.02 A. The two-point correlation
  function of the velocity splittings does not show statistically
  significant evidence of clumping. A sample at least 3 times larger
  than the one analyzed in this paper would be required to test the
  hypothesis that Lyα absorption systems observed at small redshifts
  are clustered like galaxies. The spectra of 29 quasars have been
  searched algorithmically for the existence of Lyman-limit systems. A
  total of 10 Lyman-limit systems with an optical depth greater than
  0.4 were identified. The number density of such systems at redshifts
  between 0.4 and 1.4 in our sample is (dN/dz)_LLS_ = 0.8(1+z)^0.5^ for
  a nonevolving population in a q_0_ = 0.5 universe and (dN/dz)_LLS_
  = 0.3(1 + z)^2.4^ if they evolve as rapidly as Lyα clouds observed
  at large redshifts. A search for damped Lyα lines revealed only one
  candidate line, in the spectrum of PKS 2251+11, among the spectra of
  the 36 quasars that were studied. The paucity of damped Lyα lines
  at small and moderate redshifts shows that the number density of
  damped absorption systems decreases with decreasing redshift. Of
  the observed lines, 44% are identified with Galactic interstellar
  features, 47% with extragalactic absorption systems, and 9% are
  unidentified. Eleven extragalactic C IV doublets are detected. The
  incidence of C IV absorption per unit redshift at &lt;z&gt; ~ 0.3 and
  with W_rest_(λ1548) &gt;= 0.3 A is dN/ dz = 0.9 +/- 0.4, significantly
  lower than the value found at higher redshifts. No obvious correlation
  is found between radio power of the quasars and the seven occurrences
  of associated absorption. Three individual absorption systems are of
  special interest: a broad absorption line system in the spectrum of
  PG 0043+039; a strong, apparently broad high-excitation associated
  absorption system in 3C 351; and a rich, high-excitation intervening
  metal-line system in PKS 2145_06 which has 16 identified lines.

---------------------------------------------------------
Title: G-Modes and the Solar Neutrino Problem
Authors: Bahcall, John N.; Kumar, Pawan
1993ApJ...409L..73B    Altcode: 1993hep.ph....3229B
  We show that low-order g-modes with large enough amplitudes to
  affect significantly the solar neutrino fluxes would produce surface
  velocities that are $10^4$ times larger than the observed upper
  limits and hence are ruled out by existing data. We also demonstrate
  that any large-amplitude, short-period oscillations that grow on a
  Kelvin-Helmholtz time scale will require, to affect solar neutrino
  fluxes, a large amount of energy (for g-modes, $10^9$ times the energy
  in the observed $p-$ mode oscillations) and a tiny amount of dissipation
  (for g-modes, $10^{-8}$ the dissipation rate of the $p$-modes).

---------------------------------------------------------
Title: The Hubble Space Telescope Snapshot Survey. IV. A Summary of
    the Search for Gravitationally Lensed Quasars
Authors: Maoz, D.; Bahcall, J. N.; Schneider, D. P.; Bahcall, N. A.;
   Djorgovski, S.; Doxsey, R.; Gould, A.; Kirhakos, S.; Meylan, G.;
   Yanny, B.
1993ApJ...409...28M    Altcode:
  We report the concluding results of the HST Snapshot Survey for
  gravitationally lensed quasars. New observations of 153 high-luminosity
  z &gt; 1 quasars are presented, bringing to 498 the total number of
  quasars observed in the survey. The new observations do not reveal new
  candidates for gravitational lensing. We present tables summarizing all
  of the snapshot observations, with measured V-magnitudes, accurate to
  0.1 mag, for each of the quasars successfully observed. The tables are
  available on request in machine-readable form. The observed frequency of
  lensing of quasars into multiple images is 3-6 out of 502, depending on
  whether one counts candidates that are not yet securely confirmed and
  cases in which clusters play a role. This frequency is in the range
  predicted by calculations with a vanishing cosmological constant,
  assuming galaxies can be modeled by unevolving isothermal spheres
  dominated in their centers by dark matter. The observed frequency is an
  order of magnitude lower than expected in such models when the universe
  is strongly dominated by a cosmological constant. This conclusion is,
  however, sensitive to the model assumptions and to the precise number
  of actual lensed quasars.

---------------------------------------------------------
Title: Recent work on standard solar models
Authors: Bahcall, John N.
1993NuPhS..31..125B    Altcode: 1992hep.ph...11280B
  Recent results on standard solar models are reviewed. I shall
  summarize briefly three of the themes that I stressed at the Neutrino
  '92 Conference: 1) Different solar model codes give the same answers
  when the same input data are used; 2) Improved calculations of standard
  solar models include helium diffusion, the Livermore radiative opacity,
  the meteoritic iron abundance, and a variety of other corrections; and
  3) There are a few basic rules that should be followed in using standard
  solar models. At the Neutrino '92 Conference, I reviewed in more detail
  the recent work on standard solar models by Marc Pinsonneault and
  myself. This work has by now appeared in print (Rev. Mod. Phys. 64,
  885, 1992, hereafter Paper I, and ApJ Letters, 69, 717, 1992, Paper
  II). Therefore, there is no need for me to repeat the details here.

---------------------------------------------------------
Title: Erratum - Globular Cluster Photometry with the Hubble Space
    Telescope - Part One - Description of the Method and Analysis of
    the Core of 47-TUCANAE
Authors: Guhathakurta, P.; Yanny, B.; Schneider, D. P.; Bahcall, J. N.
1993AJ....105.1607G    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Ultraviolet Absorption Spectrum of the Quasar PKS 0405-12
    and the Local Density of Lyman-Alpha Absorption Systems
Authors: Bahcall, John N.; Jannuzi, Buell T.; Schneider, Donald P.;
   Hartig, George F.
1993ApJ...405..491B    Altcode:
  A sample of 32 absorption lines has been identified in the ultraviolet
  spectrum of the z = 0.57 quasar PKS 0405 - 12. The observations were
  obtained using three R = 1300 gratings of the Faint Object Spectrograph
  of the Hubble Space Telescope. The data cover the wavelength range
  1190- 3260 A. The sample was constructed by requiring that all
  included lines have a measured equivalent width greater than the
  wavelength-dependent 3 σ detection limit for unresolved lines. Sixteen
  of the absorption features are due to Galactic interstellar lines. There
  are 10 extragalactic Lyα absorption lines in the complete sample,
  all with observed equivalent widths greater than or equal to 0.40 A;
  three of the Lyα lines have Lyβ counterparts. The number of Lyα
  lines observed in the spectrum of PKS 0405-12 is within 1 σ of the
  number predicted on the basis of previous HST observations of 3C 273 and
  of H1821 +643. Combining the HST observations of 3C 273, H1821 +643,
  and PKS 0405-12, we estimate the local number density of Lyα systems
  with rest equivalent widths larger than 0.32 A to be dN/dZ(W_res_
  &gt;= 0.32 A) ~ 15 + 4 Lyα lines per unit redshift. Ground-based
  images reveal a rich field of galaxies in the direction of PKS 0405 -
  12, including many galaxies with the brightnesses and sizes expected
  if they belong to a cluster associated with the quasar. The quasar
  spectrum does not show any evidence for absorption at the redshift of
  the emission lines, indicating a covering factor of less than unity
  for the halos of galaxies in the cluster around PKS 0405-12,

---------------------------------------------------------
Title: Do solar-neutrino experiments imply new physics\?
Authors: Bahcall, John N.; Bethe, H. A.
1993PhRvD..47.1298B    Altcode: 1992hep.ph...12204B
  None of the 1000 solar models in a full Monte Carlo simulation
  is consistent with the results of the chlorine or the Kamiokande
  experiments. Even if the solar models are forced artificially to have a
  <SUP>8</SUP>B neutrino flux in agreement with the Kamiokande experiment,
  none of the fudged models agrees with the chlorine observations. The
  GALLEX and SAGE experiments, which currently have large statistical
  uncertainties, differ from the predictions of the standard solar model
  by 2σ and 3σ, respectively.

---------------------------------------------------------
Title: An HST Study of Blue Stragglers in 47 TUC and M15
Authors: Guhathakurta, P.; Yanny, B.; Schneider, D. P.; Bahcall, J. N.
1993ASPC...53...60G    Altcode: 1993blst.conf...60G
  No abstract at ADS

---------------------------------------------------------
Title: Stellar Photometry in the Core of 47-TUCANAE Using HST
Authors: Guhathakurta, P.; Yanny, B.; Schneider, D. P.; Bahcall, J. N.
1993ASPC...50..303G    Altcode: 1993sdgc.proc..303G
  No abstract at ADS

---------------------------------------------------------
Title: Uncertainties in the calculated solar neutrino fluxes
Authors: Bahcall, J. N.
1993paas.conf...63B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: HST Observations of Globular Cluster Cores
Authors: Yanny, B.; Guhathakurta, P.; Schneider, D. P.; Bahcall, J. N.
1993ASPC...50..275Y    Altcode: 1993sdgc.proc..275Y
  No abstract at ADS

---------------------------------------------------------
Title: The Hubble Space Telescope Snapshot Survey. III. Further
    Observations in Search of Gravitationally Lensed Quasars
Authors: Maoz, D.; Bahcall, J. N.; Doxsey, R.; Schneider, D. P.;
   Bahcall, N. A.; Lahav, O.; Yanny, B.
1993ApJ...402...69M    Altcode:
  We present new HST Snapshot Survey observations of 163 high-luminosity z
  &gt; 1 quasars, bringing the total number observed to date in the survey
  to 347 quasars. Each exposure was searched for evidence of gravitational
  lensing. Among the newly observed quasars, six have additional point
  sources at separations of 2"-6", but in all six cases ground-based data
  indicate that gravitational lensing is not involved. No point sources
  were found at smaller separations. Counting the one new lens candidate
  the survey has uncovered (1208+1011, described in previous papers)
  and the known lenses excluded from the sample, the observed frequency
  of lensing of quasars by galaxies is 5/351. This frequency is in the
  range predicted by models with a vanishing cosmological constant, but
  an order of magnitude lower than expected in models strongly dominated
  by a cosmological constant. The HST pointing accuracy under gyroscope
  control has improved and is now 14"+/- 9" (mean and rms).

---------------------------------------------------------
Title: Summary Talk: International Symposium on Neutrino Astrophysics,
    Takayama/Kamioka (10/'92)
Authors: Bahcall, John
1992hep.ph...12262B    Altcode:
  Contents: 1. The Conference 2. Solar Neutrinos -A. Operating Experiments
  -B. New Funded Experiments -C. Are Solar Neutrino Fluxes Time
  Dependent? -D. Have $pp$ Neutrinos Been Detected? -E. Is Directionality
  Required for Astronomical Observations? -F. Is There a Solar Neutrino
  Problem? -G. What Have We Learned? 3. Supernova Neutrinos 4. Atmospheric
  Neutrinos 5. High-Energy Neutrinos 6. Our Field Is Flourishing

---------------------------------------------------------
Title: Radial Density Profiles in the Centers of 47 TUC and M15 from
    HST Images
Authors: Yanny, B.; Guhathakurta, P.; Schneider, D. P.; Bahcall, J. N.
1992AAS...18110802Y    Altcode: 1992BAAS...24.1294Y
  Hubble Space Telescope Planetary Camera (HST/PC) images of the
  centers of the dense Galactic globular clusters 47 Tuc and M 15 are
  presented. We study the radial dependence of the surface density of
  post-main sequence stars and the surface brightness of the diffuse
  light of faint unresolved stars below the main sequence turnoff. The
  radial profile of 47 Tuc is fit well by a King model with core radius
  r_c=23” (0.5 pc). The extremely high density of stars near the center
  of post-core collapse cluster M 15 and the broad wings of the point
  spread function (PSF) caused by spherical aberration in HST's primary
  mirror combine to make stellar photometry a painstaking process A
  technique, specially designed to work in crowded fields, has been
  used to derive an empirical PSF model and make a fit to the stellar
  images. Accurate fitting and subtraction of the light of bright red
  giant stars and estimating the incompleteness as a function of radius
  and magnitude are crucial to this study. Realistic simulated images
  have been constructed and analyzed for this purpose. We compare the M
  15 data to simulations with a small, but finite core (r_c=2”=0.1pc)
  and those with mild central cusps (surface density ~ r(-alpha ) ,
  where alpha =0.5-0.8).

---------------------------------------------------------
Title: Globular Cluster Photometry with HST: Color-Mag Diagrams in
    the Dense Cores of 47 TUC and M15
Authors: Guhathakurta, P.; Yanny, B.; Schneider, D. P.; Bahcall, J. N.
1992AAS...181.4307G    Altcode: 1992BAAS...24Q1188G
  We present accurate (sigma ~ 0.1 mag), multi-color photometry of
  stars in the cores of two of the densest known Galactic globular
  clusters, 47 Tuc and M15, using images obtained with the Hubble Space
  Telescope's Planetary Camera (HST/PC). Despite the spherical aberration
  in HST's primary mirror, the high angular resolution of the PC images
  makes it possible to construct reliable color-magnitude diagrams of
  post-main sequence stars even in the most crowded portions of these
  clusters. This task has proven impossible from the ground in the best
  of seeing conditions (FWHM ~ 0.5”). We have developed a technique that
  constructs an empirical model of the stellar point spread function (PSF)
  from a PC image of a globular cluster core. The technique corrects
  for saturation in the stellar cores (caused by the limited dynamic
  range of the CCD detector) and attempts to track the variation in
  the shape of the PSF across the image. Detailed knowledge of the PSF
  is essential in order to do crowded field stellar photometry; note,
  the low level wings of the PSF extend beyond a radius of 2.5” while
  the average projected separation between stars in these cluster cores
  is less than 1”. The PSF modeling and stellar photometry technique
  has been tested and calibrated with the help of realistic simulated
  images. Color-magnitude diagrams (U-V and V-I versus V) of 47 Tuc
  and M15 reveal a few dozen blue straggler stars within the central
  1 arcmin(2) of each cluster. The blue stragglers are more centrally
  concentrated than the average post-main sequence star and are consistent
  with having masses equal to 2m_turnoff. The ratio of the number of
  bright red giant branch stars to horizontal branch stars does not vary
  with radius within the inner 1' of 47 Tuc. In M15, that ratio declines
  near the cluster center, consistent with the hypothesis that the red
  giant envelopes have been destroyed in this region of extremely high
  stellar density.

---------------------------------------------------------
Title: Faint Object Spectrograph Observations of the Large-Redshift
    Gravitational Lens Candidate 1208+1011
Authors: Bahcall, John N.; Hartig, George F.; Jannuzi, Buell T.;
   Maoz, Dan; Schneider, Donald P.
1992ApJ...400L..51B    Altcode:
  We report HST spectroscopic observations of the z = 3.8 gravitational
  lens candidate 1208+1011. Low-dispersion (R = 200) Faint Object
  Spectrograph data, covering the wavelength range 3700-7800 A, were
  obtained for each of the two components (V ~18.3 and 19.8 mag) and
  for a comparison (blank) field; the fainter component and the blank
  field are both separated by 0.47" from the brighter image. The spectra
  of both components possess strong Lyα/N V and O VI/Lyβ emission
  lines at a redshift of 3.8 as well as a number of similar absorption
  features. Both components have a ratio of the equivalent widths of the O
  VI complex to the Lyα complex much larger than the typical value seen
  in large-redshift quasars. There are small differences in the measured
  profiles of the Lyα and O VI/Lyβ emission lines of the images. These
  differences could be caused by absorption along different paths to
  a single lensed object, by unequal imaging of extended emissions,
  by systematic measuring errors, or by intrinsic differences in two
  nearly identical neighboring quasars.

---------------------------------------------------------
Title: Element Diffusion in the Solar Interior
Authors: Thoul, A. A.; Bahcall, J. N.; Loeb, A.
1992AAS...181.8106T    Altcode: 1992BAAS...24.1253T
  We study the diffusion of helium and other heavy elements in the
  solar interior, using the flow equations developed by Burgers (1969)
  for a multi-component fluid. The set of equations is solved exactly,
  including the residual heat flow terms. No approximation is made about
  the relative concentrations and no restriction is placed on the number
  of elements considered. For helium diffusion, we compare our results
  with those obtained by Bahcall and Loeb (1990) using a simplified
  treatment with heat flows neglected. We find that the inclusion of
  the residual heat flow terms leads to a significant increase in the
  helium diffusion velocity. However, we also find that the temperature
  and charge-dependence of the Coulomb logarithm has the opposite effect,
  leading to a decrease in the helium diffusion velocity. By coincidence,
  the two effects partially cancel each other out throughout most of
  the solar interior. Our complete treatment of element diffusion could
  be directly incorporated in a standard stellar evolution code, but,
  for convenience, we also give simple analytical fits of our numerical
  results. Burgers, J.M. 1969, Flow equations for composite gases(Academic
  Press, New York). Bahcall, J.N., and Loeb, A. 1990, Ap.J.,360, 267.

---------------------------------------------------------
Title: Globular Cluster Photometry With the Hubble Space
    Telescope. I. Description of the Method and Analysis of the Core of
    47 TUC
Authors: Guhathakurta, Puragra; Yanny, Brian; Schneider, Donald P.;
   Bahcall, John N.
1992AJ....104.1790G    Altcode:
  Accurate photometry for individual post-main-sequence stars in the core
  of the Galactic globular cluster 47 Tuc is presented and analyzed using
  an empirical point spread function model and Monte Carlo simulations. A
  V vs. V-I color-magnitude diagrams is constructed which shows several
  distinct stellar types, including RGB and HB stars. Twenty-four blue
  straggler stars are detected in 47 Tuc, more concentrated toward the
  center of the cluster than the giants. This supports the hypothesis is
  that the stragglers are either coalesced stars or members of binary
  systems that are more massive than single stars. The radial profile
  of the projected stellar density is flat in the central region of 47
  Tuc with a core radius of 23 +/- 2 arcsec. No signature of a collapsed
  core is evident. The observed radial cumulative distribution of stars
  rules out the presence of a massive compact object in the center.

---------------------------------------------------------
Title: The Near-Ultraviolet Spectrum of Markarian 205
Authors: Bahcall, John N.; Jannuzi, Buell T.; Schneider, Donald P.;
   Hartig, George F.; Jenkins, Edward B.
1992ApJ...398..495B    Altcode:
  We report measurements of the absorption and of the emission lines
  between 1600 and 3200 A in the spectrum of the nearby AGN Markarian 205
  (z = 0.071), which lies at a projected distance of 3 kpc (H_0_= 100 km
  s^-1^) from the nucleus of the nearby barred spiral galaxy NGC 4319 (z
  = 0.0047). The results were obtained using high-resolution (R = 1300)
  observations with the Faint Object Spectrograph of the Hubble Space
  Telescope. A total of 15 absorption lines, 13 of which are produced
  by Galactic gas, and four AGN emission lines are detected. Two of the
  absorption lines, the Mg II resonant doublet, are produced by gas
  in the intervening galaxy NGC 4319. This is the first detection of
  absorption due to intervening gas in this famous quasar-galaxy pair.

---------------------------------------------------------
Title: Standard solar models, with and without helium diffusion,
    and the solar neutrino problem
Authors: Bahcall, J. N.; Pinsonneault, M. H.
1992RvMP...64..885B    Altcode:
  We first show that, with the same input parameters, the standard solar
  models of Bahcall and Ulrich; of Sienkiewicz, Bahcall, and Paczyński
  of Turck-Chièze, Cahen, Cassé, and Doom; and of the current Yale code
  all predict event rates for the chlorine experiment that are the same
  within +/-0.1 SNU (solar neutrino units), i.e., approximately 1% of
  the total calculated rate. We then construct new standard solar models
  using the Yale stellar evolution computer code supplemented with a more
  accurate (exportable) nuclear energy generation routine, an improved
  equation of state, recent determinations of element abundances, and the
  new Livermore (OPAL) opacity calculations. We evaluate the individual
  effects of different improvements by calculating a series of precise
  models, changing only one aspect of the solar model at a time. We
  next add a new subroutine that calculates the diffusion of helium with
  respect to hydrogen with the aid of the Bahcall-Loeb formalism. Finally,
  we compare the neutrino fluxes computed from our best solar models
  constructed with and without helium diffusion. We find that helium
  diffusion increases the predicted event rates by about 0.8 SNU, or 11%
  of the total rate, in the chlorine experiment; by about 3.5 SNU, or 3%,
  in the gallium experiments; and by about 12% in the Kamiokande and SNO
  experiments. The best standard solar model including helium diffusion
  and the most accurate nuclear parameters, element abundances, radiative
  opacity, and equation of state predicts a value of 8.0+/-3.0 SNU for the
  <SUP>37</SUP>Cl experiment and 132<SUP>+21</SUP><SUB>-17</SUB> SNU for
  the <SUP>71</SUP>Ga experiment. The quoted errors represent the total
  theoretical range and include the effects on the model predictions of
  3σ errors in measured input parameters. All 15 calculations since 1968
  of the predicted rate in the chlorine experiment given in this series
  of papers are consistent with both the range estimated in the present
  work and the 1968 best-estimate value of 7.5+/-2.3 SNU. Including
  the effects of helium diffusion and the other improvements in
  the description of the solar interior that are implemented in this
  paper, the inferred primordial solar helium abundance is Y=0.273. The
  calculated depth of the convective zone is R=0.707R<SUB>solar</SUB>,
  in agreement with the value of 0.713R<SUB>solar</SUB> inferred by
  Christensen-Dalsgaard, Gough, and Thompson from a recent analysis
  of the observed p-mode oscillation frequencies. Including helium
  diffusion increases the calculated present-day hydrogen surface
  abundance by about 4%, decreases the helium abundance by approximately
  11%, and increases the calculated heavy-element abundance by about
  4%. In the Appendix, we present detailed numerical tables of our best
  standard solar models computed both with and without including helium
  diffusion. In the context of the MSW (Mikheyev-Smirnov-Wolfenstein)
  or other weak-interaction solutions of the solar neutrino problem,
  the numerical models can be used to compute the influence of the matter
  in the sun on the observed neutrino fluxes.

---------------------------------------------------------
Title: Star Counts From The HST SnapShot Survey
Authors: Gould, A.; Bahcall, J. N.; Maoz, D.
1992AAS...181.3809G    Altcode: 1992BAAS...24.1179G
  No abstract at ADS

---------------------------------------------------------
Title: Hubble Space Telescope Wide Field Camera Imaging of the
    Gravitational Lens 2237+0305
Authors: Rix, Hans-Walter; Schneider, Donald P.; Bahcall, John N.
1992AJ....104..959R    Altcode:
  Hubble Space Telescope Wide Field Camera images of the gravitational
  lens 2237+0305 in the F336W ("U") and F702W ("A") filters are used to
  construct models of the system. Positions for the four quasar images,
  accurate to +/-0.015", and relative magnitudes in U and R, accurate
  to +/-0.06 and 0.04 mag respectively, are determined. The upper limits
  on the observed brightness of the fifth image are found to be &lt;~7%
  of the brightest quasar image. The long "color baseline," from R to U,
  permits good estimates of the differential image reddening. With M/L as
  the only free parameter describing the lens and two further parameters
  describing the position of the quasar in the source plane, the eight
  quasar image positions can be reproduced to within ~0.03" (or 2.5% of
  their separations); at the same time the three relative brightnesses can
  be reproduced to within factors of 1.5. The total image amplification is
  well constrained by these models: a factor of 18.5+/-2. This modeling
  assumes only that the surface mass density of the lens galaxy is
  proportional to the observed surface brightness. The mass of the
  lens inside 0.9" is found to be 1.08+/-0.02X10^10^M_sun_h^-1^_100_
  corresponding to a mass-to-light ratio in B of 12.3h_100_. This
  M/L estimate agrees with values obtained from stellar dynamics
  for other elliptical galaxies. The mass in the inner 500h^-1^_100_
  pc is constrained by these phenomenological models to within +/-2%,
  a more precise mass determination than for any other known bulge or
  elliptical. A comparison of predictions from this mass model with the
  measured central velocity dispersion yields a distance independent
  agreement to within 10%, assuming isotropic velocity dispersions. The
  influence of the mass associated with the Mg II absorber at z = 0.9 on
  the lensing appears to be unimportant. The detailed agreement of the
  lens model with the observations of 2237+0305, achieved by using the
  lens equations of general relativity and the cosmological interpretation
  of quasar redshifts, provides confirmation of these standard theories.

---------------------------------------------------------
Title: The Ultraviolet Absorption Spectrum of the Quasar H1821+643
    (z = 0.297)
Authors: Bahcall, John N.; Jannuzi, Buell T.; Schneider, Donald P.;
   Hartig, George F.; Green, Richard F.
1992ApJ...397...68B    Altcode:
  We report measurements of the absorption lines in the ultraviolet
  spectrum of the nearby luminous quasar H1821+643 (z = 0.297). The
  results were obtained using high-resolution observations with the
  faint object spectrograph of the Hubble Space Telescope. A total of
  51 absorption lines and a number of emission features were detected
  between 1190 and 3260 A. A complete sample of 38 absorption lines was
  constructed with the detection limit defined in terms of a limiting
  equivalent width as a function of wavelength. The identifications with
  interstellar and with extragalactic lines were made with the aid of
  software that utilizes the limiting detection sensitivity as a function
  of wavelength and the known atomic properties of cosmologically abundant
  ions. The majority of the absorption features are Galactic interstellar
  lines. The interstellar absorption lines and the quasar emission lines
  present in the spectrum of H1821+643 are similar to the lines observed
  in other small-redshift quasars. There are five strong extragalactic
  Lyα absorption lines in the spectrum of H1821+643, all with observed
  equivalent widths greater than 0.45 A. Combining the HST observations
  of 3C 273 and H1821+643, we estimate the local number density of
  Lyα systems with rest equivalent widths larger than 0.32 A to be
  (dN/dz)_0_~13 +/- 5 Lyα lines per unit redshift. Some of the Lyα
  systems with redshifts significantly different from the quasar appear
  to be associated with galaxies or with clusters of galaxies. Two of the
  Lyα lines have the same redshift within c{DELTA}z = 400 km s^-1^ as
  that of an emission-line galaxy located at a projected separation from
  the quasar of approximately 90 kpc (H_0_ = 100 km s^-1^ Mpc^-1^). This
  system at z = 0.226 is part of a triplet of Lyα lines that have a total
  redshift separation of cz = +/- 450 km s^-1^. There is also statistical
  evidence that some of the Lyα systems are clumped more than would be
  expected if they were distributed randomly along the line of sight
  to H1821+643. Many of the Lyα systems observed at small redshifts
  may be associated with large hydrogen halos of galaxies or groups and
  clusters of galaxies. One of the Lyα systems in H1821+643 occurs at an
  absorption redshift approximately equal to the emission-line redshift
  of the quasar and is accompanied by absorption from the C IV and O
  VI doublets; this is an example of what has been called associated
  absorption, z_abs_~z_em, for large-redshift quasars. No lines from
  low-ionization ions are detected in this system. The observations
  of H1821+643 fail to confirm previous suggestions that associated
  absorption is correlated with strong radio emission (H1821+643 is
  radio-quiet) or with low optical luminosity (H1821+643 is comparable
  in luminosity to 3C 273). The observations are consistent with two
  previously proposed conjectures, that associated absorption is produced
  in clusters of galaxies containing the quasars or that the absorption
  is produced in the gas associated with the quasars.

---------------------------------------------------------
Title: Helium Diffusion in the Sun
Authors: Bahcall, J. N.; Pinsonneault, M. H.
1992ApJ...395L.119B    Altcode:
  We calculate improved standard solar models using the new Livermore
  (OPAL) opacity tables, an accurate (exportable) nuclear energy
  generation routine which takes account of recent measurements and
  analyses, and the recent Anders-Grevesse determination of heavy element
  abundances. We also evaluate directly the effect of the diffusion of
  helium with respect to hydrogen on the calculated neutrino fluxes,
  on the primordial solar helium abundance, and on the depth of the
  convective zone. Helium diffusion increases the predicted event rates by
  about 0.8 SNU, or 11 percent of the total rate, in the chlorine solar
  neutrino experiment, by about 3.5 SNU, or 3 percent, in the gallium
  solar neutrino experiments, and by about 12 percent in the Kamiokande
  and SNO solar neutrino experiments. The best standard solar model
  including helium diffusion and the most accurate nuclear parameters,
  element abundances, and radiative opacity predicts a value of 8.0 SNU
  +/- 3.0 SNU for the C1-37 experiment and 132 +21/-17 SNU for the Ga -
  71 experiment, where the uncertainties include 3 sigma errors for all
  measured input parameters.

---------------------------------------------------------
Title: Monte Carlo exploration of Mikheyev-Smirnov-Wolfenstein
    solutions to the solar neutrino problem
Authors: Shi, X.; Schramm, D. N.; Bahcall, J. N.
1992PhRvL..69..717S    Altcode:
  We explore the impact of astrophysical uncertainties on the
  Mikheyev-Smirnov-Wolfenstein (MSW) solution by calculating the allowed
  MSW solutions for 1000 different solar models with a Monte Carlo
  selection of solar model input parameters, assuming a full three-family
  MSW mixing. Applications are made to the chlorine, gallium, Kamiokande,
  and Borexino experiments. The initial GALLEX result limits the mixing
  parameters to the upper diagonal and the vertical regions of the MSW
  triangle. We also calculate the expected event rates in the Borexino
  experiment assuming the MSW solutions implied by GALLEX.

---------------------------------------------------------
Title: Accurate Positions and Finding Charts for 528 High-Redshift,
    Luminous Quasars
Authors: Schneider, Donald P.; Bahcall, John N.; Saxe, David H.;
   Bahcall, Neta A.; Doxsey, Rodger; Golombek, Daniel; Krist, John;
   McMaster, Matt; Meakes, Michael; Lahav, Ofer
1992PASP..104..678S    Altcode:
  We present finding charts and J2000 positions accurate to 1" for the 528
  high-redshift (z &gt; 1), luminous (M_V &lt; -25.5) quasars investigated
  in the Hubble Space Telescope Snapshot Survey. The information was
  produced with the Space Telescope Science Institute's Astrometric
  Support Program. (SECTION: Galaxies)

---------------------------------------------------------
Title: Gravitational Lensing of Quasars as Seen by the Hubble Space
    Telescope Snapshot Survey
Authors: Maoz, D.; Bahcall, J. N.; Doxsey, R.; Schneider, D. P.;
   Bahcall, N. A.; Lahav, O.; Yanny, B.
1992ApJ...394...51M    Altcode:
  As part of the ongoing HST Snapshot Survey, 152 additional high-
  luminosity z &gt; 1 quasars were observed, bringing the total to
  184 quasars. Each exposure was searched for evidence of gravitational
  lensing. Only one quasar among those observed, 1208+1011, is a candidate
  lens system with subarcsecond image separation. Six other quasars have
  point sources within 6". Ground-based observations of five of these
  cases show that the companion point sources are foreground Galactic
  stars. The observed lensing frequency, after accounting for known
  lenses excluded from the sample, and including 32 quasars observed
  from a pilot sample described in a previous paper, is 3/184. The
  predicted lensing frequency of the sample is calculated for a variety
  of cosmological models. The effect of uncertainties in some of the
  observational parameters upon the predictions is discussed. The
  observed lensing frequency is consistent with predictions of models
  with a zero cosmological constant λ. Assuming the best estimates for
  the parameters involved in the calculation, flat cosmologies with λ
  &gt; 0.85 can be ruled out at greater than 95% confidence. From the
  engineering perspective, we find that the software corrections for
  stellar aberration when the telescope is guided on gyroscopes results
  in drift rates of 1-2 milliarcseconds s^-1^, about 3 times smaller
  than before the correction was implemented. The mean and rms pointing
  error under gyro control is 20" +/- 13". We find no correlation of the
  drift rate with time, right ascension, declination, or pointing error.

---------------------------------------------------------
Title: Quasar Absorption Line Survey - Cycle 3 High - Part 3
Authors: Bahcall, John
1992hst..prop.5225B    Altcode:
  PART 3 consists of replacement targets for objects pulled from the
  original submission because targets had been previously observed in
  other programs. The Absorption Line Survey of bright quasars provides
  a homogeneous data base for studying fundamental questions about the
  origin and evolution of gaseous systems in the universe. The initial
  results determine at small redshifts the number densities of Ly-ALPHA
  systems, of metal-lines and extragalactic halos, of Lyman-limit systems,
  of associated absorption systems, and the shapes and intensities of
  quasar emission lines and spectral energy distributions. The survey
  reveals that much of the sky is covered by high or very high velocity
  metal-line clouds present in the Galactic halo. A larger sample,
  which includes the requested Cycle 3 observations, is required to
  answer many important questions. (See abstract_temp for Part 1, P4581)

---------------------------------------------------------
Title: Quasar Absorption Line Survey - Cycle 3 High - Part 2
Authors: Bahcall, John
1992hst..prop.5081B    Altcode:
  PART 2 consists of replacement targets for objects pulled from the
  original submission because targets had been previously observed in
  other programs. The Absorption Line Survey of bright quasars provides
  a homogeneous data base for studying fundamental questions about the
  origin and evolution of gaseous systems in the universe. The initial
  results determine at small redshifts the number densities of Ly-ALPHA
  systems, of metal-lines and extragalactic halos, of Lyman-limit systems,
  of associated absorption systems, and the shapes and intensities of
  quasar emission lines and spectral energy distributions. The survey
  reveals that much of the sky is covered by high or very high velocity
  metal-line clouds present in the Galactic halo. A larger sample,
  which includes the requested Cycle 3 observations, is required to
  answer many important questions. (See abstract_temp for Part 1, P4581)

---------------------------------------------------------
Title: Quasar Absorption Line Survey - Cycle 3 High
Authors: Bahcall, John
1992hst..prop.4581B    Altcode:
  The Absorption Line Survey of bright quasars provides a homogeneous
  data base for studying fundamental questions about the origin and
  evolution of gaseous systems in the universe. The initial results
  determine at small redshifts the number densities of Ly-ALPHA systems,
  of metal-lines and extragalactic halos, of Lyman-limit systems,
  of associated absorption systems, and the shapes and intensities of
  quasar emission lines and spectral energy distributions. The survey
  reveals that much of the sky is covered by high or very high velocity
  metal-line clouds present in the Galactic halo. A larger sample, which
  includes the requested Cycle 3 observations, is required to answer many
  important questions. For example, what is the correlation function
  of Ly-ALPHA systems at small redshifts\? What fraction of the metal,
  the Ly-ALPHA, and the Ly-limit systems are associated with galaxies
  and what are the characteristic sizes of the outer gaseous regions of
  different types of galaxies\? Do absorbing systems show evidence of the
  large-scale structure seen with galaxies and clusters of galaxies\? The
  observations requested in Cycle 3 will extend the region of coverage
  of the Key Project sample from the redshift range of z = 0.0 to 1.0
  (Cycles 1&amp; 2) to z = 0.0 to 1.6 (Cycles 1-3). The increase in sample
  size will be sufficient to determine, in conjunction with ground-based
  observations at large redshifts, the evolution of Ly-ALPHA and of
  metal-line systems from early cosmic times to the present epoch.

---------------------------------------------------------
Title: Hubble Space Telescope Imaging of the Large-Redshift
    Gravitational Lens Candidate 1208+1011
Authors: Bahcall, John N.; Maoz, Dan; Schneider, Donald P.; Yanny,
   Brian; Doxsey, Rodger
1992ApJ...392L...1B    Altcode:
  Four-color photometry obtained with the Hubble Space Telescope is
  consistent with the hypothesis that the light from the quasar 1208+1011
  (z = 3.8) is gravitationally lensed. Guided exposures taken with the
  HST Planetary Camera resolve the quasar image into two point-source
  components separated by 0.476" +/- 0.004". The intensity ratio of
  the components is approximately 4:1 in each of four broad-band HST
  filters with mean wavelengths of 4352, 5416, 6898, and 8922 A. The
  HST photometry, when combined with high-resolution ground-based
  spectroscopy, rules out the possibility that the secondary component
  is a Galactic star. The limit on additional point sources is 3% of
  the brighter image for separations greater than 0.5" from the primary
  component and 5% of the brighter component for separations between 0.1"
  and 0.5". If the gravitational lens is an ordinary galaxy, it would
  not have been detected on the HST images.

---------------------------------------------------------
Title: The Cluster of Galaxies Associated with the Low-Redshift
    Quasar H1821+643
Authors: Schneider, Donald P.; Bahcall, John N.; Gunn, James E.;
   Dressler, Alan
1992AJ....103.1047S    Altcode:
  Low resolution spectra have been obtained of eight R~19 mag galaxies
  located within 1 arcmin of the low-redshift, high luminosity quasar
  H1821 + 643. Six of the eight galaxies belong to a cluster that has the
  same redshift, within the observational errors, as the quasar. Five
  of the six cluster members have the spectra of early type galaxies;
  the spectrum of the sixth cluster member contains Hα, O [III], and
  possibly O II emission lines. The other two objects are an emission
  line foreground galaxy and a back-ground galaxy. The cluster has
  a Galactocentric redshift of 0.299+/- 0.002 and a radial velocity
  dispersion of 1050 + 320 km s^-1^. The photometric and spectroscopic
  data suggest that H1821 + 643 is associated with a rich cluster of
  galaxies.

---------------------------------------------------------
Title: Local Dark Matter from a Carefully Selected Sample
Authors: Bahcall, John N.; Flynn, Chris; Gould, Andrew
1992ApJ...389..234B    Altcode:
  The precise data obtained by Flynn and Freeman (1991) on K giants
  at the south Galactic pole are used to analyze the amount of local
  dark matter in which the systematic effects can be modeled easily and
  evaluated accurately. The method of Bahcall (1984) is employed to solve
  the self-consistent equations for the distribution of dark matter. The
  K-giant survey is found to provide significant evidence for disk dark
  matter. Taking into account all recognized sources of error using a
  statistical test devised by Gould (1989, 1990), a model with no dark
  matter is inconsistent with the data at the 86-percent confidence
  level. The best-fit P-model (in which dark matter is distributed
  proportionally to known matter) has 53 percent more dark matter than
  visible matter.

---------------------------------------------------------
Title: The Snapshot Survey: A Search for Gravitationally Lensed
    Quasars with the Hubble Space Telescope
Authors: Bahcall, J. N.; Maoz, D.; Doxsey, R.; Schneider, D. P.;
   Bahcall, N. A.; Lahav, O.; Yanny, B.
1992ApJ...387...56B    Altcode:
  In a systematic attempt to find new examples of multiply imaged quasars
  that are the result of gravitational lensing, 89 short exposures,
  through two filters, of high-luminosity quasars from a well-defined
  sample have been obtained with the Hubble Space Telecope's Planetary
  Camera. Useful high-resolution images of approximately 30 quasars
  have resulted. None of the quasars show evidence of multiple images
  due to gravitational lensing. Simulations show that multiple images
  with brightness ratios of up to several magnitudes would have been
  detected, down to image separations of ~0.1". These results are compared
  with lower resolution ground-based surveys and current theoretical
  predictions. The Snapshot Survey has uncovered several engineering
  problems in the observatory's performance, some of which have already
  been corrected. In particular, we find that the large telescope
  pointing errors and drift rates are primarily the result of the lack
  of correction for stellar aberration when pointing and tracking are
  performed solely with gyroscopes. The implications of the possibly low
  intrinsic gyro drift rate on future observations are briefly discussed.

---------------------------------------------------------
Title: A Gravitational Lens Candidate Discovered with the Hubble
    Space Telescope
Authors: Maoz, Dan; Bahcall, John N.; Schneider, Donald P.; Doxsey,
   Rodger; Bahcall, Neta A.; Filippenko, Alexei V.; Goss, W. M.; Lahav,
   Ofer; Yanny, Brian
1992ApJ...386L...1M    Altcode:
  We report evidence for gravitational lensing of the high-redshift (z
  = 3.8) quasar 1208+101, observed as part of the Snapshot Survey with
  the Hubble Space Telescope Planetary Camera. An HST V image taken on
  gyroscopes resolves the quasar into three point-source components,
  with the two fainter images having separations of 0.1" and 0.5" from
  the central bright component. A radio observation of the quasar with
  the Very Large Array at 2 cm shows that, like most quasars of this
  redshift, 1208+101 is radio-quiet. Based on positional information
  alone, the probability that the observed optical components are chance
  superpositions of Galactic stars is small, but not negligible. Analysis
  of a combined ground-based spectrum of all three components, using
  the relative brightnesses from the HST image, supports the lensing
  hypothesis. If all the components are lensed images of the quasar,
  the observed configuration cannot be reproduced by simple lens
  models. Future HST observations can test the lensing hypothesis for
  1208+101.

---------------------------------------------------------
Title: What do solar models tell us about solar neutrino experiments?
Authors: Bahcall, John N.
1992AIPC..272.1111B    Altcode: 1992hep.ph...11291B
  If the published event rates of the chlorine and Kamiokande solar
  neutrino experiments are correct, then the energy spectrum of neutrinos
  produced by the decay of 8B in the sun must be different from the energy
  spectrum determined from laboratory nuclear physics measurements. This
  change in the energy spectrum requires physics beyond the standard
  electroweak model. In addition, the GALLEX and SAGE experiments,
  which currently have large statistical uncertainties, differ from the
  predictions of the standard solar model by 2σ and 3σ, respectively.

---------------------------------------------------------
Title: Women in astronomy: a sampler of issues and ideas.
Authors: Barlow, N.; Cordova, F. A.; Bahcall, J.; Price, J.; Eastwood,
   K.; Bahcall, N.; Clayton, G.; Lutz, J.; Bell Burnell, J.; Hunter, D.;
   Rubin, V.; McFadden, L.; Faber, S.; Knapp, G.; Alvarez Del Castillo,
   E. M.; Trimble, V.
1992Mercu..21...27B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: An Issue of Neglect for Astronomy?
Authors: Harrison, Shirley W.; Zirin, Harold; Bahcall, John N.
1992PhT....45b.128H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar neutrinos and the Mikheyev-Smirnov-Wolfenstein theory
Authors: Bethe, Hans A.; Bahcall, John N.
1991PhRvD..44.2962B    Altcode:
  The observation of solar neutrinos by Kamiokande shows that
  the solar-neutrino problem cannot be solved by changing
  the solar model. In combination with the observations
  with a chlorine detector, it makes the nonadiabatic form
  of the Mikheyev-Smirnov-Wolfenstein theory most likely, and
  determines Δm<SUP>2</SUP>sin<SUP>2</SUP>θ=1.0×10<SUP>-8</SUP>
  eV<SUP>2</SUP>. Probably all neutrinos go through the resonance
  in the Sun, those from <SUP>8</SUP>B nonadiabatically, all others
  adiabatically. The latter emerge from the Sun in the higher-mass
  eigenstate ν<SUB>2</SUB> and have a probability sin<SUP>2</SUP>θ
  to be detected as ν<SUB>e</SUB>. The gallium experiments,
  when done with sufficient accuracy, will be able to determine
  Δm<SUP>2</SUP>=m<SUP>2</SUP>(ν<SUB>μ</SUB>)-m<SUP>2</SUP>(ν<SUB>e</SUB>)
  within fairly close limits. If the day-night effect can be
  measured, it will further constrain these limits. The small value
  of Δm<SUP>2</SUP>sin<SUP>2</SUP>θ explains why the oscillation
  from ν<SUB>e</SUB> to ν<SUB>μ</SUB> has not been observed in the
  laboratory. From existing experiments, the temperature at the center of
  the Sun can be determined to be within about 6% of that derived from
  the standard solar model; future neutrino experiments may determine
  it to within 1%.

---------------------------------------------------------
Title: Ultraviolet HST Spectra of Three Small Redshift Quasars
Authors: Bahcall, J. N.; Jannuzi, B.; Schneider, D. P.; Hartig, G.
1991BAAS...23.1344B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Shapes of solar-neutrino spectra: Unconventional tests of
    the standard electroweak model
Authors: Bahcall, John N.
1991PhRvD..44.1644B    Altcode:
  The shapes of the neutrino energy spectra produced by β decays
  or by nuclear reactions in the solar interior are compared to the
  corresponding spectral shapes that are produced in a terrestrial
  laboratory. The most important effects of the Sun, caused by thermal
  motion of the neutrino-emitting nuclei and by gravitational redshifts,
  are shown to be small. Any currently measurable difference between the
  observed shape of a solar-neutrino energy spectrum and the spectrum
  shape for a terrestrial neutrino source must be due to a departure
  from the standard electroweak model.

---------------------------------------------------------
Title: The HST Snapshot Survey: A Progress Report on New Gravitational
    Lenses and Lensing Statistics
Authors: Maoz, D.; Bahcall, J. N.; Schneider, D. P.; Doxsey, R.;
   Bahcall, N. A.; Lahav, O.; Yanny, B.
1991BAAS...23.1352M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Ultraviolet Absorption Spectrum of 3C 273
Authors: Bahcall, J. N.; Jannuzi, B. T.; Schneider, D. P.; Hartig,
   G. F.; Bohlin, R.; Junkkarinen, V.
1991ApJ...377L...5B    Altcode:
  We identify six Lyα absorption systems with equivalent widths greater
  than 0.2 A in the ultraviolet spectrum of the nearby quasar 3C 273,
  more than expected on the basis of extrapolations of the observed
  number of Lyα clouds seen at large redshifts. Two Lyα lines appear
  to be produced by gas in the Virgo Cluster or by the halos of galaxies
  associated with the Virgo Cluster. We also detect all the interstellar
  absorption lines that are expected on the basis of abundance, atomic
  physics, and ionization considerations.

---------------------------------------------------------
Title: Quasar Absorption Line Survey: Cycle 2 Observations
    Observations of OJ287 and PG1718+481
Authors: Bahcall, John
1991hst..prop.4817B    Altcode:
  The Quasar Absorption Line Survey of bright sources is an efficient
  observing program designed to provide a homogeneous data base of
  absorption features. The data will reveal absorption regions in
  galaxies, in clusters of galaxies, in voids, in large-scale structures,
  in Lyman ALPHA clouds, and wi provide information about damped Lyman
  ALPHA and Lyman-limit systems. The survey will determine, with high SNR,
  the profiles of &gt; 200 emission lines. Using the estimated numbers
  of observed absorption lines, including archi val data, the program was
  designed to determine the cosmic evolution of absorption systems. High
  resolution spectra of a sample of quasars will be obtained with the FOS;
  the spectra will have a rest frame equivalent width detection limit
  for unresolved absorption lines of 0.3 A. The survey data base will
  address fundamental questions, for example: What is the strength and
  origin of the UV background radiation\? How do gaseous galactic disks
  and halos evolve with redshift\? What processes govern the ionization
  of absorbing gas\? THIS SUBMISSION CONTAINS THE CYCLE 2 OBSERVATIONS
  OF OJ287 and PG1718+481.

---------------------------------------------------------
Title: Quasar Absorption Line - for HOPR#0083
Authors: Bahcall, John
1991hst..prop.4799B    Altcode:
  The Quasar Absorption Line Survey of bright sources is an efficient
  observing program designed to provide a homogeneous data base of
  absorption features. The data will reveal absorption regions in
  galaxies, in clusters of galaxies, in voids, in large-scale structures,
  in Lyman ALPHA clouds, and will provide information about damped Lyman
  ALPHA and Lyman-limit systems. The survey will determine, with high SNR,
  the profiles of &gt; 200 emission lines. Using the estimated numbers
  of observed absorption lines, including archi val data, the program was
  designed to determine the cosmic evolution of absorption systems. High
  resolution spectra of a sample of quasars will be obtained with the FOS;
  the spectra will have a rest frame equivalent width detection limit for
  unresolved absorption lines of 0.3 A. The survey data base will address
  fundamental questions, for example: What is the strength and origin of
  the UV background radiation\? How do gaseous galactic disks and halos
  evolve with redshift\? What processes govern the ionization of absorbing
  gas\? How has gaseous structure in the universe evolved on scales of 1
  Mpc to 100 Mpc\? Do absorbing systems show evidence of the large-scale
  structure seen in the distribution of galaxies and clusters\?

---------------------------------------------------------
Title: Do Rich Clusters of Galaxies Produce Quasar Absorption Lines :
    Cycle 2
Authors: Bahcall, John
1991hst..prop.4117B    Altcode:
  Five quasars [NAB 0024+22, PKS 0003+15, UM 381, UM 324, and AO
  1058+11] that lie behind rich clusters of galaxies will be studied
  spectroscopically with the FOS to see if the clusters produce
  ultraviolet absorption lines. All of the quasar spectra will be used
  also to help determine the statistics of quasar absorption lines,
  the main goal of the GTO proposal "Evolution of Lyman-alpha and C IV
  Absorption Systems" (J. Bahcall, PI). ST observations are required in
  order to observe the ultraviolet absorption lines that may be produced
  by the nearby rich clusters of galaxies.

---------------------------------------------------------
Title: The Stellar Density Distributions in the Centers of Galactic
Globular Clusters: Cycle 2 Augmentation
Authors: Bahcall, John
1991hst..prop.3565B    Altcode:
  Short exposures will be made of all galactic globular clusters with
  distance moduli less than 15.5 mag and galactic latitude above or below
  15 degrees. A search will be made for cusps in the stellar density
  distributions and the colors will be measured for the brightest stars
  in the cores of the clusters. ST observations are required in order to
  reach the innermost regions of the clusters with sufficient resolution
  to separate individual stars.

---------------------------------------------------------
Title: Do Galaxies Produce Quasar Absorption Lines? : Cycle 2
Authors: Bahcall, John
1991hst..prop.4118B    Altcode:
  SPECTRA WILL BE OBTAINED WITH THE FOS FOR A NUMBER OF QUASARS THAT
  HAVE A SMALL ANGULAR SEPARATION ON THE SKY FROM GALAXIES OR GALAXY
  VOIDS, INCLUDING MARK 205, 3C 232, PKS 2020-370, THE GRAVITATIONALLY
  LENSED QUASAR, 2237+0305, 4 OBJECTS BEHIND THE BOOTES GALAXY VOID, US
  1329 (BEHIND THE BAHCALL-SONEIRA GALAXY VOID), AND 5C 03.44 (BEHIND M
  31). THE SPECTRA WILL BE USED TO TEST THE HYPOTHESIS THAT SOME METALLIC
  QUASAR ABSORPTION SYSTEMS ARE CAUSED BY VERY LARGE GALAXY HALOS OR
  DISKS. WF/PC IMAGES WILL ALSO BE OBTAINED OF THE LENSING GALAXY,
  2237+0305, IN ORDER TO LOCATE ACCURATELY THE QUASAR POSITION AND
  MEASURE THE SURFACE BRIGHTNESS OF THE INNER REGION OF THE GALAXY. ST
  OBSERVATIONS ARE REQUIRED BECAUSE, FOR THE SMALL REDSHIFTS AT WHICH
  GALAXIES WITH LARGE ANGULAR SIZE ARE FOUND, THE RESONANT ATOMIC LINES
  ARE IN THE ULTRAVIOLET.

---------------------------------------------------------
Title: Imaging and Spectroscopy of a Complete Sample of Bright Nearby
Quasars: II. Spectroscopy: Cycle 2 Baseline
Authors: Bahcall, John
1991hst..prop.3222B    Altcode:
  FOS spectra will be obtained for seven optically bright PG quasars
  [3C 273, PG 0953+415, PG 1116+215, PKS 1302-102, PG 1700+518, GQ Com,
  and 3C 249.1] with Mb &lt;/= -25.0 mag and z &lt;/= 0.35, as well as V
  &lt;/= 15.7 mag. The spectra will be analyzed for both absorption and
  emission features. ST observations are required because the spectral
  features of greatest interest in these small redshift objects are in
  the far ultraviolet, inaccessible from the ground.

---------------------------------------------------------
Title: Evolution of Lyman-Alpha and CIV Absorpton Systems: Cycle 2
Authors: Bahcall, John
1991hst..prop.4112B    Altcode:
  The evolution of Lyman-alpha and CIV absorption line systems in quasar
  spectra will be investigated using 21 optically bright quasars with
  a wide range of redshifts; the wavelength at which the Lyman cutoff
  appears will also be determined. All of the prominent emission and
  absorption lines will be measured. ST observations are required because
  the spectral features of interest are in the far ultraviolet and are
  inaccessible from the ground.

---------------------------------------------------------
Title: Quasar Absorption Line Survey: Cycle 2 Observations
Authors: Bahcall, John
1991hst..prop.3791B    Altcode:
  The Quasar Absorption Line Survey of bright sources is an efficient
  observing program designed to provide a homogeneous data base of
  absorption features. The data will reveal absorption regions in
  galaxies, in clusters of galaxies, in voids, in large-scale structures,
  in Lyman ALPHA clouds, and wi provide information about damped Lyman
  ALPHA and Lyman-limit systems. The survey will determine, with high SNR,
  the profiles of &gt; 200 emission lines. Using the estimated numbers
  of observed absorption lines, including archi val data, the program was
  designed to determine the cosmic evolution of absorption systems. High
  resolution spectra of a sample of quasars will be obtained with the FOS;
  the spectra will have a rest frame equivalent width detection limit for
  unresolved absorption lines of 0.3 A. The survey data base will address
  fundamental questions, for example: What is the strength and origin of
  the UV background radiation\? How do gaseous galactic disks and halos
  evolve with redshift\? What processes govern the ionization of absorbing
  gas\? How has gaseous structure in the universe evolved on scales of 1
  Mpc to 100 Mpc\? Do absorbing systems show evidence of the large-scale
  structure seen in the distribution of galaxies and clusters\?

---------------------------------------------------------
Title: Imaging and Spectroscopy of a Complete Sample of Bright Nearby
Quasars: II. Spectroscopy: Cycle 2
Authors: Bahcall, John
1991hst..prop.4115B    Altcode:
  FOS spectra will be obtained for seven optically bright PG quasars
  [3C 273, PG 0953+415, PG 1116+215, PKS 1302-102, PG 1700+518, GQ Com,
  and 3C 249.1] with Mb &lt;/= -25.0 mag and z &lt;/= 0.35, as well as V
  &lt;/= 15.7 mag. The spectra will be analyzed for both absorption and
  emission features. ST observations are required because the spectral
  features of greatest interest in these small redshift objects are in
  the far ultraviolet, inaccessible from the ground.

---------------------------------------------------------
Title: Do Galaxies Produce Quasar Absorption Lines: Cycle 2
    Augmentaion
Authors: Bahcall, John
1991hst..prop.3566B    Altcode:
  SPECTRA WILL BE OBTAINED WITH THE FOS FOR A NUMBER OF QUASARS THAT
  HAVE A SMALL ANGULAR SEPARATION ON THE SKY FROM GALAXIES OR GALAXY
  VOIDS, INCLUDING MARK 205, 3C 232, PKS 2020-370, THE GRAVITATIONALLY
  LENSED QUASAR, 2237+0305, 4 OBJECTS BEHIND THE BOOTES GALAXY VOID, US
  1329 (BEHIND THE BAHCALL-SONEIRA GALAXY VOID), AND 5C 03.44 (BEHIND M
  31). THE SPECTRA WILL BE USED TO TEST THE HYPOTHESIS THAT SOME METALLIC
  QUASAR ABSORPTION SYSTEMS ARE CAUSED BY VERY LARGE GALAXY HALOS OR
  DISKS. WF/PC IMAGES WILL ALSO BE OBTAINED OF THE LENSING GALAXY,
  2237+0305, IN ORDER TO LOCATE ACCURATELY THE QUASAR POSITION AND
  MEASURE THE SURFACE BRIGHTNESS OF THE INNER REGION OF THE GALAXY. ST
  OBSERVATIONS ARE REQUIRED BECAUSE, FOR THE SMALL REDSHIFTS AT WHICH
  GALAXIES WITH LARGE ANGULAR SIZE ARE FOUND, THE RESONANT ATOMIC LINES
  ARE IN THE ULTRAVIOLET.

---------------------------------------------------------
Title: Quasar Absorption Line Survey: Cycle 2 Observations
    Observations of 3C249-1
Authors: Bahcall, John
1991hst..prop.4939B    Altcode:
  THIS SUBMISSION is a change to P3791 to replace an object that
  it is not possible to acquirer with the Binary Search procedure
  with another object from our program. The object which has been
  removed is IR0450-2958. We are replacing it with 3C249-1 The Quasar
  Absorption Line Survey of bright sources is an efficient observing
  program designed to provide a homogeneous data base of absorption
  features. The data will reveal absorption regions in galaxies, in
  clusters of galaxies, in voids, in large-scale structures, in Lyman
  ALPHA clouds, and wi provide information about damped Lyman ALPHA
  and Lyman-limit systems. The survey will determine, with high SNR,
  the profiles of &gt; 200 emission lines. Using the estimated numbers
  of observed absorption lines, including archi val data, the program was
  designed to determine the cosmic evolution of absorption systems. High
  resolution spectra of a sample of quasars will be obtained with the
  FOS; the spectra will have a rest frame equivalent width detection
  limit for unresolved absorption lines of 0.3 A.

---------------------------------------------------------
Title: The Ultraviolet Absorption Spectrum of 3c 273
Authors: Bahcall, J. N.; Jannuzi, B. T.; Schneider, D. P.; Hartig,
   G. F.; Bohlin, R.; Junkkarinen, V.
1991BAAS...23R1270B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: U.S. Astronomy's Next Decade of Discovery
Authors: Bahcall, John N.
1991S&T....81..584B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The 1990s: The decade of discovery
Authors: Bahcall, John N.
1991PhT....44d..24B    Altcode:
  Recent achievements and development trends in astronomy and astrophysics
  are discussed. Ground- and space-equipment initiatives, recommended by
  the Astronomy and Astrophysics Survey Committee, are presented. Large
  programs including the Space Infrared Telescope Facility, the
  Infrared-Optimized 8-m Telescope, the Millimeter Array, Southern 8-m
  Telescope and other small and moderate programs are described. It
  is noted that theoretical research in such areas as plasma physics,
  atomic physics, nuclear physics, radiative transfer, properties of
  matter, which support analysis and interpretation of observation data
  should be developed. Establishment of national electronic archives,
  development of fast networks for linking most astronomical computers,
  and fundamental scientific research in lunar astronomy are also
  recommended. Some aspects of international collaboration are noted.

---------------------------------------------------------
Title: Comments on an historic event
Authors: Bahcall, John N.
1991NuPhS..19...94B    Altcode:
  Theoretical aspects of the solar neutrino problem are reviewed.

---------------------------------------------------------
Title: Solar-Cycle Modulation of Event Rates in the Chlorine Solar
    Neutrino Experiment
Authors: Bahcall, John N.; Press, William H.
1991ApJ...370..730B    Altcode:
  The time dependence of the event rates in the Homestake chlorine
  solar neutrino experiment are reexamined using new Ar-37 production
  data covering the period from late 1986 to mid-1989. The data span
  almost two complete solar cycles. A careful statistical analysis using
  nonparametric rank-order statistics is used to calculate quantitative
  significance levels that do not depend on experimental errors. The
  results show that the Ar-37 production rate in the experiment is
  anticorrelated with solar activity for approximately 1977-1989. The
  shape of the Ar-37 production rate is different from the inverted
  sunspot activity curve. The Ar-37 production rate is better descrbed by
  a skewed sawtooth function than by the sunspot number. The best-fitting
  sawtooth function with sunspot period has a slow rise and a rapid
  decline. The Ar-37 maximum occurs about 12.5 yr after the solar sunspot
  minimum, while minimum Ar-37 production is more nearly simultaneous
  with the sunspot maximum.

---------------------------------------------------------
Title: The Decade of Discovery
Authors: Bahcall, J. N.
1991BAAS...23Q.904B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Prioritizing Scientific Initiatives
Authors: Bahcall, John N.
1991Sci...251.1412B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Non-Proprietary Snapshot Survey - a Search for
    Gravitationally-Lensed Quasars Using the Hst/ Hubble Space Telescope
    Planetary Camera
Authors: Maoz, D.; Bahcall, J. N.; Doxsey, R.; Schneider, D. P.;
   Bahcall, N. A.; Lahav, O.; Yanny, B.
1991fyho.conf..200M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: K Giants and the amount of Local Dark Matter
Authors: Bahcall, J.; Flynn, C.; Gould, A.
1991dodg.conf..105B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Working papers. Astronomy and astrophysics panel reports.
Authors: Bahcall, John N.; Beichman, Charles A.; Canizares, Claude;
   Cronin, James; Heeschen, David; Houck, James; Hunten, Donald; McKee,
   Christopher F.; Noyes, Robert; Ostriker, Jeremiah P.
1991wpaa.book.....B    Altcode:
  This volume contains the working papers of the panels appointed by
  the Astronomy and Astrophysics Survey Committee. These papers were
  advisory to the survey committee and represent the opinions of the
  members of each panel in the context of their individual charges. The
  committee's full survey report is contained in a separately published
  document, The decade of discovery in astronomy and astrophysics
  (see 003.025). Contents: 1. Radio astronomy. 2. Infrared
  astronomy. 3. Optical/IR from ground. 4. UV-optical from
  space. 5. Interferometry. 6. High energy from space. 7. Particle
  astrophysics. 8. Theory and laboratory astrophysics. 9. Solar
  astronomy. 10. Planetary astronomy. 11. Computing and data
  processing. 12. Policy opportunities. 13. Benefits to the nation from
  astronomy and astrophysics. 14. Status of the profession. 15. Science
  opportunities.

---------------------------------------------------------
Title: IUE/HST Observations of 3C273k
Authors: Bahcall, John
1991iue..prop.4104B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: FOS Observations of the Absorption Spectrum of 3C273
Authors: Bahcall, J. N.; Jannuzi, B. T.; Schneider, D. P.; Hartig,
   G. F.; Bohlin, R.; Junkkarinen, V.
1991fyho.conf...46B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar neutrinos: new physics?
Authors: Bahcall, J. N.
1991NYASA.647...11B    Altcode: 1991tsra.symp...11B
  The author concentrates in this report on two theoretical arguments
  that suggest - independent of particular solar or particle physics
  models - that solar neutrino experiments reveal new physics beyond
  the standard electroweak model.

---------------------------------------------------------
Title: The HST Non-Proprietary SnapShot Survey
Authors: Maoz, D.; Bahcall, J. N.; Doxsey, R.; Schneider, D. P.;
   Bahcall, N. A.; Gunn, J. E.; Lahav, O.; Romani, R. W.; Yanny, B.
1991BAAS...23..832M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: New Measurement of Missing Matter in the Galactic Disk
Authors: Gould, A.; Bahcall, J. N.; Flynn, C.
1991BAAS...23..831G    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Non-Proprietary ("snapshot") Survey i Round 2
Authors: Bahcall, John
1990hst..prop.4027B    Altcode:
  Whenever the automatic scheduler produces a substantial gap between
  observations, the Wide Field/Planetary Camera will be used to
  image a nearby object selected from a list of several hundred low
  redshift quasars, normal galaxies, peculiar galaxies, and standard
  survey fields. HST observations will reveal details of the immediate
  environment of quasars, the nuclei of normal galaxies, the morphology of
  peculiar galaxies, and the star density in selected fields. The purpose
  of this program is to increase the efficiency of the HST and to provide
  scientific data that can be used by many different astronomers. The
  images acquired in this program will be non-proprietary and will be made
  available to qualified astronomers via the HST archival system. With
  the approval of the Director of STScI, the images can also be used
  for public relations purposes by appropriate NASA anad STScI personnel.

---------------------------------------------------------
Title: Gravitational Lens Candidate 1208+101: Photometry
Authors: Bahcall, John
1990hst..prop.3981B    Altcode:
  Planetary Camera images of the high-redshift quasar 1208+101 will
  be obtained with several broad band filters. These observations will
  determine whether the colors of the three unresolved sources located
  within a region 0.6" are the same; if so, then the objects are likely
  to be gravitationally lensed images of the quasar. Only HST can provide
  sufficient spatial resolution to provide accurate photometry on the
  individual images.

---------------------------------------------------------
Title: Quasar Absorption Line - for HOPR#0037
Authors: Bahcall, John
1990hst..prop.4044B    Altcode:
  The establishment of a homogeneous data base of quasar absorption
  lines using the diagnostic survey proposed here will form the basis
  for an attack on fundamental cosmological and astrophysical problems:
  What are the physical, dynamical and evolutionary properties of the
  intergalactic medium? What is the strength, shape and origin of the UV
  background radiation? What limits can be set upon the primordial He/H
  and D/H ratios? What has been the chemical and dynamical evolution of
  gaseous galactic disks and halos? What physical processes govern the
  ionization of this gas? What physical processes govern the acceleration
  of thermal and relativistic plasma in radio quiet and radio loud
  quasars? How has gaseous structure in the universe evolved on scales of
  1 Mpc to 100 Mpc? The discrimatory power of the survey and the efficient
  use of HST were the primary criteria used in constructing the survey,
  which takes account of all relevant GTO observations. Exposure times are
  based upon IUE archival data. Ground-based observations of all program
  objects will be made to monitor variability and to complement the HST
  observations. The survey contains a primary list of 103 quasars with
  0.3 &lt; Z_em &lt; 2.0, 18 additional bright quasars to be observed
  with the FOS to provide candidates for future HRS follow up, and
  a supplementary list of 49 fainter quasars for a damped Ly-alpha
  survey. A plausible extrapolation of ground-based data suggests that
  the primary survey will detect 275 Ly-alpha and 60 CIV systems.

---------------------------------------------------------
Title: Imaging and Spectroscopy of a Complete Sample of Bright Nearby
Quasars: II. Spectroscopy: Cycle 1 Observations
Authors: Bahcall, John
1990hst..prop.3220B    Altcode:
  FOS spectra will be obtained for seven optically bright PG quasars
  [3C 273, PG 0953+415, PG 1116+215, PKS 1302-102, PG 1700+518, GQ Com,
  and 3C 249.1] with Mb &lt;/= -25.0 mag and z &lt;/= 0.35, as well as V
  &lt;/= 15.7 mag. The spectra will be analyzed for both absorption and
  emission features. ST observations are required because the spectral
  features of greatest interest in these small redshift objects are in
  the far ultraviolet, inaccessible from the ground.

---------------------------------------------------------
Title: Gravitational Lens Candidate 1208+101: Spectroscopy
Authors: Bahcall, John
1990hst..prop.3992B    Altcode:
  We will obtain low resolution FOS spectra of the high-redshift quasar
  1208+101 and the brightest of two candidate gravitational lens images,
  located about .5 arcsec from the primary image. The 0.3 arcsec circular
  aperture will be used to spatially resolve the images, to test the
  gravitational lens hypothesis. Only HST can provide sufficient spatial
  resolution to permit sufficiently accurate spectrophotometry of the
  individual images.

---------------------------------------------------------
Title: Non-Proprietary ("snapshot") Survey Repeat Exposures of 3156
    3157 3158 3159
Authors: Bahcall, John
1990hst..prop.4017B    Altcode:
  Whenever the automatic scheduler produces a substantial gap between
  observations, the Wide Field/Planetary Camera will be used to
  image a nearby object selected from a list of several hundred low
  redshift quasars, normal galaxies, peculiar galaxies, and standard
  survey fields. HST observations will reveal details of the immediate
  environment of quasars, the nuclei of normal galaxies, the morphology of
  peculiar galaxies, and the star density in selected fields. The purpose
  of this program is to increase the efficiency of the HST and to provide
  scientific data that can be used by many different astronomers. The
  images acquired in this program will be non-proprietary and will be made
  available to qualified astronomers via the HST archival system. With
  the approval of the Director of STScI, the images can also be used
  for public relations purposes by appropriate NASA anad STScI personnel.

---------------------------------------------------------
Title: Quasar Absorption Line Survey: Cycle 1 Observations-Fos
Authors: Bahcall, John
1990hst..prop.2424B    Altcode:
  The establishment of a homogeneous data base of quasar absorption
  lines using the diagnostic survey proposed here will form the basis
  for an attack on fundamental cosmological and astrophysical problems:
  What are the physical, dynamical and evolutionary properties of the
  intergalactic medium? What is the strength, shape and origin of the UV
  background radiation? What limits can be set upon the primordial He/H
  and D/H ratios? What has been the chemical and dynamical evolution of
  gaseous galactic disks and halos? What physical processes govern the
  ionization of this gas? What physical processes govern the acceleration
  of thermal and relativistic plasma in radio quiet and radio loud
  quasars? How has gaseous structure in the universe evolved on scales of
  1 Mpc to 100 Mpc? The discrimatory power of the survey and the efficient
  use of HST were the primary criteria used in constructing the survey,
  which takes account of all relevant GTO observations. Exposure times are
  based upon IUE archival data. Ground-based observations of all program
  objects will be made to monitor variability and to complement the HST
  observations. The survey contains a primary list of 103 quasars with
  0.3 &lt; Z_em &lt; 2.0, 18 additional bright quasars to be observed
  with the FOS to provide candidates for future HRS follow up, and
  a supplementary list of 49 fainter quasars for a damped Ly-alpha
  survey. A plausible extrapolation of ground-based data suggests that
  the primary survey will detect 275 Ly-alpha and 60 CIV systems.

---------------------------------------------------------
Title: Evolution of Lyman-Alpha and CIV Absorpton Systems: Cycle
    1 Observations
Authors: Bahcall, John
1990hst..prop.3221B    Altcode:
  The evolution of Lyman-alpha and CIV absorption line systems in quasar
  spectra will be investigated using 21 optically bright quasars with
  a wide range of redshifts; the wavelength at which the Lyman cutoff
  appears will also be determined. All of the prominent emission and
  absorption lines will be measured. ST observations are required because
  the spectral features of interest are in the far ultraviolet and are
  inaccessible from the ground.

---------------------------------------------------------
Title: Quasar Absorption Line - for HOPR#0025
Authors: Bahcall, John
1990hst..prop.4000B    Altcode:
  The establishment of a homogeneous data base of quasar absorption
  lines using the diagnostic survey proposed here will form the basis
  for an attack on fundamental cosmological and astrophysical problems:
  What are the physical, dynamical and evolutionary properties of the
  intergalactic medium? What is the strength, shape and origin of the UV
  background radiation? What limits can be set upon the primordial He/H
  and D/H ratios? What has been the chemical and dynamical evolution of
  gaseous galactic disks and halos? What physical processes govern the
  ionization of this gas? What physical processes govern the acceleration
  of thermal and relativistic plasma in radio quiet and radio loud
  quasars? How has gaseous structure in the universe evolved on scales of
  1 Mpc to 100 Mpc? The discrimatory power of the survey and the efficient
  use of HST were the primary criteria used in constructing the survey,
  which takes account of all relevant GTO observations. Exposure times are
  based upon IUE archival data. Ground-based observations of all program
  objects will be made to monitor variability and to complement the HST
  observations. The survey contains a primary list of 103 quasars with
  0.3 &lt; Z_em &lt; 2.0, 18 additional bright quasars to be observed
  with the FOS to provide candidates for future HRS follow up, and
  a supplementary list of 49 fainter quasars for a damped Ly-alpha
  survey. A plausible extrapolation of ground-based data suggests that
  the primary survey will detect 275 Ly-alpha and 60 CIV systems.

---------------------------------------------------------
Title: Non-Proprietary ("snapshot") Survey II Round 2
Authors: Bahcall, John
1990hst..prop.4028B    Altcode:
  Whenever the automatic scheduler produces a substantial gap between
  observations, the Wide Field/Planetary Camera will be used to
  image a nearby object selected from a list of several hundred low
  redshift quasars, normal galaxies, peculiar galaxies, and standard
  survey fields. HST observations will reveal details of the immediate
  environment of quasars, the nuclei of normal galaxies, the morphology of
  peculiar galaxies, and the star density in selected fields. The purpose
  of this program is to increase the efficiency of the HST and to provide
  scientific data that can be used by many different astronomers. The
  images acquired in this program will be non-proprietary and will be made
  available to qualified astronomers via the HST archival system. With
  the approval of the Director of STScI, the images can also be used
  for public relations purposes by appropriate NASA anad STScI personnel.

---------------------------------------------------------
Title: The Stellar Density Distributions in the Centers of Galactic
Globular Clusters: Cycle 1 Observations
Authors: Bahcall, John
1990hst..prop.3227B    Altcode:
  Short exposures will be made of all galactic globular clusters with
  distance moduli less than 15.5 mag and galactic latitude above or below
  15 degrees. A search will be made for cusps in the stellar density
  distributions and the colors will be measured for the brightest stars
  in the cores of the clusters. ST observations are required in order to
  reach the innermost regions of the clusters with sufficient resolution
  to separate individual stars.

---------------------------------------------------------
Title: Quasar Absorption Line Survey: Cycle 1 FOS Part II
Authors: Bahcall, John
1990hst..prop.3418B    Altcode:
  The establishment of a homogeneous data base of quasar absorption
  lines using the diagnostic survey proposed here will form the basis
  for an attack on fundamental cosmological and astrophysical problems:
  What are the physical, dynamical and evolutionary properties of the
  intergalactic medium? What is the strength, shape and origin of the UV
  background radiation? What limits can be set upon the primordial He/H
  and D/H ratios? What has been the chemical and dynamical evolution of
  gaseous galactic disks and halos? What physical processes govern the
  ionization of this gas? What physical processes govern the acceleration
  of thermal and relativistic plasma in radio quiet and radio loud
  quasars? How has gaseous structure in the universe evolved on scales of
  1 Mpc to 100 Mpc? The discrimatory power of the survey and the efficient
  use of HST were the primary criteria used in constructing the survey,
  which takes account of all relevant GTO observations. Exposure times are
  based upon IUE archival data. Ground-based observations of all program
  objects will be made to monitor variability and to complement the HST
  observations. The survey contains a primary list of 103 quasars with
  0.3 &lt; Z_em &lt; 2.0, 18 additional bright quasars to be observed
  with the FOS to provide candidates for future HRS follow up, and
  a supplementary list of 49 fainter quasars for a damped Ly-alpha
  survey. A plausible extrapolation of ground-based data suggests that
  the primary survey will detect 275 Ly-alpha and 60 CIV systems.

---------------------------------------------------------
Title: Solution of the solar-neutrino problem
Authors: Bahcall, John N.; Bethe, H. A.
1990PhRvL..65.2233B    Altcode:
  Comparison of the results from the Kamiokande neutrino-electron
  scattering experiment with those from the chlorine experiment and with
  solar models shows that the explanation of the solar-neutrino problem
  probably requires physics beyond the standard electroweak model with
  zero neutrino masses. The experimental results, including the shape
  of the electron-recoil energy spectrum measured by Kamiokande,
  are in excellent agreement with a nonadiabatic solution of the
  Mikheyev-Smirnov-Wulfenstein effect, yielding a neutrino mass difference
  of Δm<SUP>2</SUP>=1×10<SUP>-8</SUP> sin<SUP>-2</SUP>Θ<SUB>V</SUB>
  eV<SUP>2</SUP>.

---------------------------------------------------------
Title: Book-Review - Neutrino Astrophysics
Authors: Bahcall, J. N.; Haubold, H. J.
1990AN....311R.421B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Neutrino Astrophysics
Authors: Bahcall, John N.; Wasserman, Ira
1990AmJPh..58..895B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Element Diffusion in Stellar Interiors
Authors: Bahcall, John N.; Loeb, Abraham
1990ApJ...360..267B    Altcode:
  Simple equations are derived that describe element diffusion in
  radiative stellar interiors and that may be incorporated in standard
  stellar evolution codes. For the sun, diffusion is expected to increase
  the predicted event rates in the Cl-37 solar neutrino experiment
  and in electron-neutrino scattering experiments by 5 - 10 percent;
  the expected increase in the predictions for Ga-71 solar neutrino
  experiments is between 1 and 3 percent.

---------------------------------------------------------
Title: Kinematic Modeling of the Galaxy. II. Two Samples of High
    Proper-Motion Stars
Authors: Casertano, Stefano; Ratnatunga, Kavan U.; Bahcall, John N.
1990ApJ...357..435C    Altcode:
  The paper analyzes two independent surveys, due to Fouts and Sandage and
  to Carney and Latham, of high proper motion stars with photoelectric
  photometry and line-of-sight velocity information. A purely kinematic
  study of both samples indicates that a two-component classical (disk +
  spheroid) model of the Galaxy is inadequate to represent the kinematics
  of stars in the solar neighborhood. A component with intermediate
  kinematic properties (old disk) is required. An asymmetric drift of
  50 + or - 15 km/s and principal velocity dispersions of (66, 37, 38)
  + or - 10 km/s are determined, in good agreement with the results of
  the metallicity-based analysis of Sandage and Fouts and of Carney and
  collaborators. The density of this component is poorly constrained,
  and is 10 percent + or - 5 percent of the local disk density for the
  same color range; the scale height is less than 1 kpc.

---------------------------------------------------------
Title: Das Rätsel der fehlenden Sonnenneutrinos.
Authors: Bahcall, J. N.
1990SpWis...8...76B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The solar-neutrino problem
Authors: Bahcall, John N.
1990SciAm.262e..54B    Altcode: 1990SciAm.262...54B
  Consideration is given to the discrepancies between the theory of
  solar neutrino emission and experimentally determined values for the
  solar neutrino flux. The results of the Homestake Gold Mine and the
  Kamiokande II experiments and the process of neutrino production in the
  standard solar model are reviewed. Possible reasons for the discrepancy
  between theory and observations are examined, including possible errors
  in the standard solar model, experimental error, and a lull in solar
  activity. Experiments concerning solar activity are discussed, including
  the Sudbury Neutrino Observatory and gallium neutrino detectors such
  as the Soviet-American Gallium Experiment and the Gallex program.

---------------------------------------------------------
Title: The solar-neutrino problem.
Authors: Bahcall, J. N.
1990SciAm.262e..26B    Altcode: 1990SciAm.262...26B
  Far fewer neutrinos from the sun are detected than current physics
  predicts. But a grand unification theory that ties together all natural
  forces permits neutrinos to change so they are not readily detected
  on the earth. New detectors are being designed to spot these "mutant"
  neutrinos - and confirm the theory.

---------------------------------------------------------
Title: Line versus continuum solar neutrinos
Authors: Bahcall, John N.
1990PhRvD..41.2964B    Altcode:
  The rate of neutrino line emission is calculated for nuclei that
  are usually assumed to produce only continuum neutrino emission. A
  convenient formula is derived that gives for solar interior conditions
  the ratio of the rates of neutrino line emission to continuum neutrino
  emission. The only significant line emission from the solar interior
  is expected from the pep and <SUP>7</SUP>electron capture reactions.

---------------------------------------------------------
Title: Book reviews
Authors: Bahcall, J. N.; Rosner, R.
1990SoPh..127..209B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book-Review - Neutrinos
Authors: Klapdor, H. V.; Bahcall, J. N.
1990SoPh..127..209K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: What the Longest Exposures from the Hubble Space Telescope
    Will Reveal
Authors: Bahcall, John N.; Guhathakurta, Puragra; Schneider, Donald P.
1990Sci...248..178B    Altcode:
  Detailed simulations are presented of the longest exposures on
  representative fields that will be obtained with the Hubble Space
  Telescope, as well as predictions for the numbers and types of objects
  that will be recorded with exposures of different durations. The Hubble
  Space Telescope will reveal the shapes, sizes, and content of faint,
  distant galaxies and could discover a new population of Galactic stars.

---------------------------------------------------------
Title: Neutrinos from the sun - an astronomical puzzle
Authors: Bahcall, John N.
1990Mercu..19...53B    Altcode:
  The current situation concerning neutrinos from the sun is
  summarized. The discussion presents a definition of neutrinos,
  an introduction to the science of neutrino astronomy, and the
  implications of these findings. It is noted that neutrinos from the
  sun and from supernovae provide cosmic particle beams for probing
  the weak interactions of particles with energies and on time scales
  that cannot be achieved with traditional laboratory experiments. The
  solar neutrino unit, or SNU, is defined and the model that provides a
  combined description of electrical and weak interaction phenomena is
  detailed. The solar neutrino problem is explained and the importance
  of neutrino experiments and the theory of stellar evolution is
  emphasized. Nuclear energy generation and neutrino fluxes, the Cl-37
  experiment, the Kamiokande II experiment, and gallium detectors and
  their contribution to understanding the solar neutrino problem are
  discussed.

---------------------------------------------------------
Title: Where are the solar neutrinos?
Authors: Bahcall, J. N.
1990Ast....18c..40B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Mixing and the Solar Neutrino Problem
Authors: Sienkiewicz, R.; Bahcall, J. N.; Paczynski, B.
1990ApJ...349..641S    Altcode:
  Evolutionary sequences for the sun were calculated assuming continuous
  or episodic mixing of matter in the solar interior. The ad hoc mixing
  affects solar neutrino emission because it increases the interior H-1
  and He-3 content and reduces the temperature at the solar center. For
  a typical postulated massive mixing 'event', the flux of the basic pp
  neutrinos is strongly reduced for about 10 million yr following the
  mixing, and the B-8 neutrino is greatly decreased for more than 10 to
  the 8th yr. The flux of hep neutrinos is significantly increased for
  about 100,000 yr. The neutrino fluxes calculated from the standard
  (unmixed) solar model obtained here with an independent numerical
  code agree with the neutrino fluxes of Bahcall and Ulrich (1988)
  to an accuracy of a few percent or better.

---------------------------------------------------------
Title: The solar neutrino mystery.
Authors: Bahcall, J. N.
1990AsNow...4...15B    Altcode: 1990AstNw...4...15B
  When the first attempts were made to test our ideas and understanding
  of how the Sun shines, scientists were unexpectedly confronted with
  the case of the missing neutrinos. This mystery has stimulated and
  confounded scientists since 1968, but may soon be solved. Critical
  experiments will soon be performed and a clear understanding of the
  neutrino problem will hopefully follow.

---------------------------------------------------------
Title: Book-Review - Neutrino Astrophysics
Authors: Bahcall, J. N.
1990AstQ....7..189B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Standard Solar Model
Authors: Bahcall, John N.; Cribier, M.
1990ASSL..159...21B    Altcode: 1990IAUCo.121...21B; 1990insu.conf...21B
  No abstract at ADS

---------------------------------------------------------
Title: Book-Review - Neutrino Astrophysics
Authors: Bahcall, J. N.
1989Sci...246.1648B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Neutrino Astrophysics
Authors: Bahcall, John N.
1989neas.book.....B    Altcode: 1989QB464.2.B34....
  List of tables; List of figures; Preface; 1. Overview; 2. Stellar
  structure and evolution; 3. Nuclear fusion reactions; 4. The
  standard solar model; 5. Nonstandard solar models; 6. The neutrinos;
  7. Theoretical uncertainties; 8. Neutrino cross sections; 9. Beyond the
  standard model of electroweak interactions; 10. The 37CI experiment;
  11. The 71Ga experiments; 12. Geochemical and radiochemical detectors:
  Mo, Tl, Li, Br, I; 13. Neutrino-electron scattering experiments;
  14. Direct counting experiments; 15. Stellar collapse; 16. Synopsis
  and future directions; Appendix; References; Index.

---------------------------------------------------------
Title: Matter-enhanced neutrino oscillations in the standard solar
    model
Authors: Bahcall, J. N.; Haxton, W. C.
1989PhRvD..40..931B    Altcode:
  The effects of matter-enhanced neutrino oscillations on solar-neutrino
  experiments can be calculated accurately only if uncertainties in
  the standard solar model are treated properly. As the oscillation
  probability depends on the neutrino energy, while modifications in the
  parameters of the standard solar model produce correlated changes in
  the various solar-neutrino sources, Monte Carlo calculations appear
  to offer the only means for addressing this problem. We consider the
  effects of matter-enhanced neutrino oscillations for 1000 standard solar
  models that were constructed by varying the solar input parameters
  according to their estimated probability distributions. From these
  Monte Carlo calculations [carried out for a neutrino parameter
  grid of 10<SUP>4</SUP> cases corresponding to 3×10<SUP>8</SUP>
  separate Mikheyev-Smirnov-Wolfenstein (MSW) calculations] we derive
  95%-C.L. limits on the neutrino mass difference δm<SUP>2</SUP>
  and mixing angle sin<SUP>2</SUP>2θ for possible outcomes for the
  <SUP>37</SUP>Cl, <SUP>71</SUP>Ga, and Kamioka II experiments and the
  assumption of two-flavor oscillations. We find that <SUP>71</SUP>Ga
  counting rates as large as 128 solar-neutrino units (SNU) or as
  small as 4 SNU are not ruled out by present 95%-C.L. results from
  the <SUP>37</SUP>Cl and Kamioka II experiments, given possible solar
  and nuclear cross-section uncertainties. Considering all three of
  the experiments, <SUP>37</SUP>Cl (existing results), Kamioka II
  (existing results), and <SUP>71</SUP>Ga (hypothesized results), we
  find the allowed neutrino parameters form two distinct “islands”
  in the δm<SUP>2</SUP>-sin<SUP>2</SUP>2θ plane for <SUP>71</SUP>Ga
  results between 20 and 100 SNU, even with our restrictive assumption of
  oscillations between only two flavors. Thus additional experiments may
  be required to distinguish between solutions that are each consistent
  with the results from the <SUP>37</SUP>Cl, <SUP>71</SUP>Ga, and Kamioka
  II experiments. We explore the implications of future Kamioka II results
  of improved accuracy. To permit analyses of new experiments that focus
  on individual fluxes, we also present separate predictions of the MSW
  effect for <SUP>7</SUP>Be and <SUP>3</SUP>+p (hep) neutrinos.

---------------------------------------------------------
Title: Book-Review - Neutrino Astrophysics
Authors: Bahcall, J. N.; Cherry, M. L.
1989Natur.340..520B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: How does the Sun shine?
Authors: Bahcall, John
1989Natur.340..265B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Sharing astronomical costs
Authors: Bahcall, John N.
1989Natur.339..574B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Magnitude of 3He Diffusion in the Sun
Authors: Loeb, A.; Bahcall, J. N.; Milgrom, M.
1989ApJ...341.1108L    Altcode:
  The diffusion of He-3(2+) has been determined in the four-component
  solar plasma. It is found that the fractional diffusive changes in
  the solar lifetime are bounded by (-2, +5) percent of the standard
  solar model values for the He-3 abundance. These changes are shown
  to be negligible in the solar core due to the large rate of the
  destruction of diffused ions by the (He-3)-(He-3) and (He-3)-(He-4)
  reactions occurring there.

---------------------------------------------------------
Title: Kinematic Modeling of the Galaxy. I. The Yale Bright Star
    Catalogue
Authors: Ratnatunga, Kavan U.; Bahcall, John N.; Casertano, Stefano
1989ApJ...339..106R    Altcode:
  A code has been developed to investigate the kinematic properties
  of stellar populations of the Galaxy by modeling the distributions
  of proper motion and line-of-sight velocity. The coordinate frames of
  reference are discussed in detail and the general matrix transformations
  valid beyond the solar neighborhood are given. As a first application,
  the kinematic properties of the magnitude-selected sample of 3993
  stars in the Bright Star Catalogue with V less than 6.0 and (B-V)
  greater than 0 are selected. The observed kinematic distributions
  are compared with a conventional model that has an exponential disk
  with scale heights, components of velocity dispersion ellipsoid, and
  asymmetric drift taken from the literature and defined as functions
  of spectral type. The comparisons suggest that a significant fraction
  of the Bright Star Catalogue belongs to a relatively young population
  that is not properly represented in the model.

---------------------------------------------------------
Title: Solar Neutrinos: Waiting for Kamiokande II
Authors: Bahcall, J. N.
1989bbag.conf..399B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Supernova 1987A.
Authors: Arnett, W. David; Bahcall, John N.; Kirshner, Robert P.;
   Woosley, Stanford E.
1989ARA&A..27..629A    Altcode:
  The circumstances of SN 1987A are nearly ideal for studying supernovae
  and we have a relatively complete observational record. The Large
  Magellanic Cloud is fortuitously well placed in the sky, circumpolar
  for recently constructed southern observatories and near the ecliptic
  pole. These practical advantages, a rich and varied set of observations
  can be used to test a well-developed, but hitherto poorly calibrated,
  theory for supernova explosions. This review cannot explore every
  aspect of SN 1987A. The authors have tried to emphasize the main event:
  the test of stellar evolution represented by the observations.

---------------------------------------------------------
Title: De Vaucouleurs's Galaxy.
Authors: Bahcall, John N.
1989woga.conf..188B    Altcode:
  Gérard de Vaucouleurs proposed the standard geometrical descriptions
  of both the disk and spheroid populations of spiral galaxies, and
  applied this description in a pioneering model of the Galaxy. This
  talk describes the results of computer modeling of the Galaxy using
  the de Vaucouleurs distributions for the disk and spheroid.

---------------------------------------------------------
Title: A Survey of G and K Giants at the South Galactic Pole
Authors: Flynn, C.; Bahcall, J.; Freeman, K. C.
1989gfpg.conf..105F    Altcode: 1989LDP....12..105F
  No abstract at ADS

---------------------------------------------------------
Title: Solar flares and neutrino detectors
Authors: Bahcall, John N.
1988PhRvL..61.2650B    Altcode:
  Solar flares have been suggested as the cause of occasional high
  counting rates in the <SUP>37</SUP>Cl solar-neutrino experiment. The
  sensitivity of neutrino detectors to flares is evaluated. Several
  neutrino detectors will show large signals when prominent flares are
  observed electromagnetically, if flares are detected in the chlorine
  experiment.

---------------------------------------------------------
Title: What will the <SUP>98</SUP>Mo solar-neutrino experiment
    measure\?
Authors: Bahcall, John N.
1988PhRvD..38.2006B    Altcode:
  It is shown that the geochemical measurement of the solar-neutrino flux
  using <SUP>98</SUP>Mo should yield the same value for the <SUP>8</SUP>B
  neutrino flux as is determined by contemporary observations using the
  <SUP>37</SUP>Cl and Kamiokande II detectors. The <SUP>98</SUP>Mo and
  contemporary fluxes should be equal to an accuracy of better than 1%,
  provided standard ideas regarding time scales in stellar evolution
  are correct.

---------------------------------------------------------
Title: Solar neutrinos: a field in transition
Authors: Bahcall, John N.; Davis, Raymond, Jr.; Wolfenstein, Lincoln
1988Natur.334..487B    Altcode:
  Solar-neutrino experiments provide a unique opportunity for studying
  weak interactions in a realm where new physics may be revealed. At
  the same time the neutrinos carry important information about the
  physical processes occurring in the otherwise inaccessible core
  of a main-sequence star. A variety of experiments, electronic and
  radiochemical, must be carried out to determine what new physics and
  astronomy are being uncovered with these underground detectors.

---------------------------------------------------------
Title: Neutral-current reactions of solar and supernova neutrinos
    on deuterium
Authors: Bahcall, J. N.; Kubodera, K.; Nozawa, S.
1988PhRvD..38.1030B    Altcode:
  We calculate the cross sections for the neutral-current disintegration
  of deuterium by neutrinos and antineutrinos: ν+d--&gt;ν'+n+p
  and ν¯+d--&gt;ν¯'+n+p. We put special emphasis on estimates
  of the theoretical uncertainties of these cross sections. For
  <SUP>8</SUP>B and hep solar neutrinos, the averaged cross sections are
  &lt;σ(<SUP>8</SUP>B)&gt;=4.1(1+/-0.1)×10<SUP>-43</SUP> cm<SUP>2</SUP>
  and &lt;σ(hep)&gt;=1.15(1+/-0.1)×10<SUP>-42</SUP> cm<SUP>2</SUP>,
  respectively, where hep denotes <SUP>3</SUP>He+p. The cross-section
  uncertainty is negligible, +/-1/2%, for the ratio of neutral-current
  to charged-current events. Independent of neutrino oscillations,
  the cross sections correspond to 4.5(1+/-0.38)×10<SUP>3</SUP>
  solar-neutrino events per year in the proposed one-kiloton Sudbury
  Neutrino Observatory if the standard solar model is correct. For
  a galactic supernova, the total number of neutral-current events
  expected in the Sudbury detector is about 10<SUP>3</SUP> (distance/8
  kpc)<SUP>-2</SUP>; most of the signal is expected to arise from μ
  and τ neutrinos and antineutrinos. If either μ or τ neutrinos have
  a mass greater than 2×10<SUP>2</SUP> eV, then this mass should be
  measurable using the neutrino signal from a galactic supernova.

---------------------------------------------------------
Title: Supernovae leave their mark
Authors: Bahcall, John N.
1988Natur.333..301B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar models, neutrino experiments, and helioseismology
Authors: Bahcall, John N.; Ulrich, Roger K.
1988RvMP...60..297B    Altcode:
  The event rates and their recognized uncertainties are calculated for
  eleven solar neutrino experiments using accurate solar models. The
  same solar models are used to evaluate the frequency spectrum of the
  p and g oscillation modes of the sun and to compare with existing
  observations. A numerical table of the characteristics of the standard
  solar model is presented. Improved values have been calculated for all
  of the neutrino absorption cross sections evaluating the uncertainties
  for each neutrino source and detector as well as the best estimates. The
  neutrino capture rate calculated from the standard solar model for
  the <SUP>37</SUP>Cl experiment is 7.9(1+/-0.33) SNU, which spans the
  total theoretical range; the rate observed by Davis and his associates
  is (2.0+/-0.3) SNU. The ratio of the observed to the predicted
  flux at Earth of neutrinos from <SUP>8</SUP>B decay lies in the range
  0&lt;=[ϕ(<SUP>8</SUP>B)<SUB>observed</SUB>ϕ(<SUP>8</SUP>B)<SUB>predicted</SUB>]&lt;=0.5.
  The recent results from the Kamiokande II electron scattering experiment
  confirm this conclusion. This discrepancy between calculation
  and observation is the solar neutrino problem. Measurements of the
  energy spectrum of solar neutrinos can discriminate between suggested
  solutions of the solar neutrino problem. Nonstandard solar models,
  many examples of which are also calculated in this paper, preserve the
  shape of the energy spectrum from individual neutrino sources, whereas
  most proposed weak-interaction explanations imply altered neutrino
  energy spectra. Detailed energy spectra of individual neutrino sources
  are presented as well as a composite solar neutrino spectrum. hep
  neutrinos from the <SUP>3</SUP>He+p reaction, probe a different region
  of the solar interior than do <SUP>8</SUP>B neutrinos. Measurements
  of the very rare but highest-energy hep neutrinos are possible
  in proposed experiments using electron scattering, <SUP>2</SUP>H,
  and <SUP>40</SUP>Ar detectors. The standard solar model predicts
  p-mode oscillation frequencies that agree to within about 0.5% with
  the measured frequencies and reproduce well the overall dispersion
  relation of the modes. However, there are several small but significant
  discrepancies between the measured and observed frequencies. The
  complementarity of helioseismology and solar neutrino experiments
  is demonstrated by constructing a solar model with a drastically
  altered nuclear energy generation that eliminates entirely the
  important high-energy <SUP>8</SUP>B and <SUP>7</SUP>Be neutrinos,
  but which affects by less than 0.01% the calculated p-mode oscillation
  frequencies.

---------------------------------------------------------
Title: Book-Review - the Galaxy and the Solar System
Authors: Smoluchowski, R.; Bahcall, J. N.; Matthews, M. S.; Hilditch,
   R.
1988Obs...108...23S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The mass of the electron neutrino: Monte Carlo studies of SN
    1987A observations
Authors: Spergel, David N.; Bahcall, John N.
1988PhLB..200..366S    Altcode:
  Monte Carlo simulations of a wide class of possible neutrino emission
  models are used to assign statistical significance to the limits set
  on the mass of the electron neutrino by observations of SN 1987A. Using
  the combined Kamiokande II and IMB data sets, we reject neutrino masses
  greater than 16 eV at the 5% significance level.

---------------------------------------------------------
Title: Simulations of HST observations of globular clusters.
Authors: Bahcall, John N.; Schneider, Donald P.
1988IAUS..126..455B    Altcode:
  Simulations of Hubble Space Telescope observations to study galactic
  globular clusters are examined. Studies of the cores of nearby
  globular clusters to determine the stellar density distributions and
  luminosity functions in the innermost regions of the clusters are
  presented. Pictures of M 13 are included to demonstrate the usefulness
  of these studies. Stellar population studies of a relatively unobscured
  globular cluster to detect white dwarfs and the faint red end of the
  cluster luminosity function are discussed and illustrated with pictures
  of NGC 6397.

---------------------------------------------------------
Title: Phenomenological analysis of neutrino emission from SN 1987A.
Authors: Bahcall, J. N.; Spergel, D. N.; Press, W. H.
1988slmc.proc..172B    Altcode:
  The allowed range of the nu(e) emission temperature, rise time, cooling
  time, flux, and total energy of the neutrino emission from SN 1987A
  are determined from Monte Carlo and maximum likelihood analyses. The
  acceptable ranges are found to be 4.2 + 1.2, - 0.8 MeV for temperature,
  4.5 + 1.7, - 2.0 sec for cooling time, and 6.1 + 3.5, - 3.6 x 10 to
  the 52nd N(all) erg for total emitted energy, where N(all) is the
  ratio of energy emitted in all neutrino forms to that emitted in the
  form of nu(e). It is suggested that masses of nu(e) that exceed 16 eV
  at the 5 percent significance level can be rejected.

---------------------------------------------------------
Title: Neutrinos and sunspots
Authors: Bahcall, J. N.
1987Natur.330..318B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Is Solar Neutrino Capture Rate Correlated with Sunspot Number?
Authors: Bahcall, J. N.; Field, G. B.; Press, W. H.
1987ApJ...320L..69B    Altcode:
  The statistical significance of the apparent correlation between
  sunspots and the observed neutrino rate is quantified. It is shown that
  the correlation depends almost entirely upon four low neutrino capture
  rates near the beginning of 1980. A calculation based on standard
  electroweak theory and neutrino production processes demonstrates that
  a correlation, if real, would be extremely puzzling on energetic grounds
  alone. It is concluded that measurements with the Cl-37 detector during
  the next sunspot cycle will be needed to show that there is a physical
  correlation, since the existing data are not statistically significant
  at a definitive level.

---------------------------------------------------------
Title: An Analysis of the Yale Bright Star Catalog
Authors: Bahcall, John N.; Casertano, Stefano; Ratnatunga, Kavan U.
1987ApJ...320..515B    Altcode:
  The authors analyze the direction, color, and apparent-magnitude
  distributions of a complete sample of 3993 stars with m<SUB>v</SUB>≤
  6.0 mag and B-V ≥ 0.0 from the Yale Bright Star Catalog (BSC). Many
  of the sample stars are intrinsically bright disk giants. The total
  number and overall distributions of the BSC stars (excluding O and B
  stars) are well described by the standard Galaxy model with two major
  density components. The spatial distribution of O and B stars shows a
  density enhancement due to the Gould Belt in a 15° region inclined
  about 20°±3° to the Galactic plane. The total number of O and B
  stars in the Galaxy is estimated to be ≡10<SUP>7</SUP>.

---------------------------------------------------------
Title: A Simple Model for Neutrino Cooling of the Large Magellanic
    Cloud Supernova
Authors: Spergel, D. N.; Piran, T.; Loeb, A.; Goodman, J.; Bahcall,
   J. N.
1987Sci...237.1471S    Altcode:
  A simplified analytic model of a cooling hot neutron star, motivated
  by detailed computer calculations, describes well the neutrinos
  detected from the recent supernova in the Large Magellanic Cloud. The
  observations do not require explanations that invoke exotic physics
  or complicated astrophysics. The parameters in this simple model
  are not severely constrained: 6.1<SUB>-3.6</SUB><SUP>+3.5</SUP>
  × 10<SUP>52</SUP> ergs emitted in electron antineutrinos, a peak
  temperature of 4.2<SUB>-0.8</SUB><SUP>+1.2</SUP> megaelectron volts,
  a radius of 27<SUB>-15</SUB><SUP>+17</SUP> kilometers, and a cooling
  time of 4.5<SUB>-2.0</SUB><SUP>+1.7</SUP> seconds.

---------------------------------------------------------
Title: Book-Review - the Galaxy and the Solar System
Authors: Smoluchowski, R.; Bahcall, J. N.; Matthews, M. S.
1987Sci...237...89S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Neutrino temperatures and fluxes from the LMC supernova
Authors: Bahcall, J. N.; Piran, T.; Press, W. H.; Spergel, D. N.
1987Natur.327..682B    Altcode: 1987Nat...327..682B
  The observation<SUP>1,2 </SUP>of neutrinos from the LMC supernova
  makes possible direct tests of the theory of supernova explosions
  and of properties of weakly interacting particles. Here we describe a
  combined analysis of the angular and energy distributions of the events
  observed in the Kamiokande and the 1MB detectors which determines the
  effective temperatures and fluxes of neutrinos and anti-neutrinos*
  produced by the explosion. Our main result is that a simple model is
  consistent with the available data and in reasonable agreement with
  conventional models of supernova explosions. The parameters of the model
  are: a single temperature, T, of 4.1<SUP>+1.0</SUP> <SUB>-0.4</SUB>
  MeV, a flux of electron anti-neutrinos of (O.5<SUB>-0.35</SUB>
  <SUP>+0.2</SUP>)×10<SUP>10</SUP>cm<SUP>-2</SUP> [total energy
  in \vmacr<SUB>e</SUB> = (3.0<SUP>+1.7</SUP> <SUB>-1.4</SUB> ×
  10<SUP>52</SUP> erg)], and a poorly determined flux of 'scattered' (see
  below) neutrinos = (0.2-5)× 10<SUP>10</SUP> cm<SUP>-2</SUP>. Several
  statistical tests were used to determine the acceptable range of
  these parameters. We have also set limits on possible high-temperature
  fluxes of neutrinos or anti-neutrinos that might result from matter
  oscillations<SUP>3,4</SUP>

---------------------------------------------------------
Title: Dust Distribution in Spiral Galaxies
Authors: Kylafis, Nikolaos D.; Bahcall, John N.
1987ApJ...317..637K    Altcode:
  A method for determining the dust distribution in edge-on, late Hubble
  type, spiral galaxies from their surface photometry is described. The
  method assumes that both the stars and the dust are distributed
  isothermally in the direction perpendicular to the galactic plane with
  scale heights z(s) and z(d) respectively, and exponentially in the
  radial direction with corresponding scale lengths h(s) and h(d). By
  comparing the observed surface photometry and the model calculations
  in which the radiative transfer is treated properly, z(s), z(d), h(s),
  and h(d) can be determined, as well as the optical depth along the line
  of sight and the central brightness. As a demonstration, the method is
  applied to NGC 891. The extension of the method to early-type spiral
  galaxies and to inclination angles less than 90 deg is described.

---------------------------------------------------------
Title: Book-Review - the Galaxy and the Solar System
Authors: Smoluchowski, R.; Bahcall, J. N.; Matthews, M. S.
1987S&T....73Q.624S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book-Review - the Galaxy and the Solar System
Authors: Smoluchowski, R.; Bahcall, J. N.; Matthews, M. S.; Bailey,
   M. E.
1987Sci...236..619S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Mikheyev-Smirnov-Wolfenstein effect in electron-neutrino
    scattering experiments
Authors: Bahcall, J. N.; Gelb, J. M.; Rosen, S. P.
1987PhRvD..35.2976B    Altcode:
  We calculate the influence of resonant neutrino scattering
  [the Mikheyev-Smirnov-Wolfenstein (MSW) effect] in the Sun and
  in the Earth on measurable quantities in solar-neutrino-electron
  scattering experiments. The MSW effect reduces the expected rate for
  <SUP>8</SUP>electron scattering by a factor that ranges from ~0.8
  to ~0.2 if resonant scattering is the correct explanation for the
  discrepancy between observation and calculation in the <SUP>37</SUP>Cl
  experiment. The Earth can produce a significant diurnal effect for
  certain values of the neutrino mixing angle and mass difference.

---------------------------------------------------------
Title: Upper limit on the mass of the electron neutrino
Authors: Bahcall, J. N.; Glashow, S. L.
1987Natur.326..476B    Altcode:
  The historic detection by the Kamiokande-II collaboration<SUP>1</SUP>
  and the IMB collaboration<SUP>2</SUP> of neutrinos from the Large
  Magellanic Cloud (LMC) supernova provides the first opportunity to
  determine the mass, m<SUB>v<SUB>c</SUB></SUB>, of the electron
  neutrino from astronomical observations. Here we show that
  m<SUB>v<SUB>c</SUB></SUB>, is less than 11 eV, provided only that
  propagation effects have not conspired to sharpen, by more than a
  factor of two the narrow pulse-width of neutrinos, observed by the
  Kamiokande-II collaboration from the LMC supernova. This result improves
  on the laboratory limit on m<SUB>v<SUB>c</SUB></SUB> and confirms the
  view that electron neutrinos do not constitute the major component of
  the matter density of the Universe.

---------------------------------------------------------
Title: Neutrino-electron scattering and solar neutrino experiments
Authors: Bahcall, John N.
1987RvMP...59..505B    Altcode:
  Neutrino-electron scattering experiments can elucidate the flavor
  content, spectrum shape, intensity, time dependence, and angular
  distribution of solar neutrinos. The author presents detailed
  calculations for all of the important solar neutrino sources of the
  predicted energy and angular dependence of the recoil electrons, as
  well as the total cross sections. In addition, the author discusses
  how neutrino-electron experiments can help distinguish between various
  proposed solutions of the solar neutrino problem.

---------------------------------------------------------
Title: Neutrinos from the recent LMC supernova
Authors: Bahcall, J. N.; Dar, A.; Piran, T.
1987Natur.326..135B    Altcode: 1987Nat...326..135B
  No abstract at ADS

---------------------------------------------------------
Title: Supernova 1987A in the Large Magellanic Cloud
Authors: West, R. M.; Madsen, C.; Bahcall, J.; Dar, A.; Piran, T.;
   Murdin, P.; Beresford, T.
1987IAUC.4329....2W    Altcode: 1987IAUC.4329....1W; 1987IAUC.4329....0W
  R. M. West, European Southern Observatory, informs us that a color
  exposure (Agfachrome 1000 RS, Hasselblad 6 x 6) of the LMC was made by
  C. Madsen at La Silla during Feb. 23.042-23.056 UT. Sanduleak -69 202 is
  just seen near the limiting magnitude of about 12. J. Bahcall, A. Dar
  and T. Piran, Institute for Advanced Study, Princeton, communicate
  the following note, prepared in advance of the report of the neutrino
  detection on IAUC 4323: "We have calculated the event rate expected in
  terrestrial neutrino detectors from neutrinos produced in the formation
  of the neutron star in the LMC supernova. Using neutrino fluxes from a
  model stellar collapse calculation of Wilson et al. and cross sections
  from Bahcall, we estimate that only about one atom of Ar is produced in
  the Davis Cl tank, but that about 50 electron recoils, with energies of
  about 10 MeV, are produced in the Kamiokande II water detector. We also
  estimate about 3 events each in the scintillators of the University of
  Pennsylvania (Homestake Mine) and the Italian- Russian collaboration
  (Mont Blanc). The results are sensitive to the effective temperature of
  the emitted neutrino spectrum." P. Murdin, Royal Greenwich Observatory,
  reports: "It is not clear whether the relative constancy of the light
  curve of SN 1987A from Feb. 25 to Mar. 3 represents the maximum in a
  typical type II light curve or the 20 day premaximum halt seen in SN
  1940B and 1941A. If SN 1987A follows precedent, either it will decline
  soon to mag 6, where it will remain in the post-maximum plateau until
  early May, or it will brighten in mid-March to a maximum at mag about
  2, remaining brighter than mag 6 until early July. Observers should be
  aware of this uncertainty when planning observations." Visual magnitude
  estimate by T. Beresford, Adelaide, South Australia: Mar. 3.42 UT, 4.3.

---------------------------------------------------------
Title: Kinematic Model of Our Galaxy
Authors: Ratnatunga, K. U.; Bahcall, J. N.; Casertano, S.
1987BAAS...19..679R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Dark Matter in the Galactic Disk
Authors: Bahcall, John N.
1987IAUS..117...17B    Altcode:
  Observational data on the distributions of tracer stars, F dwarfs
  and K giants were used as input to obtain self-consistent solutions
  for the Poisson and Vlasov equations to set bounds on the amount of
  missing matter in the solar neighborhood. The numerical computations
  were carried out using Galaxy models which feature multiple disk
  components and an unseen massive halo. The star data included the
  mass components and velocity dispersions. Consideration of various
  possible distributions of the unseen matter leads to the conjecture
  that half of the disk material in the solar neighborhood has yet to be
  observed. Techniques for determining if brown dwarfs are a significant
  component of the missing mass are discussed, as are improved models
  which would use limited numbers of tracer stars to set further
  constraints on the amount and distribution of the missing mass.

---------------------------------------------------------
Title: Estimating the Masses of Galaxy Groups - Alternatives to the
    Virial Theorem
Authors: Heisler, J.; Tremaine, S.; Bahcall, J.
1987IAUS..117..113H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Some Possible Regularities in Missing Mass
Authors: Bahcall, John N.; Casertano, Stefano
1987dmu..conf...50B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Dark matter in the universe. Proceedings of the Fourth
    Jerusalem Winter School for Theoretical Physics, held at Jerusalem,
    Israel, 30 December 1986 - 8 January 1987.
Authors: Bahcall, J.; Piran, T.; Weinberg, S.
1987dmup.book.....B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Dark Matter Near the Sun
Authors: Bahcall, John N.
1987dmu..conf....2B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: K-Giants and the Total Amount of Matter Near the Sun
Authors: Bahcall, John N.
1987dmu..conf...13B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: K-giants and the total amount of matter near the Sun.
Authors: Bahcall, J. N.
1987IAUS..117...13B    Altcode:
  Reprint of paper 38.155.084.

---------------------------------------------------------
Title: Dark matter in the universe
Authors: Bahcall, John N.; Piran, T.; Weinberg, S.
1987dmu..conf.....B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solutions to the solar neutrino problem?
Authors: Bahcall, J.
1987PhT....40a..11B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Dark Matter in the Solar Vicinity
Authors: Bahcall, John N.
1987dmu..conf....1B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Dark matter near the Sun.
Authors: Bahcall, J. N.
1987IAUS..117....2B    Altcode:
  Reprint of paper 43.155.059.

---------------------------------------------------------
Title: Distribution of Dark Matter in the Spiral Galaxy NGC 3198
Authors: van Albada, T. S.; Bahcall, John N.; Begeman, K.; Sanscisi, R.
1987dmu..conf...58V    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Distribution of dark matter in the spiral galaxy NGC 3198.
Authors: van Albada, T. S.; Bahcall, J. N.; Begeman, K.; Sanscisi, R.
1987IAUS..117...58V    Altcode:
  [Reprint of paper 40.157.046.]

---------------------------------------------------------
Title: Some possible regularities in missing mass.
Authors: Bahcall, J. N.; Casertano, S.
1987IAUS..117...50B    Altcode:
  Reprint of paper 39.157.203.

---------------------------------------------------------
Title: Some Regularities in the Missing Mass Problem
Authors: Casertano, S.; Bahcall, J. N.
1987IAUS..117..136C    Altcode:
  The authors discuss available information on the distribution of
  luminous and dark matter in eight galaxies.

---------------------------------------------------------
Title: Dark matter near the Sun
Authors: Bahcall, J. N.
1987mcu..conf..111B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Dark Matter near the Sun
Authors: Bahcall, J. N.
1986RSPTA.320..543B    Altcode: 1986RSLPT.320..543B
  The amount of dark matter in the disc of the Galaxy at the solar
  position is determined by comparing the observed distributions of tracer
  stars with the predictions obtained from different assumptions of how
  the unseen matter is distributed. The major uncertainties, observational
  and theoretical, are estimated. For all the observed samples, typical
  models imply that about half of the mass in the solar vicinity must
  be in the form of unobserved matter. The volume density of unobserved
  material near the Sun is about [Note: Equation omitted. See the image
  of page 111 for this equation.]; the corresponding column density
  is about [Note: Equation omitted. See the image of page 111 for this
  equation.] (1 pc ≈ 30857 × 10<SUP>12</SUP> m). This, so far unseen,
  material must be in a disc with an exponential scale height of less
  than 0.7 kpc. All the existing observations are consistent with the
  unseen disc material being in the form of stars not massive enough
  to burn hydrogen. It is suggested that the unseen material that is
  required to hold up the rotation curves of galaxies and to satisfy the
  virial theorem for clusters of galaxies might also be in the form of
  low-mass stars.

---------------------------------------------------------
Title: Tests of neutrino stability
Authors: Bahcall, J. N.; Petcov, S. V.; Toshev, S.; Valle, J. W. F.
1986PhLB..181..369B    Altcode:
  A possible solution of the solar neutrino problem is that electron
  neutrinos decay in transit from the sun. The phenomenological
  consequences of this hypothesis for solar neutrino experiments
  with detectors of <SUP>2</SUP>H, <SUP>40</SUP>Ar, <SUP>71</SUP>Ga,
  <SUP>98</SUP>Mo, and electron-neutrino scattering are discussed. The
  postulated fast decay can occur in models of majoron type without
  violating laboratory, cosmological, or astrophysical constraints. <P
  />Address after January 1st, 1987: Department de Física Teòrica,
  Universitat de Valencia, Burjassot, Valencia, Spain.

---------------------------------------------------------
Title: Multiple quasars for multiple images
Authors: Bahcall, John N.; Bahcall, Neta A.; Schneider, Donald P.
1986Natur.323..515B    Altcode: 1986Nat...323..515B
  Three quasar pairs that have been identified as the products of
  gravitational lenses have no obvious visible lenses<SUP>1-3</SUP>. They
  are: 1146+111 (redshift z=1.01; pair separation Δθ=157 arc
  s)<SUP>3</SUP>, 1635+267 (z=1.96; Δθ=4 arc s)<SUP>1</SUP> and
  2345+007 (z=2.15; Δθ=7 arc s)<SUP>2</SUP>. An even number (two)
  of quasar images is observed in each case, although an odd number
  of images is produced by gravitational lenses with non-singular
  potentials<SUP>4</SUP>. The absence of a visible lens creates, in
  the lens hypothesis, a severe `missing matter' problem. The missing
  lenses range in estimated mass<SUP>3,5</SUP> from &gt;10<SUP>12</SUP>
  M <SUB>solar</SUB> for 1635+267 (where M <SUB>solar</SUB> is the mass
  of the Sun) to ~10<SUP>15</SUP> M <SUB>solar</SUB> for 1146+111. We
  investigate here the possibility that these quasar images are pairs
  of physically distinct quasars in galaxy associations. We show that,
  at the same redshifts as the quasars, only galaxy associations of
  exceptional richness would be identifiable in the existing data. Less
  prominent groups of galaxies, such as those known to be associated with
  nearby quasars<SUP>6</SUP>, would not be visible. We calculate the
  probability of pairs of quasars appearing in galaxy associations and
  find that physical pairs could appear with the observed frequency if,
  as expected, quasars are more common relative to galaxy associations
  at earlier epochs. We also discuss observations that can distinguish
  between the hypothesis of a gravitational lens and that of physical
  pairs.

---------------------------------------------------------
Title: Predictions for a liquid argon solar neutrino detector
Authors: Bahcall, J. N.; Baldo-Ceolin, M.; Cline, D. B.; Rubbia, C.
1986PhLB..178..324B    Altcode:
  A liquid argon time projection chamber can be used to make separate
  measurements of electron neutrinos and neutrinos of different
  flavors, to determine the incident neutrino spectrum, and to verify
  that neutrinos come from the direction of the sun. Resonant neutrino
  oscillation has a dramatic effect on the shape of the predicted spectrum
  of recoil electrons.

---------------------------------------------------------
Title: Kinematics and Density of the Galactic Spheroid
Authors: Bahcall, J. N.; Casertano, S.
1986ApJ...308..347B    Altcode:
  The authors reanalyze Eggen's proper-motion and radial velocity
  data for a sample of 94 stars with transverse velocities in excess
  of 220 km s<SUP>-1</SUP>, correcting for observational biases and
  selection effects by a Monte Carlo analysis of simulated catalogs of
  proper-motion stars. They obtain a local spheroid number density of n =
  (9.5±1.3)×10<SUP>-5</SUP>pc<SUP>-3</SUP> for 4 ≤ M<SUB>V</SUB> ≤
  11 mag. The Eggen catalog yields the following kinematic parameters
  for the spheroid: an asymmetric drift of 154 km s<SUP>-1</SUP>
  (corresponding to a rotation velocity ≡66 km s<SUP>-1</SUP>), and
  velocity dispersions in the r, θ, and z directions of 140, 100, and
  76 km s<SUP>-1</SUP>, respectively. All three of the commonly applied
  definitions of the spheroid (pressure supported, low metallicity,
  and geometric distribution) yield consistent results for the density
  of Population II stars in the vicinity of the Sun.

---------------------------------------------------------
Title: Solar neutrinos from the decay of <SUP>8</SUP>B
Authors: Bahcall, John N.; Holstein, Barry R.
1986PhRvC..33.2121B    Altcode:
  The spectrum of neutrinos produced by the beta decay of <SUP>8</SUP>B
  in the sun is computed including forbidden corrections to the weak
  interactions. The total cross section for absorption by <SUP>37</SUP>Cl
  of <SUP>8</SUP>B neutrinos is (1.06+/-0.1)×10<SUP>-42</SUP>
  cm<SUP>2</SUP>. The uncertainty is determined by calculating the
  cross section using different measured spectra for the alpha particles
  that result from the decay of <SUP>8</SUP>B to <SUP>8</SUP>Be and by
  varying the transition matrix elements consistent with the branching
  ratios measured using delayed protons emitted in the beta decay of
  <SUP>37</SUP>Ca.

---------------------------------------------------------
Title: Wide Binaries in the Direction of Andromeda
Authors: Bahcall, John N.; Jones, Burton F.; Ratnatunga, Kavan U.
1986ApJS...60..939B    Altcode:
  A statistically well-defined sample of candidate binary stars with
  separations that are expected to be mostly in the range 0.01-0.1
  pc is presented. The 36 candidate pairs are all brighter than
  apparent visual magnitude 12; about half of the projected pairs are
  expected to be physically associated. After the candidates are studied
  spectroscopically and photometrically to establish which pairs are real
  binaries and to measure their physical characteristics, the sample
  can be used to help determine the dependence of number density on
  semimajor axis for wide binaries, a function that is of considerable
  theoretical interest.

---------------------------------------------------------
Title: The galactic environment of the solar system.
Authors: Bahcall, John N.
1986gss..conf....3B    Altcode: 1986gass.book....3B
  The general features of the galactic environment of the solar system
  are described. The principal components of the distribution of matter
  in the solar vicinity are discussed. Special emphasis is placed upon
  the question of determining the total amount of matter in the vicinity
  of the Sun.

---------------------------------------------------------
Title: Solar neutrinos: theory.
Authors: Bahcall, J. N.
1986wein.conf..705B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Missing matter in the vicinity of the Sun.
Authors: Bahcall, John N.
1986isos.book..207B    Altcode:
  The Poisson and Vlasov equations are solved numerically for realistic
  Galaxy models which include multiple disk components, a Population
  II spheroid, and an unseen massive halo. The total amount of matter
  in the vicinity of the sun is determined by comparing the observed
  distributions of tracer stars, samples of F dwarfs, and K giants with
  the predictions of the Galaxy models. Results are obtained for a number
  of different assumed distributions of the unseen disk mass. For all
  the observed samples, typical models imply that about half of the mass
  in the solar vicinity must be in the form of unobserved matter. The
  volume density of unobserved material near the sun is about 0.1 solar
  mass/cu pc; the corresponding column density is about 30 solar mass/sq
  pc. This so far unseen material must be in a disk with an exponential
  scale height of less than 0.7 kpc.

---------------------------------------------------------
Title: Solar Neutrinos
Authors: Bahcall, John N.
1986hmac.book...85B    Altcode:
  Contents: 1. Introduction. 2. Stellar evolution. 3. Nuclear
  fusion in the Sun. 4. The <SUP>37</SUP>Cl solar neutrino
  experiment. 5. Uncertainties in the predictions. 6. Observational
  implications. 7. New experiments. 8. Conclusion.

---------------------------------------------------------
Title: Brown dwarfs: conference summary.
Authors: Bahcall, J. N.
1986abd..proc..233B    Altcode:
  Some of the major observational and theoretical issues in the study of
  brown dwarfs are reviewed. It is concluded that all of the unseen local
  disk matter could be in the form of brown dwarfs without conflicting
  with any available observations.

---------------------------------------------------------
Title: Star counts and galactic structure.
Authors: Bahcall, John N.
1986ARA&A..24..577B    Altcode:
  Star counts are discussed as an aid in studies of galactic
  structure. Iterative computations using a method-of-color-bins to match
  numerical models with observational data are described. The star counts
  provide bounds for the luminosity function and the color-magnitude
  diagram and allow spheroid normalization in a copycat Galaxy model
  which posits a galaxy with a Population I disk and a Population
  II spheroid. Good agreement has been obtained between star counts
  predicted by the model and observed distributions, including color
  and magnitude ranges and direction. Modifications being considered
  for the model include consideration of the halo, a galactic bulge and
  a thick disk. Several galactic structural features which have yet to
  be modeled and which may be tractable to the copycat model corrected
  with star counts are identified.

---------------------------------------------------------
Title: An analysis of the Basel star catalog.
Authors: Bahcall, J. N.; Ratnatunga, K. U.; Buser, R.; Fenkart, R. P.;
   Spaenhauer, A.
1985ApJ...299..616B    Altcode:
  The standard Bahcall-Soneira (1980) Galaxy model is compared with
  the data from the 12 fields in the Basel star catalog that are at
  Galactic latitudes above 20 deg and have E(B-V) of less than 0.1
  mag. Good agreement is found between the calculated and observed color
  distributions, as well as star counts, for all the fields. The globular
  cluster feature that is observed in the luminosity function of globular
  clusters near M(v) = +1 to +4 mag is also present in the spheroid
  field stars. It is possible to assign some of the spheroid stars from
  the standard two-component Galaxy model (thin disk plus de Vaucouleurs
  spheroid) to a third stellar component (a thick disk with a spheroid
  luminosity function) without disturbing the agreement with observations.

---------------------------------------------------------
Title: Estimating the masses of galaxy groups: alternatives to the
    virial theorem.
Authors: Heisler, J.; Tremaine, S.; Bahcall, J. N.
1985ApJ...298....8H    Altcode:
  The authors present three alternatives to the virial
  theorem for estimating the masses of groups of
  galaxies. The projected mass estimator uses the mean
  value of V<SUB>i</SUB><SUP>2</SUP>|R<SUB>i</SUB>|,
  where V<SUB>i</SUB> and R<SUB>i</SUB>are the radial
  velocity and projected separation of galaxy i from the group
  center. The other two methods rely on the average and median of
  (V<SUB>i</SUB>-V<SUB>j</SUB>)<SUP>2</SUP>|R<SUB>i</SUB>-R<SUB>j</SUB>|
  over all pairs of galaxies in the group. These three estimators and the
  virial theorem estimator are tested using a series of N-body simulations
  and Monte Carlo realizations of Michie models. The authors use the mass
  estimators to calculate the masses and mass-to-light ratios of nearby
  groups catalogued by Huchra and Geller. The results confirm their work,
  implying that there is a large amount of dark mass in groups on scales
  of ≡700 kpc.

---------------------------------------------------------
Title: The Solar Neutrino Problem
Authors: Bahcall, J. N.
1985SoPh..100...53B    Altcode:
  The observed capture rate for solar neutrinos in the <SUP>37</SUP>Cl
  detector is lower than the predicted capture rate. This discrepancy
  between theory and observation is known as the `solar neutrino
  problem'. I review the basic elements in this problem: the detector
  efficiency, the theory of stellar (solar) evolution, the nuclear physics
  of energy generation, and the uncertainties in the predictions. I also
  answer the questions of: So What? and What Next?

---------------------------------------------------------
Title: Estimated number of field stars toward galactic globular
    clusters andlocal group galaxies.
Authors: Ratnatunga, K. U.; Bahcall, J. N.
1985ApJS...59...63R    Altcode:
  Field star densities are estimated for 89 fields with /b/ greater than
  10 degrees based on the Galaxy model of Bahcall and Soneira (1980,
  1984; Bahcall et al. 1985). Calculated tables are presented for 76
  of the fields toward Galactic globular clusters, and 16 Local Group
  Galaxies in 13 fields. The estimates can be used as an initial guide
  for planning both ground-based and Space Telescope observations of
  globular clusters at intermediate-to-high Galactic latitudes.

---------------------------------------------------------
Title: Sampling errors in the determination of the total amount of
    mass at the solar position
Authors: Gilden, D. L.; Bahcall, J. N.
1985ApJ...296..240G    Altcode:
  The sampling errors that occur in the determination of the total volume
  and column density of mass at the solar position have been evaluated
  by analyzing simulated star catalogs as if they were observed sets of
  stars. The simulations were achieved by generating ensembles of stellar
  orbits that pass through the solar position in a realistic mass model
  of the Galaxy. These orbits are sampled in a way that mimics observing
  procedures in order to form pseudo-star catalogs. The catalogs are used
  to determine the sampling errors in a derivation of the total volume
  density of matter near the Sun (the Oort limit). The simulations show
  that the overall analysis is unbiased. It is demonstrated that sampling
  errors alone cannot account for the missing matter in the disk, as
  analyzed most recently by Bahcall.

---------------------------------------------------------
Title: Gamow-Teller strength function in <SUP>71</SUP>Ge via the
    (p,n) reaction at medium energies
Authors: Krofcheck, D.; Sugarbaker, E.; Rapaport, J.; Wang, D.;
   Bahcall, J. N.; Byrd, R. C.; Foster, C. C.; Goodman, C. D.; van
   Heerden, I. J.; Gaarde, C.; Larsen, J. S.; Horen, D. J.; Taddeucci,
   T. N.
1985PhRvL..55.1051K    Altcode:
  The Gamow-Teller strength function in <SUP>71</SUP>Ge has been measured
  by use of the <SUP>71</SUP>Ga(p,n) reaction at E<SUB>p</SUB>=120 and 200
  MeV. While a significant fraction of the total strength is associated
  with excited states located below particle-emission threshold, the first
  excited state exhibits little strength. Excited-state contributions to
  the total solar-neutrino capture rate for a <SUP>71</SUP>Ga detector are
  about 14 solar neutrino units for the neutrino spectrum of the standard
  solar model and about 3-4 solar neutrino units for representative
  nonstandard solar models.

---------------------------------------------------------
Title: Distribution of dark matter in the spiral galaxy NGC 3198.
Authors: van Albada, T. S.; Bahcall, J. N.; Begeman, K.; Sancisi, R.
1985ApJ...295..305V    Altcode:
  Two-component mass models, consisting of an exponential disk and a
  spherical halo, are constructed to fit a newly determined rotation
  curve of NGC 3198 that extends to 11 disk scale lengths. The amount of
  dark matter inside the last point of the rotation curve, at 30 kpc,
  is at least 4 times larger than the amount of visible matter, with
  M/L(B)tot = 18 solar M/L(B). The maximum mass-to-light ratio for the
  disk is M/L(B) = 3.6. The available data cannot discriminate between
  disk models with low M/L and high M/L, but arguments are presented
  which suggest that the true mass-to-light ratio of the disk is close
  to the maximum computed value. The core radius of the distribution of
  dark matter is found to satisfy R(core) of between 1.7 and 12.5 kpc.

---------------------------------------------------------
Title: The Sun's motion perpendicular to the galactic plane
Authors: Bahcall, J. N.; Bahcall, S.
1985Natur.316..706B    Altcode:
  The period and amplitude of the Sun's motion perpendicular to the
  galactic plane are important parameters in some explanations of the
  terrestrial mass extinctions and cratering records<SUP>1-5</SUP>. Here
  we have calculated the range of periods and vertical excursions that are
  consistent with the distributions of tracer stars in the Galaxy and have
  also evaluated the probable phase jitter in the solar period. We find
  acceptable half-periods for the vertical oscillation that range from 26
  to 37 Myr (including the range of periods that have been inferred from
  the terrestrial records on mass extinctions and on cratering), maximum
  heights above the plane from 49 to 93 pc, and an average phase jitter
  per half-period of the order of 6-9%. The largest uncertainty in all
  these calculations is caused by the unknown distribution of the unseen
  mass that must be postulated to explain the distribution of observed
  stars<SUP>6-7</SUP>. For all the models we consider, the most recent
  passage of the Sun through the galactic plane occurred in the past
  3 Myr provided only that the present position of the Sun is between
  0 and 20 pc above the plane. We extend the argument of Thaddeus and
  Chanan<SUP>8</SUP> to show that the apparent periodicity in the mass
  extinction and cratering records cannot be caused by an population of
  objects (observed or unobserved) that contributes a major fraction of
  the total mass density at the solar vicinity.

---------------------------------------------------------
Title: Some possible regularities in the missing mass problem.
Authors: Bahcall, J. N.; Casertano, S.
1985ApJ...293L...7B    Altcode:
  In the present consideration of the missing mass problem, equations
  are developed which express relatively well determined parameters
  characterizing the internal properties of all the mass models invoked in
  a sampling of spiral galaxy cases. The numerical values thus obtained
  constitute benchmarks, relative to which theories of spiral galaxy
  formation can be tested. Simple regularities are noted to be exhibited
  by the unseen matter in the spiral galaxy sample. Attention is given to
  the possibility that both the visible and invisible matter are baryonic.

---------------------------------------------------------
Title: Chlorine and gallium solar neutrino experiments
Authors: Bahcall, J. N.; Cleveland, B. T.; Davis, R., Jr.; Rowley,
   J. K.
1985ApJ...292L..79B    Altcode:
  The authors reevaluate the expected capture rates and their
  uncertainties for the chlorine and gallium solar neutrino experiments
  using improved laboratory data and new theoretical calculations. They
  also derive a minimum value for the flux of solar neutrinos that
  is expected provided only (1) that the sun is currently producing
  energy by fusing light nuclei at the rate that it is emitting energy
  in the form of photons from its surface and (2) that nothing happens
  to solar neutrinos on their way to earth. These results are used -
  together with Monte Carlo simulations - to determine how much gallium
  is required for a solar neutrino experiment.

---------------------------------------------------------
Title: Solar neutrino detection: Experimental determination of
    Gamow-Teller strengths via the <SUP>98</SUP>Mo and <SUP>115</SUP>In
    (p,n) reactions
Authors: Rapaport, J.; Welch, P.; Bahcall, J.; Sugarbaker, E.;
   Taddeucci, T. N.; Goodman, C. D.; Foster, C. F.; Horen, D.; Gaarde,
   C.; Larsen, J.; Masterson, T.
1985PhRvL..54.2325R    Altcode:
  The empirical distribution of Gamow-Teller strengths in <SUP>98</SUP>Tc
  and <SUP>115</SUP>Sn have been obtained via the (p,n) reaction at
  E<SUB>p</SUB>=120 MeV and E<SUB>p</SUB>=200 MeV on <SUP>98</SUP>Mo
  and <SUP>115</SUP>In targets. This information is used to calculate
  the cross section for absorption of solar neutrinos in <SUP>98</SUP>Mo
  and <SUP>115</SUP>In, nuclides which are being considered as neutrino
  detectors to accomplish solar neutrino spectroscopy.

---------------------------------------------------------
Title: Maximum mass of objects that constitute unseen disk material
Authors: Bahcall, J. N.; Hut, P.; Tremaine, S.
1985ApJ...290...15B    Altcode:
  It is suggested that the mass of the individual unseen 'disk things'
  which furnish unseen mass satisfies an inequality that is based on
  the demonstrated existence of a large number of wide binary stars in
  the Galaxy whose projected separations are as large as 0.1 pc. Since
  these binaries are weakly bound, with orbital velocities of 0.3 km/sec
  and periods of the order of 1 million years, they can be disrupted by
  passing stars or other pointlike objects. This implies that the mass
  of the unseen disk objects, which provide about half the local mass
  density, must be less than 2 solar masses.

---------------------------------------------------------
Title: The Total Amount of Matter in the Solar Vicinity
Authors: Bahcall, J. N.
1985BAAS...17..581B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: An Analysis of the Basel Star Catalog
Authors: Ratnatunga, K. U.; Bahcall, J. N.; Buser, R.; Fenkart, R. P.;
   Spaenhauer, A.
1985BAAS...17Q.559R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On the Density of the Spheroid in the Solar Neighborhood
Authors: Casertano, S.; Bahcall, J. N.
1985BAAS...17..560C    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Comparisons of the Standard Galaxy Model with observations
    in two fields
Authors: Bahcall, J. N.; Ratnatunga, K. U.
1985MNRAS.213P..39B    Altcode:
  The Bahcall-Soneira (1984) model for the distribution of stars in
  the Galaxy is compared with the observations reported by Gilmore,
  Reid, and Hewett (1984) in two directions in the sky, the pole and
  the Morton-Tritton (1982) region. It is shown that the Galaxy model
  is in good agreement with the observations everywhere it has been
  tested with modern data, including the magnitude range, V = 17-18,
  and provided that the globular cluster feature is included in the
  luminosity function of the field Population II stars.

---------------------------------------------------------
Title: On the spatial distribution of population II stars in SB and
    later type galaxies.
Authors: Bahcall, J. N.; Kylafis, N. D.
1985ApJ...288..252B    Altcode:
  It is shown that surface-brightness measurements must be accurate to
  about 0.1 mag at 1 percent of the visual sky brightness in order to
  determine the spatial distribution of Population II stars in Sb galaxies
  with bulge-to-disk ratios like those in NGC 891 and in galaxies of
  later Hubble type. The observations of van der Kruit and Searle (1981)
  of the edge-on galaxy NGC 891 are fitted with two different models:
  a thin disk and a de Vaucouleurs spheroid, and a thin disk plus a
  thicker disk. The observations are well described by both models. The
  difficulty of discriminating between various shapes for the light
  distribution of Population II stars increases with galaxy inclination.

---------------------------------------------------------
Title: Space Telescope observations of globular clusters.
Authors: Bahcall, J. N.
1985IAUS..113..481B    Altcode:
  Six proposed Space Telescope programs involving globular clusters are
  described. The projects appropriate for galactic clusters are: the
  detection of white dwarfs, the study of the faint end of the Population
  II luminosity function, the measurement of mass segregation, and the
  search for a cusp in the density distribution caused by core collapse
  or by a massive black hole. The two programs that involve extragalactic
  globular clusters are: the determination of the luminosity function
  of clusters around different galaxies and the measurement of tidal
  radii of clusters surrounding elliptical galaxies.

---------------------------------------------------------
Title: The solar neutrino problem: astronomy or physics?
Authors: Bahcall, J. N.
1985fsgf.book..267B    Altcode: 1986fsgf.book..267B
  A review of current theoretical and observational attempts to resolve
  the solar neutrino dilemma is presented.

---------------------------------------------------------
Title: Solar neutrino experiments: Theory
Authors: Bahcall, J. N.
1985AIPC..126...60B    Altcode: 1985snna.proc...60B
  The expected capture rates and their uncertainties are reevaluated
  for the chlorine and gallium experiments using improved laboratory
  data and new theoretical calculations. I also state a minimum value
  for the flux of solar neutrinos that is expected provided only that
  the sun is currently burning light nuclei at the rate it is emitting
  photons from its surface and that nothing happens to solar neutrinos
  on their way to the earth. These results are used-together with Monte
  Carlo simulations performed by Bruce Cleveland-to determine how much
  gallium is required for a solar neutrino experiment.

---------------------------------------------------------
Title: K giants and the total amount of matter near the sun
Authors: Bahcall, J. N.
1984ApJ...287..926B    Altcode:
  The Poisson and Boltzmann equations are solved numerically for realistic
  Galaxy models which include multiple disk components (between 14 and
  28), a Population II spheroid, and an unseen massive halo. As a guide in
  constructing the theoretical models, a population of normal-metallicity
  (disk) K giants is isolated using existing data and is shown to be
  well described by an isothermal distribution function with a velocity
  dispersion perpendicular to the plane of 20 km s<SUP>-1</SUP>. The
  total amount of matter in the vicinity of the Sun is determined by
  comparing the observed distributions of K giants with the predictions
  of detailed Galaxy models. The volume density of unobserved material
  near the Sun is about 0.1 M_sun; pc<SUP>-3</SUP>; the corresponding
  column density is about 30 M_sun; pc<SUP>-2</SUP>.

---------------------------------------------------------
Title: Dark Matter Near the Sun: Simulated Star Counts and the
    Oort Limit
Authors: Gilden, D.; Bahcall, J. N.
1984NASCP2345..326G    Altcode: 1984lism.rept..326G; 1984IAUCo..81..326G
  An ensemble of orbits passing through the solar position have been
  generated for a specific mass model of the galaxy. These orbits are
  randomly sampled to form simulated density distributions of tracer stars
  perpendicular to the galactic disk. The simulated distributions are
  analyzed in order to determine the sampling errors in a self-consistent
  derivation of the total amount of matter near the Sun (the Oort limit).

---------------------------------------------------------
Title: Velocity dispersions of disk stars in spiral galaxies.
Authors: Bahcall, J. N.; Casertano, S.
1984ApJ...284L..35B    Altcode:
  For multicomponent spiral disks, the authors derive a relation for
  individual stellar components between the total surface density of
  mass and the observed luminosity scale height and vertical velocity
  dispersion. A criterion is given for the validity of the relation in
  the presence of spheroidal mass distributions and an inhomogeneous
  disk. Mass models for the Milky Way and NGC 891, 4565, and 5907 are
  used to illustrate what velocity dispersions observers might expect
  to measure in nearly face-on spiral galaxies.

---------------------------------------------------------
Title: Detection of binaries with projected separations as large as
    0.1 parsec.
Authors: Latham, D. W.; Tonry, J.; Bahcall, J. N.; Soneira, R. M.;
   Schechter, P.
1984ApJ...281L..41L    Altcode:
  Repeated, accurate radial velocity measurements have been made of the 19
  candidate wide binary stellar pairs of Bahcall and Soneira. There are 16
  unambiguous cases of which six pairs are physical binaries. Projected
  separations of the binaries are estimated using the observed angular
  separations and well-determined spectroscopic parallaxes. The projected
  separations vary from about 0.002 pc to 0.08 pc. This validation of
  the statistical techniques used in identifying the candidate wide
  binaries opens up the possibility of large-scale systematic studies
  of the characteristics of wide binaries.

---------------------------------------------------------
Title: K-Giants and the Total Amount of Matter Near the Sun
Authors: Bahcall, J. N.
1984BAAS...16..733B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Comparisons of a standard galaxy model with stellar
    observations in five fields.
Authors: Bahcall, J. N.; Soneira, R. M.
1984ApJS...55...67B    Altcode:
  Modern data on the distribution of stellar colors and on the number
  of stars as a function of apparent magnitude in five directions
  in the Galaxy are analyzed. It is found that the standard model is
  consistent with all the available data. Detailed comparisons with
  the data for five separate fields are presented. The bright end of
  the spheroid luminosity function and the blue tip of the spheroid
  horizontal branch are analyzed. The allowed range of the disk scale
  heights and of fluctuations in the volume density is determined, and
  a lower limit is set on the disk scale length. Calculations based on
  the thick disk model of Gilmore and Reid (1983) are presented.

---------------------------------------------------------
Title: Current Status of Solar Neutrino Research
Authors: Bahcall, J.
1984BAAS...16..521B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Self-consistent determinations of the total amount of matter
    near the sun.
Authors: Bahcall, J. N.
1984ApJ...276..169B    Altcode:
  The combined Poisson-Boltzmann equation for the gravitational
  potential is solved numerically for detailed Galaxy models whose mass
  components have been determined previously by a variety of observational
  techniques. The basic assumption made is that the disk is composed of
  a finite number of isothermal components. The calculated potential as
  a function of height above the plane is used to fit the distribution
  of F stars reported by Hill, Hilditch, and Barnes to a distance of 200
  pc. The inferred mass and column densities depend upon the model adopted
  for the unseen matter. The total mass density at the solar position is
  0.185 + or - 0.02 solar mass per cu pc if the distribution of unobserved
  matter is proportional to the distribution of observed material,
  the Bahcall and Soneira Galaxy model is adopted, and the isothermal
  approximation is valid. The corresponding column density is 67 solar
  mass per sq pc, and the disk mass-to-light ratio is 2.9. The total mass
  and column densities are computed for a number of other assumptions
  about the unobserved material and the Galaxy model. The inferred
  mass and column densities are not sensitive to small contaminations
  or departures from isothermality in the sample of F stars that was
  used. The unobservd disk material is at least as large as 50 percent
  of the total observed disk material in all of the models considered.

---------------------------------------------------------
Title: The distribution of stars perpendicular to galactic disk
Authors: Bahcall, J. N.
1984ApJ...276..156B    Altcode:
  The combined Boltzmann and Poisson equations for the isothermal
  distribution of stars perpendicular to a galactic disk are solved in the
  presence of a spheroidal halo. The solutions depend in a simple way upon
  the ratio, epsilon, of effecive halo mass density to disk mass density
  in the fundamental plane of the disk. These results suggest a new way of
  measuring the ratio of halo to disk mass densities either by observing
  the number of stars of a given type as a function of height above
  the plane in the Galaxy or by observing the distribution of starlight
  perpendicular to the disks of other galaxies. Exact numerical - and
  approximate analytic solutions are derived for disks that are composed
  of one or several separate stellar components. Non-isothermal solutions
  are also discussed. The advantages of using the self-consistent models
  described here for the determination of the total amount of matter
  near the sun are enumerated.

---------------------------------------------------------
Title: El Telescopio Espacial.
Authors: Bahcall, J. N.; Spitzer, L., Jr.
1984RvA....56....9B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Missing Matter in the Vicinity of the Sun
Authors: Bahcall, J. N.
1984ASSL..110..241B    Altcode: 1984astt.coll..241B; 1984IAUCo..78..241B
  The combined Poisson-Boltzmann equation for the gravitational potential
  is solved numerically for a detailed Galaxy model. The main result -
  obtained by comparing the calculated densities with observations of
  F dwarfs and K giants - is that about half of the mass density in the
  vicinity of the sun has not yet been observed.

---------------------------------------------------------
Title: Some constraints N the color-magnitude diagram of giants in
    the galactic spheroid.
Authors: Bahcall, J. N.; Soneira, R. M.; Morton, D. C.; Tritton, K. P.
1983ApJ...272..627B    Altcode:
  The color-magnitude diagram of giants in the Galactic spheroid is shown
  to be important in determining the number-color histogram of stars
  brighter than B = 19 mag. This result is demonstrated by comparing a
  standard Galaxy model with observations of 391 stars in a field in
  the direction of Aquarius (l = 36.5 deg, b = -51.1 deg). More than
  80 percent of the spheroid stars and 40 percent of all stars in this
  magnitude range and direction are predicted to be giants. At most,
  a few percent of the spheroid stars in the current sample can lie on
  the main sequence bluer than the turn-off onto the giant branch near
  B - V approximately 0.4. The available observations suggest that the
  blue tip of the horizontal branch of the spheroid must be sparsely
  populated about a factor of 10 less than would be expected if the
  color-magnitude diagram of the spheroid were the same as diagrams for
  any of the globular clusters M3, M13, or M92. The total dispersion in
  colors (measurement errors and intrinsic dispersion) has a standard
  deviation in B - V color that is less than 0.2 mag.

---------------------------------------------------------
Title: The Total amount of Matter Near the Sun
Authors: Bahcall, J. N.
1983nssl.conf..271B    Altcode: 1983IAUCo..76..271B; 1983LDP.....4..271B
  The combined Poisson-Boltzmann equation for the gravitational potential
  is solved numerically for detailed Galaxy models whose mass components
  have been determined previously by a variety of observational
  techniques. The calculated potential as a function of height above
  the plane is used to fit the distribution of F stars reported by Hill,
  Hilditch, and Barnes to a distance of 200 pc. The total mass density
  at the solar position is 0.185±0.02 M_sun; pc<SUP>-3</SUP> if the
  distribution of unobserved matter is proportional to the distribution
  of observed material, the Bahcall and Soneira Galaxy model is adopted,
  and the isothermal approximation is valid.

---------------------------------------------------------
Title: Detection of Stars in the Dark Galactic Halo
Authors: Bahcall, J. N.; Soneira, R. M.
1983nssl.conf..223B    Altcode: 1983LDP.....4..223B; 1983IAUCo..76..223B
  The authors show how available star counts to m<SUB>v</SUB> = 22
  together with a model of the Galaxy can be used to set limits on the
  maximum brightness of the stellar constituents of a massive halo. They
  find there can be few stars brighter than M<SUB>v</SUB> = +14 in an
  r<SUP>-2</SUP> halo component.

---------------------------------------------------------
Title: Comparison of the Bahcall / Soneira Galaxy Model with
    Observations
Authors: Bahcall, J. N.; Soneira, R. M.
1983nssl.conf..209B    Altcode: 1983LDP.....4..209B; 1983IAUCo..76..209B
  Modern data on the distribution of stellar colors and on the number
  of stars as a function of apparent magnitude in five directions in
  the Galaxy are analyzed. Observational studies by various authors are
  analyzed. All of the data are described well by a two-component model
  with an exponential disk and a de Vaucouleurs spheroid. The fat-disk
  model proposed by Gilmore and Reid does not fit the results of Kron
  for SA57 and of Koo and Kron for SA68.

---------------------------------------------------------
Title: Binary-single star scattering. I - Numerical experiments for
    equal masses
Authors: Hut, P.; Bahcall, J. N.
1983ApJ...268..319H    Altcode:
  A first report is presented regarding an extensive project which is
  designed to provide a representative coverage of binary-single star
  scattering, and at least an exploration of binary-binary scattering. It
  is the aim of the project to present cross sections and reaction
  rates which are obtained by numerical orbit integration from initial
  conditions determined by Monte Carlo techniques. The main difference
  between the current project and previous work is related to the large
  amount of computer time available. In this connection, it has already
  been possible to conduct a million orbit calculations. The results
  of these calculations are analyzed in this report. A framework of
  binary-single star scattering is described for the most general
  case. Data are provided for the case where all stars have equal masses.

---------------------------------------------------------
Title: The ratio of the unseen halo mass to the luminous disk mass
    in NGC 891.
Authors: Bahcall, J. N.
1983ApJ...267...52B    Altcode:
  The present investigation has the objective to provide an estimate of
  the range of halo to disk mass ratios which are compatible with the
  available observations for NGC 891 and to suggest ways by which future
  observations could add to the understanding of the mass distribution in
  this galaxy. It is found that the ratio of total halo to disk mass for
  NGC 891 varies by more than an order of magnitude for phenomenological
  models based on the available observations. The models with halo to
  disk mass ratios of order unity have self-gravitating stellar disks
  (close to the plane of the disk) out to galactocentric distances of at
  least as large as 21 kpc, the apparent truncation radius. A model with
  a very massive halo has a disk which is not self-gravitating beyond
  R approximately 7 kpc.

---------------------------------------------------------
Title: Stellar collapses in the Galaxy.
Authors: Bahcall, J. N.; Piran, T.
1983ApJ...267L..77B    Altcode:
  Comparisons are made between the sensitivities of the one existing
  chlorine vat neutrino detector and gravity wave detectors for
  providing evidence of stellar collapse. The galactic star fraction
  within detection range is calculated as a controlling factor for the
  detectors. An expected collapse rate of 0.1 per year is projected by
  using a model of star distribution in the disk and standard values
  for Population I star lifetimes. A maximum detection radius of 1.5 kpc
  is obtained, as well as a detection rate of 0.0006/yr, two orders of
  magnitude less than the observational upper limit. For stars between
  3-10 solar masses, the expected detection rate is 0.01/yr. The existing
  solar neutrino detector is concluded not to have registered a stellar
  collapse in the last 10 yr. Only 6 pecent of the stars in the galaxy
  can be monitored with present gravity wave detectors, and methods for
  increasing their effectiveness to 90 percent are indicated.

---------------------------------------------------------
Title: Galaxies, quasars, and beyond - The Space Telescope
Authors: Bahcall, J. N.
1983aans.sympR..25B    Altcode:
  The overall NASA plans for the Space Telescope are described. A brief
  history of the development of the Space Telescope is presented and
  the major characteristics of the ST Observatory are summarized. The
  astronomical instruments that will be used in the first few years are
  described and some of the important scientific projects are outlined.

---------------------------------------------------------
Title: The galactic spheroid
Authors: Bahcall, J. N.; Soneira, R. M.; Schmidt, M.
1983ApJ...265..730B    Altcode:
  Analytic approximations and numerical simulations are used to derive
  the characteristic behavior of star counts in a galactic spheroidal
  population, whose visible stars' stellar luminosity function is
  obtainable for galactocentric distances between about 4 and 12 kpc
  from star count observations above 30 deg galactic latitude. The
  total densities of stars and of mass in the spheroid at the solar
  position are evaluated using different assumed luminosity functions,
  in order to extrapolate the measured values to a wider range of absolute
  magnitudes. The upper limits to the frequency of intermediate population
  stars are derived for the absolute visual magnitude range of 5-8. If
  such stars occur in either a flat disk with a scale height of 3 kpc
  or a spheroid with an ellipticity of 0.5, their local surface density
  is less than 1.8 times that of the spheroid.

---------------------------------------------------------
Title: Solar neutrinos.
Authors: Bahcall, J. N.
1983neap.conf...71B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The distribution of stars in the Galaxy
Authors: Bahcall, J. N.; Soneira, R. M.
1983ASSL..100..209B    Altcode: 1983kdsm.work..209B
  A discussion is presented of the basic ideas underlying the use of
  star counts to determine galactic parameters. Previous work using star
  counts is reviewed, and possible future observational programs that
  will be important in increasing the knowledge of the stellar content
  of the galaxy are indicated. The techniques used in star counts are
  illustrated by applications to the differential number-magnitude
  counts in SA 57, the frequency-color diagrams in SA 57 and SA 68,
  the paucity of intermediate population stars in the range M(V) = 5-8,
  and the M/L ratio for the unseen matter in the halo.

---------------------------------------------------------
Title: Galaxies, quasars, and beyond - the Space Telescope.
Authors: Bahcall, J. N.
1983gqb..book.....B    Altcode:
  The overall NASA plans for the Space Telescope are described. A brief
  history of the development of the Space Telescope is presented and
  the major characteristics of the ST Observatory are summarized. The
  astronomical instruments that will be used in the first few years are
  described and some of the important scientific projects are outlined.

---------------------------------------------------------
Title: Asymmetric emission-line regions with out-flowing mass in
    QSOs and the z/ab/ at least equal to z/em/ systems
Authors: Goldman, I.; Bahcall, J. N.
1982A&A...115..242G    Altcode:
  A heuristic asymmetrical model for a quasar emission-line region,
  with material streaming out, is described. The physical parameters
  are essentially the same as those of static models; the geometry
  turns out to be the dominant factor in determining the emission line
  profiles. Calculations are carried out for a variety of parameterized
  flow models and for the Blumenthal and Mathews (1975) theoretical
  model of a radiatively driven flow. The emission-line profiles are
  insensitive to the details of the acceleration, the filling factor,
  and the ionization profile. Absorption is assumed to take place in
  stationary matter in the QSO's galaxy or associated group or cluster,
  so that z(ab) is identified with the cosmological redshift. Due
  to the flow, the emission-lines are shifted with respect to the
  absorption-lines; in cases of a flow directed towards the observer
  systems with z(ab) at least equal to z(em) result. The distribution
  of absorption redshifts is symmetric about z(em).

---------------------------------------------------------
Title: On the interpretation of rotation curves measured at large
    galactocentric distances
Authors: Bahcall, J. N.; Schmidt, M.; Soneira, R. M.
1982ApJ...258L..23B    Altcode:
  It is shown that the inferred slope of the density law for a massive
  galactic halo is sensitive to the distribution of mass within the
  radius of interest. Illustrative rotation curves are presented that
  are flat to + or - 1 km/s in the region from 40 to 60 kpc, but which
  have local logarithmic slopes for the halo density law of about 2.7
  (and in one case a finite total mass) instead of the conventionally
  assumed logarithmic slope of 2.0. The contributions of the disk and
  spheroid must be taken into account in the intermediate region of
  about 10-30 kpc in which most current observations are being carried
  out. These results complicate the interpretation of galaxy rotation
  curves at large galactocentric distances.

---------------------------------------------------------
Title: The Space Telescope
Authors: Bahcall, J. N.; Spitzer, L., Jr.
1982SciAm.247a..40B    Altcode: 1982SciAm.247...40B
  After defining the problems posed for optical telescopy by atmospheric
  absorption in the infrared and ultraviolet regions, and a brief history
  of attempts to date to circumvent these problems by the deployment of
  small telescopes aboard rockets, balloons and satellites, a description
  is given of the design features and operational capabilities of the
  NASA Space Telescope. This telescope, which is scheduled to be put in
  earth orbit by the Space Shuttle in 1985, will have a 2.4 m-diameter
  primary mirror capable of concentrating electromagnetic radiation from
  all optical parts of the spectrum and carry scientific instruments which
  will record ultrahigh resolution astronomical images. The telescope's
  scientific instrument section will include a high speed photometer,
  a high resolution spectrograph, a faint object spectrograph, a wide
  field planetary camera, and a faint object camera

---------------------------------------------------------
Title: Standard solar models and the uncertainties in predicted
    capture rates of solar neutrinos
Authors: Bahcall, John N.; Huebner, Walter F.; Lubow, Stephen H.;
   Parker, Peter D.; Ulrich, Roger K.
1982RvMP...54..767B    Altcode:
  The uncertainties that affect the prediction of solar neutrino fluxes
  are evaluated with the aid of standard solar models. The uncertainties
  are determined from available data for all measured quantities that
  are known to affect significantly the neutrino fluxes; these include
  nuclear reaction rates, the solar constant, and the primordial surface
  composition of the sun. Uncertainties in theoretical quantities
  (such as the stellar opacity, the equation of state, and the rate of
  the proton-proton reaction) are estimated from the range of values
  in published state-of-the-art calculations. The uncertainty in each
  neutrino flux that is caused by a specified uncertainty in any of
  the parameters is evaluated with the aid of a series of standard
  solar models that were constructed for this purpose; the results are
  expressed in terms of the logarithmic partial derivative of each flux
  with respect to each parameter. The effects on the neutrino fluxes
  of changing individual parameters by large amounts can usually be
  estimated to satisfactory accuracy by making use of the tabulated
  partial derivatives. An overall "effective 3σ level of uncertainty"
  is defined using the requirement that the true value should lie within
  the estimated range unless someone has made a mistake. Effective 3σ
  levels of uncertainty, as well as best estimates, are determined for
  the following possible detectors of solar neutrinos: <SUP>2</SUP>H,
  <SUP>7</SUP>Li, <SUP>37</SUP>Cl, <SUP>71</SUP>Ga, <SUP>79</SUP>Br,
  <SUP>81</SUP>Br, <SUP>97</SUP>Mo, <SUP>98</SUP>Mo, <SUP>115</SUP>In,
  and electron-neutrino scattering. The most important sources of
  uncertainty in the predicted capture rates are identified and discussed
  for each detector separately. For the <SUP>37</SUP>Cl detector,
  the predicted capture rate is 7.6+/-3.3 (effective 3σ errors)
  SNU. The measured production rate is (Cleveland, Davis, and Rowley,
  1981) 2.1+/-0.3 SNU (1σ error). For a <SUP>71</SUP>Ga detector,
  the expected capture rate is 106 (1<SUP>+0.12</SUP><SUB>-0.08</SUB>)
  SNU (also effective 3σ errors). The relatively small uncertainty
  quoted for the <SUP>71</SUP>Ga detector is a direct result of the
  fact that <SUP>71</SUP>Ga is primarily sensitive to neutrinos from
  the basic proton-proton reaction, the rate of which is determined
  largely by the observed solar luminosity. The Caltech and Munster
  measured values for the cross-section factor for the reaction
  <SUP>3</SUP>He(α,γ)<SUP>7</SUP>Be are inconsistent with each
  other. The capture rates quoted above were obtained using the Caltech
  value for the cross-section factor. If the Munster value is used
  instead, then the predicted capture rate for the <SUP>37</SUP>Cl
  experiment is 4.95+/-2.1 SNU (effective 3σ errors) and, for the
  <SUP>71</SUP>Ga experiment, 96.7 (1<SUP>+0.12</SUP><SUB>-0.08</SUB>) SNU
  (effective 3σ errors). In order for the best-estimate value to agree
  with the observation of Davis (1978) of 2 SNU for the <SUP>37</SUP>Cl
  experiment, the cross-section factor S<SUB>34</SUB> (0) would have
  to be reduced by about 15σ to less than the Caltech value, i.e. to
  7σ less than the Munster value. The characteristics of the standard
  solar model, constructed with the best available nuclear parameters,
  solar opacity, and equation of state, are presented in detail. The
  computational methods by which this and similar models were obtained are
  also described briefly. The primordial helium abundance inferred with
  the aid of standard solar models is Y=0.25+/-0.01. The complementary
  relation between observations of solar neutrinos and of the normal
  modes of oscillation of the sun is examined. It is shown that the
  splitting of the observed large-n, small-l, p-mode (five minute)
  oscillations of the sun primarily originates in the outer ten percent
  of the solar mass, while the neutrinos from <SUP>8</SUP>B beta decay
  originate primarily in the inner five percent of the solar mass. The
  solar luminosity, and the flux of neutrinos from the proton-proton
  reaction, come mostly from an intermediate region.

---------------------------------------------------------
Title: Three-Body Gravitational Scatterings
Authors: Hut, P.; Bahcall, J. N.
1982BAAS...14..654H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: An Account of the Development of the Solar Neutrino Problem
Authors: Bahcall, J. N.; Davis, R., Jr.
1982ena..conf..243B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Gallium Solar Neutrino Detector.
Authors: Hampel, W.; Davis, R., Jr.; Cleveland, B. T.; Friedlander,
   G.; Katcoff, S.; Remsberg, L. P.; Rowley, J. K.; Weneser, J.; Kirsten,
   T.; Heusser, G.; Hübner, M.; Kiko, J.; Pernicka, E.; Schlotz, R.;
   Wunderlich, R.; Dostrovsky, I.; Bahcall, J. N.; Lande, K.; Steinberg,
   R. I.
1982AIPC...96...88H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar nutrinos
Authors: Bahcall, J. N.
1981NASCP2191...81B    Altcode: 1981vsc..conf...81B
  The topics covered include: an overview of the subject of solar
  neutrinos, a brief summary of the theory of stellar evolution, a
  description of the main sources of solar neutrinos, a brief summary
  of the results of the Brookhaven C1-37 experiment, an anaysis of the
  principal solar neutrino experiments, and a discussion of how solar
  neutrino experiments can be used to detect the collapse of stars in
  the Galaxy. A description of how the Ga-71 experiment can be used to
  decide whether the origin of the present discrepancy between theory
  and observation lies in conventional solar models or conventional
  physics is presented.

---------------------------------------------------------
Title: Predicted star counts in selected fields and photometric bands
    Applications to galactic structure, the disk luminosity function,
    and the detection of a massive halo.
Authors: Bahcall, J. N.; Soneira, R. M.
1981ApJS...47..357B    Altcode:
  Tables are presented of predicted star counts in 17 selected directions
  on the sky as a function of apparent B, V, R, and I magnitudes and
  absolute visual magnitudes calculated from the Bahcall-Soneira Galaxy
  model. It is noted that eight of the fields were selected ab initio
  for their usefulness in determining from star counts either parameters
  of galactic structure, the faint end of the disk luminosity function,
  or the detection of a massive stellar halo. Star counts in specified
  fields to m<SUB>I</SUB> = 19 mag are able to reveal the faint end of the
  disk luminosity function down to the end of the hydrogen-burning main
  sequence. It is thought that star counts at high galactic latitudes
  to m<SUB>I</SUB> = 22 mag should reveal the stellar constituents of a
  massive halo if they are massive enough to be on the hydrogen-burning
  main sequence.

---------------------------------------------------------
Title: Dust-sensitive forbidden line ratios
Authors: Draine, B. T.; Bahcall, J. N.
1981ApJ...250..579D    Altcode:
  The paper studies observations of certain pairs of forbidden emission
  lines in the redshifted spectra of intrinsically bright objects, which
  may make possible the study of dust at large distances. The forbidden
  line pairs most likely to be useful in detecting dust in both galactic
  and extragalactic objects are presented, and forbidden O III 2322,
  4364 A, which is the best line pair for the ground-based detection of
  dust intermediate-redshift quasars is discussed. Spectrophotometric
  observations at 1-2 microns could permit the study of dust toward highly
  luminous quasars at redshifts as large as 5, and quasars brighter than
  visual magnitude 17 are presented as candidates for studying dust with
  forbidden O III 2322, 4364 A.

---------------------------------------------------------
Title: <SUP>81</SUP>Br and <SUP>79</SUP>Br as detectors of solar
    neutrinos
Authors: Bahcall, John N.
1981PhRvC..24.2216B    Altcode:
  Uncertainties in nuclear matrix elements that are important for
  the interpretation of proposed bromine solar neutrino experiments
  are evaluated. Some laboratory measurements that could reduce
  these uncertainties are suggested. The question of what can be
  learned about the interior of the sun by performing a bromine
  solar neutrino experiment is discussed with the aid of neutrino
  absorption cross sections that are calculated using simplifying
  assumptions. RADIOACTIVITY <SUP>79</SUP>Br, <SUP>81</SUP>Br calculated
  neutrino absorption cross sections. <SUP>81</SUP>Kr excited states
  considered.

---------------------------------------------------------
Title: The distribution of stars to V = 16th magnitude near the north
    galactic pole - Normalization, clustering properties, and counts in
    various bands.
Authors: Bahcall, J. N.; Soneira, R. M.
1981ApJ...246..122B    Altcode:
  The distribution on the sky of stars brighter than V= 16 mag near the
  North Galactic Pole is discussed. The available data are reviewed; the
  most important new data are from the catalog of Weistrop. All of the
  data are in agreement with predictions made from our standard Galaxy
  model when the giants are treated separately from the main sequence
  stars. <P />Transformations between different photometric bands,
  including U, B, J, F, V, R, I, g, and r, are given for a wide range
  of stellar types and luminosity classes. The necessary ingredients
  are provided for making color transformations to arbitrary bands that
  may be defined in the future with characteristic wavelengths between
  4000 and 8500 A. Some illustrative applications are made to bands that
  are defined for Space Telescope instruments. <P />The star counts are
  predicted in all of the above listed bands down to 16th magnitude using
  the data of Weistrop with the color corrections of Faber et al. <P
  />The clustering properties of the stars are investigated with the aid
  of the two-point correlation function and the distributions of first
  and second-nearest neighbors, as well as photometric parallaxes. A
  significant fraction (∼15%) of the stars appear to be in binaries
  or triplets with a typical separation of order 0.1 pc.

---------------------------------------------------------
Title: X-ray absorption and the POST - auger decay spectrum of
    multielectronatoms.
Authors: Shapiro, P. R.; Bahcall, J. N.
1981ApJ...245..335S    Altcode:
  Auger ionization frequently leaves an atom in an excited state which
  decays to the ground state by a spontaneous radiative cascade. This
  process has not previously been considered and is potentially important
  as a source of line emission following X-ray absorption. We show that
  the post-Auger decay yields a rich spectrum of UV and optical emission
  lines as a direct signature of the X-ray absorption. <P />Our results
  are applied to some astrophysical problems of interest. We show that
  the direct X-ray-induced emission considered here may contribute to
  the UV line spectra of quasars and Seyfert galaxies, as well as those
  of Galactic compact X-ray sources. We also find that the neutral gas
  responsible for the absorption turnover in the soft X-ray spectrum of
  the Crab Nebula may be a detectable source of neutral oxygen fluorescent
  Kα emission at 0.525 keV if the gas is local to the nebula. The same
  gas should be undetectable in its O III post-Auger decay lines.

---------------------------------------------------------
Title: Methods for determining the masses of spherical
    systems. I. Test particles around a point mass.
Authors: Bahcall, J. N.; Tremaine, S.
1981ApJ...244..805B    Altcode:
  Mass estimators for spherical systems may be based either on the virial
  theorem or on moments of the projected mass q= (projected distance)
  × (radial velocity)<SUP>2</SUP>/G. The statistical characteristics
  of both estimators are derived and discussed for the special case
  of test particles bound to a massive central object. We illustrate
  their relative merits by a series of Monte Carlo experiments. We
  find that the projected mass method is generally more reliable
  than the virial theorem. We apply our results to three systems:
  3C 273, Ml0l, and M3l. The mass of 3C 273 is estimated to be 5 ×
  l0<SUP>13</SUP>h<SUP>-1</SUP> M<SUB>sun</SUB> from radial velocities of
  companion galaxies measured by Stockton. The mass of M101 within ∼400
  kpc is found to be about 2 × l0<SUP>12</SUP> M<SUB>sun</SUB>. The
  mass of M3l within ∼100 kpc is found to be about 1 × 10<SUP>12</SUP>
  M<SUB>sun</SUB>, an order of magnitude larger than given by the virial
  theorem from the same data, but consistent with the optical and 21 cm
  rotation curves.

---------------------------------------------------------
Title: Solar Neutrinos: Present Status
Authors: Bahcall, J.
1981neu1.conf....1B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Neutrinos: Rapporteurs Talk
Authors: Bahcall, J. N.
1981neu2.conf..253B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Guide star probabilities.
Authors: Soneira, R. M.; Bahcall, J. N.
1981NASCR3374.....S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar neutrinos.
Authors: Bahcall, J. N.
1981PrPNP...6..111B    Altcode:
  Studies of solar neutrinos as a tool to understanding the evolution and
  working nuclear processes in the interiors of stars are reviewed. Fusion
  reaction models for stellar interiors are described, noting the
  0.81 MeV proton-proton reaction which produces neutrinos, and the
  Brookhaven experiment designed to study reactions produced by solar
  neutrino capture. A neutrino was posited to be captured by Cl-37
  to yield Ar-37 and an electron. The experiment involved a 400,000
  l tank of perchloroethylene situated 1500 m underground to shield
  from cosmic rays. Insufficient neutrinos were detected to establish a
  distinction from cosmic ray neutrinos. Further experiments comprising
  counting from Ga-71, Rb-87, In-115, and Tl-205 reactions occurring
  from solar proton-proton and proton + electron + H2 + nu reactions are
  outlined, and are shown to be dependent on conservation of electric
  charge. Finally, the detection of stellar collapses is discussed.

---------------------------------------------------------
Title: Guide star probabilities
Authors: Soneira, R. M.; Bahcall, J. N.
1981ias..rept.....S    Altcode:
  Probabilities are calculated for acquiring suitable guide stars (GS)
  with the fine guidance system (FGS) of the space telescope. A number of
  the considerations and techniques described are also relevant for other
  space astronomy missions. The constraints of the FGS are reviewed. The
  available data on bright star densities are summarized and a previous
  error in the literature is corrected. Separate analytic and Monte Carlo
  calculations of the probabilities are described. A simulation of space
  telescope pointing is carried out using the Weistrop north galactic
  pole catalog of bright stars. Sufficient information is presented so
  that the probabilities of acquisition can be estimated as a function of
  position in the sky. The probability of acquiring suitable guide stars
  is greatly increased if the FGS can allow an appreciable difference
  between the (bright) primary GS limiting magnitude and the (fainter)
  secondary GS limiting magnitude.

---------------------------------------------------------
Title: The effects of X-ray absorption on the spectra of distant
    objects.
Authors: Shapiro, P. R.; Bahcall, J. N.
1980ApJ...241....1S    Altcode:
  The X-ray absorption spectrum above 0.1 keV that would be introduced
  into the continuous X-ray spectrum of a quasar by an intervening
  uniform, hot intergalactic gas with a small admixture of atoms of C,
  N, O, Ne, Mg, Si, S and Fe has been calculated in detail. This work is
  relevant to the well-known search for cosmologically distributed missing
  mass. The results indicate that soft X-ray absorption can be appreciable
  for all quasar X-ray sources, from the most distant to the very nearby,
  for a significant range of IGM temperatures, densities, heavy-element
  abundances, and observed photon energies. A brief comparison with
  the preliminary results of the Einstein Observatory quasar sample is
  made. The possibility that gas 'clumped' on noncosmological scales
  produces observable absorption lines and/or edges in quasar X-ray
  spectra is also considered.

---------------------------------------------------------
Title: The Space Telescope Observatory
Authors: Bahcall, J. N.; Odell, C. R.
1980srst.coll....5B    Altcode: 1980IAUCo..54....5B; 1979STIN...8022131B
  A guide to the expected characteristics of the space telescope
  (ST) observatory is presented. The general objectives of the ST
  observatory are summarized. The plans for the development of the
  observatory are described with a brief history of the scientific
  activities; an account of the scope of the present program; a summary
  of the major responsibilities of the contractors; and a list of the
  project milestones are included. The performance characteristics of
  the observatory are provided including the imaging and stray light
  characteristics, pointing capability, and operational access. The
  expected performance characteristics of all six of the first generation
  science instruments are summarized. The mode of operations is described
  which includes a discussion of program options, guide star selection,
  methods of acquisition, and quick look data capabilities.

---------------------------------------------------------
Title: Absorption Lines in the Spectra of Distant Objects
Authors: Bahcall, J. N.
1980srst.coll..215B    Altcode: 1979srst.coll..215B; 1979srst.nasa..215B; 1980IAUCo..54..215B
  Studies that can be carried out with the Space Telescope of absorption
  line systems which may be expected to occur in the spectra of
  distant objects are discussed. The phenomenology of quasar absorption
  line systems is described and the principal suggested explanations
  are summarized. It is proposed that the numerous Ly-alpha systems
  are caused by 'extremely large hydrogenic halos around galaxies or
  clusters of galaxies. Two tests are also described for the origins of
  known absorption systems, the results of which will favor either the
  cosmological or intrinsic hypothesis. Absorption lines that are likely
  to be strongest are listed and a sample observing program is presented.

---------------------------------------------------------
Title: The effect of variability on the V/V-max test
Authors: Bahcall, J. N.
1980ApJ...240..377B    Altcode:
  Knowledge of the distribution of quasars in space has been obtained
  primarily from applications of the V/V-max test to complete flux-limited
  samples of sources. The intrinsic luminosities of many quasars are
  variable. Other objects, such as X-ray or gamma-ray sources, for which
  one might wish to use the V/V-max test are also variable. However,
  previous formulations of the V/V-max test have not included the
  effects of variations. We generalize the V/V-max test to include
  explicitly the effects of variability and estimate the biases that
  can be introduced by the treatment of luminosity variations. Random
  photometric observations have the same effects on the expected value of
  V/V-max as do luminosity variations and are therefore included in the
  discussion. We distinguish between archival identifications (made on
  previously existing photographs) and contemporaneous identifications
  (made at the same time as the basic flux measurements are carried
  out). For contemporaneous identifications, the effects of flux
  variability and broad luminosity function can be avoided entirely by the
  use of density-weighted volumes that are corrected for source evolution.

---------------------------------------------------------
Title: The universe at faint magnitudes. I. Models for the Galaxy
    and the predicted star counts.
Authors: Bahcall, J. N.; Soneira, R. M.
1980ApJS...44...73B    Altcode:
  A detailed model is constructed for the disk and spheroid components
  of the Galaxy from which the distribution of visible stars and mass
  in the Galaxy is calculated. The application of star counts to the
  determination of galactic structure parameters is demonstrated. The
  possibility of detecting a halo component with the aid of star counts
  is also investigated quantitatively. <P />The stellar luminosity
  functions and scale heights are determined from observations in the
  solar neighborhood. The global distribution of matter is assumed,
  based on studies of other galaxies, to be an exponential disk plus a
  de Vaucouleurs spheroid. The spheroid luminosity function is found to
  have the same shape as the disk luminosity function over the range
  of absolute magnitudes (+4 to + 12) that contributes significantly
  to the star counts for m<SUB>V</SUB> ≤ 30. The density of spheroid
  stars in the solar neighborhood is 1/800 of the value for the disk. The
  star counts calculated using the density variation of a de Vaucouleurs
  spheroid are consistent with the available data; the counts predicted
  with the aid of a Hubble law are inconsistent with observations at
  more than the two-sigma level of significance. <P />The variations
  of the calculated star densities with apparent magnitude, latitude,
  and longitude agree well with the available star count data for the
  observationally well studied range of 4 ≲ m<SUB>V</SUB> ≲ 22. The
  calculated (B - V) color distributions are also in good agreement with
  existing data. The color data also indicate that QSOs comprise only a
  few percent of the total number of stellar objects to m<SUB>V</SUB>
  = 22 (m<SUB>B</SUB> = 22.5). The spheroid component is found to be
  approximately spherical. The scale lengths of the Galaxy model and
  computed total luminosity and M/L ratios for the disk and spheroid
  are in agreement with observations of other Sbc galaxies. Illustrative
  Fig. and a table of interesting characteristics (such as the mass and
  luminosity contained within various radii and the escape velocity)
  are provided. <P />Further ground-based observations at attainable
  faint magnitudes (m<SUB>V</SUB> ≤ 23 mag) would be important. Star
  counts and (B - V) colors in several widely separated selected fields
  would permit a more accurate determination of the disk scale length and
  the spheroid star density and ellipticity. The most effective regions
  in which to make these observations are specified. <P />The Galaxy
  model of the disk and spheroid is used to predict the star densities
  (in B and V) that may be observable with the aid of the Space Telescope
  down to very faint magnitudes. The stellar density to m<SUB>V</SUB> =
  28 from the disk and spheroid is predicted to be 10<SUP>4</SUP> stars
  per square degree at the galactic pole. The predicted star counts are
  insensitive to many of the model parameters, although drastic changes in
  the shape of the luminosity function outside the presently determined
  magnitude range could produce measurable departures from the predicted
  star counts at faint magnitudes. <P />The rotation curve computed
  solely from the disk and spheroid components decreases beyond about
  10 kpc from the center of the Galaxy. A halo with even a relatively
  small mass density in the Solar neighborhood (ρ<SUB>Halo</SUB>
  (Sun) = 0.01 M<SUB>sun</SUB> pc<SUP>-3</SUP>) can give rise to a flat
  rotation curve. The stellar content of such a halo would be revealed by
  observations with Space Telescope cameras if the halo consists of main
  sequence stars with M<SUB>V</SUB> ≲ 19.0 mag (existing observations
  imply M<SUB>V</SUB><SUP>MS</SUP> ≳ 14.0 mag) or faint white dwarfs
  with M<SUB>V</SUB><SUP>WD</SUP> ≲ 17.5 mag (existing observations
  imply M<SUB>V</SUB><SUP>WD</SUP> ≳ 13.0 mag). Existing data imply
  (M/L)<SUB>Halo</SUB> ≳650 (Solar Visual units). <P />The results for
  V magnitudes are described in the main text; the corresponding results
  for B magnitudes are summarized in Appendix A. A table of predicted
  differential and integrated star counts for both V and B magnitudes
  is given in Appendix B. Simple formulae that reproduce to an accuracy
  of 15% the predicted model star densities as a function of magnitude,
  latitude, and longitude are also provided in Appendix B.

---------------------------------------------------------
Title: New Solar-Neutrino Flux Calculations and Implications Regarding
    Neutrino Oscillations
Authors: Bahcall, J. N.; Lubow, S. H.; Huebner, W. F.; Magee, N. H.,
   Jr.; Merts, A. L.; Argo, M. F.; Parker, P. D.; Rozsnyai, B.; Ulrich,
   R. K.
1980PhRvL..45..945B    Altcode:
  The results of new calculations of solar-neutrino fluxes are
  presented; the fluxes are obtained from detailed solar models that
  make use of improved opacities and nuclear-physics cross sections. By
  evaluating known uncertainties in the predicted capture rate for the
  <SUP>37</SUP>Cl solar-neutrino experiment, we find that the ratio of
  theoretical to (best-estimate) observed capture rate lies in the range
  4.0 to 2.6. These results constitute a strong constraint on models
  of neutrino oscillations if the entire discrepancy is ascribed to
  neutrino oscillations.

---------------------------------------------------------
Title: The Space Telescope Observatory.
Authors: Bahcall, J. N.; Odell, C. R.
1980JAnSc..28..107B    Altcode:
  The Space Telescope is an international astronomical observatory
  which will be placed into a low earth orbit in December 1983. The
  observatory will provide astronomers the opportunity to use five
  different instruments (wide field/planetary camera, faint object camera,
  high-resolution spectrograph, faint-object spectrograph, and high speed
  photometer), and to do astrometry with the use of the fine guidance
  sensors used primarily for pointing control. These instruments, the
  spectral range available above the earth's atmosphere, and the spatial
  resolution available from the combination of a near-diffraction limited
  94-in. primary mirror and the stability provided by the Pointing Control
  System provide a tremendous potential to the astronomical community.

---------------------------------------------------------
Title: Star counts as an indicator of galactic structure and quasar
    evolution
Authors: Bahcall, J. N.; Soneira, R. M.
1980ApJ...238L..17B    Altcode:
  A detailed model of the stellar content of the Galaxy is described
  briefly. Illustrative applications of the model are made, using
  existing data, to indicate how star counts can be used to determine
  some parameters of galactic structure, to detect a massive (stellar)
  halo, and to constrain models of quasar evolution.

---------------------------------------------------------
Title: On the simultaneous analysis of several complete samples. The
    V/Vmax and Ve/Va variables, with applications to quasars.
Authors: Avni, Y.; Bahcall, J. N.
1980ApJ...235..694A    Altcode:
  Methods are derived for applying the V/Vmax variable when several
  complete samples are analyzed simultaneously. A new, related,
  variable, V(e)/V(a), which is superior to V/Vmax when sufficient
  observational data are available, is introduced. It is shown how
  statistically independent complete samples can be generated from
  partially overlapping samples such that each observed object appears
  only once in the analysis. These methods make it possible to combine the
  information from different complete samples, and to make an efficient
  use of all available data. Illustrative examples for quasars are
  given. It is shown how the generalized V/Vmax and V(e)/V(a) can be
  used to find the amount of cosmological evolution of quasars and its
  associated range of uncertainty.

---------------------------------------------------------
Title: The magnetic dipole model for superluminal radio sources
Authors: Bahcall, J. N.; Milgrom, M.
1980ApJ...236...24B    Altcode:
  The magnetic dipole model (MAD) for superluminal radio sources is
  described in detail. Analytic derivations are presented for a number
  of observationally accessible kinematic quantities, as well as for the
  size and shape of the radio lobes and the probability distributions
  for the velocities. The results are in satisfactory agreement with
  observations. The astrophysical aspects of MAD are discussed assuming
  that the dominant emission mechanism is curvature radiation. The
  possibility that the local radius of curvature of the magnetic field
  is much smaller than the curvature radius of an ideal dipole field is
  considered. The physical effects that are discussed include coherent
  emission and absorption, circular and linear polarization, and inverse
  Compton scattering. The time-dependence of the flux and the shape of
  the spectrum that are deduced on the basis of the assumed emission
  mechanism are consistent with observation.

---------------------------------------------------------
Title: Solar Neutrinos
Authors: Bahcall, J. N.
1980aepc.conf...25B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Effects of X-ray Absorption on the Spectra of Distant
    Objects
Authors: Shapiro, P. R.; Bahcall, J. N.
1979BAAS...11..694S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Models for the Galaxy and the Predicted Star Counts
Authors: Bahcall, J. N.; Soneira, R. M.
1979BAAS...11..706B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Neutrinos: Theory Versus Observation
Authors: Bahcall, John N.
1979SSRv...24..227B    Altcode:
  The current state of the solar neutrino problem is described. The
  predictions of solar models (standard and nonstandard) are reviewed. The
  neutrino absorption cross sections for all detectors of current
  interest are reviewed with special emphasis on the uncertainties that
  exist in the calculations for each target. A long-term program for
  neutrino spectroscopy of the solar interior is outlined. It is shown,
  in addition, that stellar collapses can be detected within the galaxy
  by the proposed solar neutrino detectors.

---------------------------------------------------------
Title: The Effects of X-ray Absorption on the Spectra of Distant
    Objects.
Authors: Shapiro, P. R.; Bahcall, J. N.
1979BAAS...11..778S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Space Telescope Observatory.
Authors: Bahcall, J. N.; Odell, C. R.
1979NASCP2111....5B    Altcode: 1979STIN...7927043B
  The purpose of this review is to provide a convenient guide to the
  expected characteristics of the Space Telescope Observatory for
  astronomers and physicists. The authors have tried to provide enough
  detail so that a professional scientist, observer or theorist, can plan
  how the observatory may be used to further his observing program or to
  test theoretical models. Further detail is available in NASA documents
  that are referenced throughout the report.

---------------------------------------------------------
Title: Absorption lines in the spectra of distant objects.
Authors: Bahcall, J. N.
1979NASCP2111..215B    Altcode:
  The author discusses studies that can be carried out with the Space
  Telescope of absorption-line systems which may be expected to occur
  in the spectra of distant objects.

---------------------------------------------------------
Title: Solar neutrino experiments
Authors: Bahcall, John N.
1978RvMP...50..881B    Altcode:
  New results are presented for absorption cross sections of nine
  possible detectors of solar neutrinos (<SUP>7</SUP>Li, <SUP>37</SUP>Cl,
  <SUP>51</SUP>V, <SUP>55</SUP>Mn, <SUP>71</SUP>Ga, <SUP>81</SUP>Br,
  <SUP>87</SUP>Rb, <SUP>115</SUP>In, and <SUP>205</SUP>Tl). Special
  attention is given to nuclear physics uncertainties. The calculated
  cross sections are used (with the aid of illustrative solar models
  and ad hoc assumptions about neutrino propagation) to discuss what
  can be learned about the sun or weak interactions from each of the
  nine suggested solar neutrino experiments. An experimental program
  for neutrino spectroscopy of the solar interior is outlined. It is
  shown in addition that stellar collapses can be detected to typical
  distances of several kpc (kiloparsecs) by the proposed <SUP>7</SUP>Li,
  <SUP>37</SUP>Cl, and <SUP>115</SUP>In solar neutrino detectors (provided
  that electron neutrinos do not decay or oscillate).

---------------------------------------------------------
Title: Apparent superluminal expansion velocities in the dipole
    magnetic field model
Authors: Milgrom, M.; Bahcall, J. N.
1978Natur.274..349M    Altcode:
  Observations of compact radio sources conducted with very long baseline
  interferometry methods have shown that the components of some radio
  sources seem to move apart with relative velocities more than twice
  the speed of light. A model for compact extragalactic radio sources
  presented by Sanders is considered (1974). In this model apparent
  superluminal expansion arises naturally and radiating particles move
  at relativistic velocities along dipole magnetic field lines. Sanders
  discusses the relationship of this proposal to other explanations
  of superluminal velocities in compact radio sources. However, he
  incorrectly evaluated the consequences of the dipole field model,
  obtaining results both for the magnitude of the expansion velocity
  and its time dependence that are in conflict with observations. An
  investigation is conducted in which the valid geometrical consequences
  of the model are presented. It is shown that these consequences agree
  with available observations.

---------------------------------------------------------
Title: Proposed solar-neutrino experiment using <SUP>71</SUP>Ga
Authors: Bahcall, J. N.; Cleveland, B. T.; Davis, R., Jr.; Dostrovsky,
   I.; Evans, J. C., Jr.; Frati, W.; Friedlander, G.; Lande, K.; Rowley,
   J. K.; Stoenner, R. W.; Weneser, J.
1978PhRvL..40.1351B    Altcode:
  A solar-neutrino experiment that uses <SUP>71</SUP>Ga as a detector can
  distinguish between broad classes of explanations for the discrepancy
  between prediction and observation in the <SUP>37</SUP>Cl experiment. A
  radiochemical experiment with the required amount of <SUP>71</SUP>Ga
  is feasible.

---------------------------------------------------------
Title: The Hubble diagrams for quasars.
Authors: Bahcall, J. N.; Turner, E. L.
1978PhyS...17..353B    Altcode:
  The optical Hubble diagram for a complete sample of 112 quasars is
  constructed for q(0) = 1. With no correction for selection effects,
  the Hubble diagram shows a strong correlation of magnitude with
  redshift (slope 4.43 plus or minus 0.44; correlation coefficient
  of 0.956). These uncorrected results place an interesting limit on
  luminosity evolution. The optical and radio Hubble diagrams are also
  discussed after applying the proper corrections for selection effects.

---------------------------------------------------------
Title: On the origin of quasar absorption lines.
Authors: Bahcall, J. N.
1978PhyS...17..229B    Altcode:
  Many predictions have been made on the basis of the cosmological
  hypothesis for the origin of quasar absorption lines. The observational
  evidence relating to these predictions is summarized. It appears likely
  that many of the observed absorption lines originate in material that
  is separated from the emitting quasar by cosmological distances. Two
  special problems are briefly discussed: the interpretation of redshift
  splittings and the origin of absorption redshifts larger than their
  associated emission redshifts.

---------------------------------------------------------
Title: X-ray line spectroscopy for clusters of galaxies. I.
Authors: Bahcall, J. N.; Sarazin, C. L.
1978ApJ...219..781B    Altcode:
  Theoretical models for the intracluster gas in X-ray clusters of
  galaxies are studied. The limits of validity of all the published models
  are derived from self-consistent arguments and existing data. Results
  are presented for the well model (gas trapped in the potential well
  of a single galaxy) and the wind model. A scaling law is proved that
  allows one to apply the results calculated for spherical systems to the
  nonspherical groupings that are often observed. The particular line
  intensities that can best be used to discriminate among theoretical
  models or to diagnose the gas (i.e., determine abundances, temperatures,
  ionization state, and other properties) are listed along with the
  required experimental sensitivity and resolution. Possible observing
  programs are described that can be carried out with existing instruments
  on currently operating satellites and with future space experiments
  (e.g., on HEAO-A, HEAO-B, and other planned X-ray missions).

---------------------------------------------------------
Title: Theoretical Introduction to the <SUP>37</SUP>Cl Solar Neutrino
    Experiment
Authors: Bahcall, J. N.
1978sfsn.conf...55B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Masses of neutron stars and black holes in X-ray binaries.
Authors: Bahcall, J. N.
1978ARA&A..16..241B    Altcode:
  A coherent summary is presented of the methods used to determine
  the masses of X-ray sources in binary systems, and the presently
  available results are described. The elements of the analysis are
  considered, taking into account X-ray and optical mass functions,
  the equipotential surfaces of the optical primaries, eccentric orbits,
  X-ray eclipse durations, rotational velocities of the optical primaries,
  and ellipsoidal light variations. The mass determinations are discussed
  for six X-ray sources in binary systems which have been extensively
  studied. The systems include 3U 0900-40, SMC X-1, Cen X-3, Her X-1,
  3U 1700-37, and Cyg X-1.

---------------------------------------------------------
Title: Theoretical Introduction to the <SUP>37</SUP>CI Solar-neutrino
    Experiment
Authors: Bahcall, J. N.
1978ComAp...8...37B    Altcode: 1978STIA...7924515B
  At the present time, within the framework of the observational
  information about stars, only the Cl-37 experiment is clearly
  inconsistent with the standard theory of stellar evolution. With a
  minimum of technical detail and calculations, the author tries to
  explain the relevance of the Cl-37 experiment to theories of stellar
  evolution and nuclear-energy generation. The basic neutrino-producing
  p-p reaction and the pep line are reviewed, and their role in a typical
  solar model is explained. The expected flux of solar neutrinos is
  about 5 SNU for the standard theory of stellar evolution. In any case,
  it predicts too large a B-8 flux.

---------------------------------------------------------
Title: Optical properties of binary X-ray sources
Authors: Bahcall, J. N.
1978pans.proc...63B    Altcode:
  The paper attempts to summarize in a convenient form the present
  state of experimental knowledge on the optical properties of binary
  X-ray sources, and to draw attention to the most important problems in
  which observational progress can be made with current techniques. The
  basic observational techniques which have been applied to this study
  are described, including spectroscopic classification, photometry,
  IR measurements, and polarization measurements. Attention is given
  to the following systems: Cygnus X-1/HDE 226868; Cen X-3; Sanduleak
  160/SMC X-1; Hz Herculis/Her X-1; V 818 Sco/Sco X-1; Cygnus X-3;
  HD 77581/Vela XR-1; and HD 153919/3U 1700-37.

---------------------------------------------------------
Title: Capture Rates for Various Solar Neutrino Detectors
Authors: Bahcall, J. N.
1978sfsn.conf..223B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar neutrinos
Authors: Bahcall, J. N.
1977AIPC...37...53B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A Model for Superluminal Radio Sources
Authors: Bahcall, J. N.; Milgrom, M.
1977BAAS....9..586B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Neutrino absorption cross sections for <SUP>37</SUP>Cl with
    applications.
Authors: Bahcall, J. N.
1977ApJ...216L.115B    Altcode:
  Neutrino absorption cross sections for Cl-37 are
  calculated. Applications are made to problems involving solar neutrinos,
  collapsing stars, and the cosmic neutrino mass density. The present
  Brookhaven experiment can detect stellar collapses as far away as 5
  kpc for plausible collapse parameters.

---------------------------------------------------------
Title: On the Zeeman splitting of X-ray lines by neutron-star
    magnetic fields.
Authors: Sarazin, C. L.; Bahcall, J. N.
1977ApJ...216L..67S    Altcode:
  In the strong magnetic fields usually assumed to exist near neutron
  stars (of the order of 100 billion to 10 trillion gauss), X-ray emission
  lines may exhibit easily detected Zeeman splitting (at least when the
  field in the emission region does not exceed approximately 500 billion
  gauss). Detection of this splitting would allow a direct measurement of
  the neutron-star magnetic-field strength. The observed Zeeman pattern
  would determine the direction of the magnetic field; in an oblique
  rotator, the pattern would alternate with the pulsar period.

---------------------------------------------------------
Title: The star distribution around a massive black hole in a globular
    cluster. II. Unequal star masses.
Authors: Bahcall, J. N.; Wolf, R. A.
1977ApJ...216..883B    Altcode:
  The steady-state distribution of stars around a massive black hole in
  a globular cluster is determined by solving numerically the coupled
  time-dependent Boltzmann equations for a system containing stars of
  two different masses. Similar results are found for an arbitrary
  spectrum of masses with the aid of approximate analytic solutions
  of the time-independent equations. The effects of mass segregation
  are summarized by scaling laws that are derived both by analytic
  approximations and by numerical solutions. The detectability of a
  black hole in a globular cluster is discussed in terms of possible
  observations of the central star distributions.

---------------------------------------------------------
Title: X-ray line emission for clusters of galaxies. II. Numerical
    models.
Authors: Sarazin, C. L.; Bahcall, J. N.
1977ApJS...34..451S    Altcode:
  The predicted X-ray spectra of clusters of galaxies have been calculated
  assuming that the X-ray emission arises from hot intracluster gas in
  collisional ionization equilibrium. An extensive grid of models is
  presented for isothermal models, polytropic hydrostatic models, and
  wind models. The integrated X-ray spectrum is given for each model,
  including line and recombination radiation. The intensities of satellite
  lines due to dielectronic recombination and inner-shell excitation are
  also presented; these satellites can be used to derive the temperature
  and ionization state of the gas. The projected distributions on the
  sky of continuum X-ray intensity, line strengths and line widths, and
  the satellite intensities are given as a function of projected radius
  from the cluster center. The predicted microwave diminution has been
  calculated as a function of cluster position. The observable X-ray
  emission properties scale simply with cluster parameters; relations
  are given for deriving the predicted X-ray properties from other
  observations.

---------------------------------------------------------
Title: On the mass determination of Hercules X-1.
Authors: Bahcall, J. N.; Chester, T. J.
1977ApJ...215L..21B    Altcode:
  Middleditch and Nelson (1976) obtained a value of 1.30 + or - 0.14
  solar masses for the mass of Her X-1 on the basis of the observed
  frequencies of the optical pulsations due to absorption, reprocessing,
  and reemission of pulsed X-ray energy from the surface of HZ Her. A
  more conventional estimate of the uncertainty in the mass inferred for
  Her X-1 from the cited optical-pulsation data is computed using those
  data in combination with a simple geometrical model for the optical
  pulsations and Uhuru X-ray observations of the mass function and the
  half-angle of the eclipse duration of the HZ Her/Her X-1 system. It
  is assumed that the surface of HZ Her is an equipotential surface of
  the restricted three-body potential and that HZ Her just fills its
  critical equipotential. The allowed ranges of masses obtained are 0.6
  to 2.0 solar masses for Her X-1 and 1.6 to 2.7 solar masses for HZ
  Her. It is found that the calculated mass of Her X-1 is especially
  sensitive to the unknown rotational velocity of HZ Her.

---------------------------------------------------------
Title: Parameters and predictions for the X-ray emitting gas of Coma,
    Perseus, and Virgo.
Authors: Bahcall, J. N.; Sarazin, C. L.
1977ApJ...213L..99B    Altcode:
  The range of acceptable models for the intracluster gas in the Coma,
  Perseus, and Virgo clusters is determined from previous observations of
  the spectrum, intensity, and size of the cluster X-ray sources. Standard
  hydrostatic, wind, and inflow models are considered. For Virgo, a 'well'
  model is proposed in which the gas is trapped in the gravitational
  potential of M87, assumed to be very massive and extended. The iron
  abundance in the intracluster gas is determined from the observed
  strength of the 7-keV line feature; the required abundances for
  all models and all clusters are approximately equal and solar in
  value. The similarity of the abundances derived for these three clusters
  suggests that the line emission probably arises from the intracluster
  gas. Predictions are given for the cosmic microwave diminution and the
  dependence of X-ray size on observed energy for acceptable models for
  the intracluster gas.

---------------------------------------------------------
Title: The Hubble Diagrams for Quasars
Authors: Bahcall, J. N.; Turner, E. L.
1977IAUS...74..295B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Circumstellar matter in the binary V Puppis.
Authors: York, D. G.; Flannery, B.; Bahcall, J.
1976ApJ...210..143Y    Altcode:
  Results are reported for Copernicus observations of the double-lined
  binary V Puppis in the wavelength region from 1155 to 1310 A with a
  resolution of 0.2 A. The sharp-lined UV absorption spectrum is found
  to provide a line of sight dominated by an apparently 'textbook'
  H II region in a Stromgren sphere surrounding the stars. Several
  characteristics of this H II region are deduced by analyzing absorption
  features arising from excited fine-structure states of N II and Si
  II. Evidence is given for the presence of a normal interstellar H
  I region containing H2 and a separate H I region which could be the
  transition zone of the H II region. A possible blueshifted N V feature
  is noted in absorption. It is suggested that the H(+) emission measure
  and a characteristic size and shape for the H II region can probably
  be determined by optical observations of Balmer recombination lines
  within about 1 deg of V Puppis.

---------------------------------------------------------
Title: The sun's missing particles
Authors: Bahcall, J. N.
1976NatH...85...76B    Altcode:
  Attention is focused on the theoretical puzzle and crisis in solar
  physics provoked by discrepancies between results of the Davis-Evans
  neutrino trap experiment and theoretical predictions. The importance
  of neutrinos in current theory on the sun's heat production mechanisms
  (including sustained thermonuclear fusion as energy source) is explained
  and the Davis-Evans Brookhaven neutrino detector is described. A
  computer model of the solar interior is sketched. Conjectures advanced
  to challenge existing theory and account for the anomalous neutrino
  evidence are sketched (thermonuclear fusion reactions downgraded; black
  hole at center of sun; lower estimate of temperature of solar interior;
  higher content of heavy elements in solar interior; extremely high
  central magnetic fields; immiscibility of hydrogen and helium below
  some critical temperature; neutrino decay by unknown modes)

---------------------------------------------------------
Title: Star distribution around a massive black hole in a globular
    cluster.
Authors: Bahcall, J. N.; Wolf, R. A.
1976ApJ...209..214B    Altcode:
  The distribution of solar-mass stars around a massive black hole
  in a globular star cluster is investigated using a basic physical
  picture in which stars in bound orbits in the gravitational potential
  well of the black hole diffuse from one bound orbit to another via
  star-star gravitational scattering. Detailed expressions are derived
  for the relevant diffusion coefficients, the time-dependent Boltzmann
  equation is solved numerically, and solutions are found which satisfy
  the boundary conditions at both zero and large binding energy. The
  results indicate that the distribution function is approximately a
  power law throughout most of the black hole's gravitational well,
  that stars in bound orbits diffuse slowly down the gravitational well
  under equilibrium conditions, and that a black hole of less than or
  approximately 1000 solar masses may accrete stars primarily by capture
  from unbound orbits. Several methods for detecting massive black holes
  in cores of globular clusters are discussed along with expected large
  statistical fluctuations close to the black hole and the possible
  relevance of various stellar accretion processes for globular-cluster
  X-ray sources.

---------------------------------------------------------
Title: Search for X-ray emission from globular clusters using
    Uhuru data.
Authors: Ulmer, M. P.; Murray, S. S.; Gursky, H.; Bahcall, J. N.
1976ApJ...208...47U    Altcode:
  We searched the Uhuru data for X-ray emission from 40 globular
  clusters. We were unable to extend the list of known globular cluster
  X-ray sources (NGC 1851, 6440, 6441, 6624, and 7078). Our 3 a upper
  limits ranged from 2 x 10 ergs 1 to 1036 ergs 1 (2-10 keV). Subject
  headings: clusters: globular - X-rays: sources

---------------------------------------------------------
Title: X-ray pulses from globular clusters
Authors: Bahcall, J. N.; Ostriker, J. P.
1976Natur.262...37B    Altcode:
  GIANT X-ray pulses have been observed recently by several
  groups<SUP>1-7</SUP> from sources located in a number of celestial
  positions. Two of these sources may plausibly be identified with
  the globular cluster X-ray sources: NGC6624 and NGC1851. In several
  cases<SUP>2,7</SUP> the pulses seem to occur in approximately periodic
  sequences; in other sources the intervals are irregular, but in one case
  there is a relation between pulse strength and interpulse interval. The
  non-burst behaviour of globular cluster X-ray sources has been
  interpreted<SUP>8,9</SUP> in terms of massive (≳ 10<SUP>3</SUP>Msolar)
  black holes powered by accretion from a disk supplied by cluster gas. We
  suggest here that compact stars bound to the central massive black
  hole and orbiting through the accretion disk may produce, by several
  possible mechanisms, giant pulses. These pulses might be expected to
  exhibit a variety of types of X-ray behaviour corresponding to the
  uncertain characteristics (for example, density and spatial extent)
  of the individual accretion disks at the different points at which the
  orbits of the bound compact stars intersect the disks. We note that
  there may be more than one class of sources of giant X-ray bursts and
  that our speculation refers only to those sources in globular clusters.

---------------------------------------------------------
Title: X-ray Sources in Globular Clusters
Authors: Bahcall, John
1976BAAS....8R.442B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Energy Transport in the Solar Interior
Authors: Katz, J. I.; Bahcall, J. N.
1976BAAS....8..320K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Models for X-Ray Line Emission from Clusters of Galaxies
Authors: Bahcall, J. N.; Sarazin, C. L.
1976BAAS....8..355B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Her X-1 panel.
Authors: Bahcall, J. N.
1976NASSP.389...99B    Altcode: 1976NASSP.589...99B
  No abstract at ADS

---------------------------------------------------------
Title: Is the local supercluster a physical association?
Authors: Bahcall, J. N.; Joss, P. C.
1976ApJ...203...23B    Altcode:
  A quantitative measure of the degree of concentration of a sample
  of galaxies toward any great circle is described and applied to the
  Shapley-Ames and de Vaucouleurs catalogs of bright galaxies as well
  as to computer-simulated catalogs of galaxies. It is found that the
  observed distribution can be explained as the combined result of
  obscuration by our Galaxy, purely local clustering on angular scales
  of less than about 10 deg, and our proximity to a rather large and
  populous cluster, the Virgo cluster. In order for this interpretation
  to be correct, the Virgo cluster must have a mean angular radius of the
  order of or greater than 15 deg. This interpretation is supported by
  recent measurements which do not indicate any large inhomogeneities
  in the motions of nearby galaxy clusters and which show that the
  mean recessional velocity of the Virgo cluster is consistent with a
  uniform Hubble expansion. If the present interpretation is correct,
  it may be possible to determine the Hubble constant directly from
  measurements of individual distance indicators (such as H II regions
  and the brightest stars) with distance moduli less than about 32.

---------------------------------------------------------
Title: Status of the study of ellipsoidal light variations in 3U
    0900-40 and other X-ray binaries.
Authors: Avni, Y.; Bahcall, J. N.
1976NASSP.389..615A    Altcode: 1976NASSP.589..615A; 1976xrbi.nasa..615A
  Estimates of system parameters and component masses are reviewed. The
  mass for the X-ray source in 3U0900-40 is found. The importance of
  determining the X-ray eclipse duration in binary systems is explained. A
  list of important observations for testing and utilizing the standard
  picture is presented.

---------------------------------------------------------
Title: Solar Neutrinos: A Scientific Puzzle
Authors: Bahcall, John N.; Davis, Raymond, Jr.
1976Sci...191..264B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Masses for Vela X-1 and other X-ray binaries.
Authors: Avni, Y.; Bahcall, J. N.
1975ApJ...202L.131A    Altcode:
  A detailed analysis of the optical light curve and other previously
  known observations of the X-ray binary Vela X-1 (3U 0900-40) is
  reported. All constraints are consistent only with a projected orbital
  velocity of the X-ray source of between 200 and 300 km/s. The allowed
  ranges of the masses and other parameters are estimated. If the mass of
  the X-ray source is less than the Chandrasekhar limit for white dwarfs,
  then the optical star must have an unusually small mass-to-radius
  ratio for its spectral type. The importance of the X-ray eclipse
  duration in determining binary parameters is emphasized, and some
  results are presented from analyses of observations of 3U 1700-37 and
  other X-ray binaries.

---------------------------------------------------------
Title: Splittings in quasar absorption lines.
Authors: Bahcall, J. N.
1975ApJ...200L...1B    Altcode:
  It is shown that the apparent constancy of the splitting between
  quasar absorption lines observed by Boksenberg and Sargent could be
  understood if the typical velocity in the absorbing material were
  somewhat less than the observing resolution (estimated to be 100 km
  per sec). If this interpretation were correct, then there should be
  many more redshifts that are split with velocity separations that are
  less than 100 km per sec than have been so far observed at velocity
  separations of the order of 150 km per sec. The above conclusions are
  independent of whether or not the absorption lines originate close to,
  or very far away from, the quasar. Some results are presented for a
  specific model in which the splittings are supposed due to absorption
  in halos or clouds surrounding galaxies or small groups of galaxies
  and some tests of this model are suggested. The model parameters are
  consistent with recent radio observations of H I clouds or halos that
  extend far from their parent galaxies.

---------------------------------------------------------
Title: The unidentified high galactic latitude X-ray sources: bright
    galaxies or rich clusters?
Authors: Bahcall, J. N.; Bahcall, N. A.
1975ApJ...199L..89B    Altcode:
  Positional correlations are analyzed among the 51 unidentified
  high-galactic-latitude X-ray sources in the third Uhuru catalog,
  all 2712 rich clusters of galaxies in the Abell catalog, and all
  bright galaxies in the Zwicky catalog. Computer-simulated Uhuru
  catalogs are used to evaluate the chance coincidence rate as well as
  its dispersion, and the validity is confirmed of practically all the
  previously suggested identifications of 3U sources with nearby rich
  Abell clusters. It is shown that one or two of the distance-group 4
  Abell clusters may be associated with 3U sources and that very few,
  if any, of the 3U sources are associated with the most distant Abell
  clusters. On this basis, an upper limit to the X-ray luminosity
  is established which is in agreement with the highest such value
  observed for nearby clusters. Although about 50% of the source error
  boxes contain a bright Zwicky galaxy, very few valid identifications
  are expected.

---------------------------------------------------------
Title: Optical studies of 10 high galactic latitude X-ray sources.
Authors: Bahcall, J. N.; Bahcall, N. A.; Murray, S. S.; Schmidt, M.
1975ApJ...199L...9B    Altcode:
  Optical studies are reported for a representative sample of 10
  unidentified high galactic latitude X-ray sources that are north of
  declination minus 25 deg and that have 3U error boxes less than or of
  the order of 0.5 square degrees. The source 3U 1410-03 is identified
  with a peculiar emission-line spiral galaxy, NGC 5506, and a distance
  group 4 rich cluster of galaxies, Abell 2142, is suggested as a
  possible identification for 3U 1555+27. It is shown that very few
  of the unidentified high galactic latitude sources are quasi-stellar
  sources brighter than 17.5 mag, although one possible X-ray quasar,
  NAB 0137-01, is reported.

---------------------------------------------------------
Title: Massive black holes in globular clusters.
Authors: Bahcall, J. N.; Ostriker, J. P.
1975Natur.256...23B    Altcode:
  It is proposed that the observed X-ray emission in globular star
  clusters may be caused by the accretion of gas onto a massive black
  hole at the center of a cluster. The amount of accreting gas is
  estimated for a model cluster together with the minimum black hole
  mass and the X-ray luminosity. It is shown that the X-ray emission
  should be pointlike and located at the center of the cluster, and that
  there should be no eclipses and no orbital or spin periods observed
  in the X-ray flux. Possible explanations are considered for the model
  limitation that only a small fraction of the globular clusters in the
  galaxy are X-ray sources.

---------------------------------------------------------
Title: Copernicus - X-ray observations of 3U 9759-49.
Authors: Bahcall, J. N.; Charles, P. A.; Davison, P. J. N.; Sanford,
   P. W.; Kellogg, E.; York, D.
1975MNRAS.171P..41B    Altcode:
  Possible associations between the weak X-ray source 3U 0750-49
  and bright variable stars are investigated using X-ray data from
  the Copernicus satellite on V Pup and HD 64740, two bright variable
  stars within the Uhuru error box for 3U 0750-49. Analysis of the data
  indicates that the X-ray source is almost certainly closer to V Pup
  than to HD 64740, and the latter object is completely ruled out as
  a possible candidate. An error box is derived which is perpendicular
  to the Uhuru error box and of similar dimensions. Based on both error
  boxes, the variable stars most likely to be the X-ray source are found
  to be V Pup, CN Pup, and CSV 1199.

---------------------------------------------------------
Title: Ellipsoidal light variations and masses of X-ray binaries.
Authors: Avni, Y.; Bahcall, J. N.
1975ApJ...197..675A    Altcode:
  The ellipsoidal light curves of four binary X-ray systems (HDE
  226868/Cyg X-1, Sk 160/ SMC X-1, Krzeminski's star/Cen X-3, and HZ
  Her/Her X-1) are analyzed assuming that the light variations are caused
  by gravitational and limb-darkening effects on a tidally distorted
  star. Some uncertainties regarding the validity of this interpretation
  are discussed, including departures from repeatability in the light
  curve and from corotation, the effects of heating and reflection, and
  the possibility that the primary is inside the Roche lobe. Numerical
  calculations of light curves show that Cyg X-1 can be either a black
  hole or a normal early-type star with a mass not less than 9 solar
  masses; the mass of SMC X-1 is about 2.3 solar masses, close to the
  upper limit for a nonrotating neutron star; and the mass of Cen X-3
  is between 0.6 and 1.1 solar masses. No significant constraints could
  be derived from the available data for Her X-1.

---------------------------------------------------------
Title: The Star Distribution in M15
Authors: Bahcall, J. N.; Bahcall, N. A.; Weistrop, D.
1975ApL....16..159B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Further optical observations of HZ Herculis.
Authors: Bahcall, J. N.; Bahcall, N. A.; Herczeg, T. J.; Joss, P. C.;
   Leibowitz, E. M.; Segalovitz, A.; Stolero, S.; Véron, M.; Véron,
   P.; Wehinger, P. A.; Weistrop, D.; Wyckoff, S.
1975PASP...87..141B    Altcode:
  Optical observations of HZ Her made in the spring and summer of 1973
  are presented. Some of the observations are practically coincident
  with estimated turn-on times for Her X-1 and others are simultaneous
  with X-ray observations made using the Copernicus satellite. Eight
  magnitudes were also measured from old plates for the epoch 1953-60;
  these measurements confirm the long-term variations for that epoch
  reported by Jones, Forman, and Liller (1973). An interesting theoretical
  explanation by Fabian, Pringle, and Rees (1973) for the persistence
  of large optical variations throughout the 35-day X-ray period is
  ruled out by simultaneous UHURU (X-ray) and Wise Observatory (optical)
  observations.

---------------------------------------------------------
Title: Some remarks on solar neutrinos.
Authors: Bahcall, J. N.
1975ucyr.conf..131B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Some properties of X-ray binaries
Authors: Bahcall, J. N.
1975xris.conf..147B    Altcode:
  Three questions are discussed regarding the optically identified
  binary X-ray sources HZ Her/Her X-1, Krzeminski/Cen X-3, and HDE
  226868/Cyg X-1: (1) the origin of the observed periodicities, (2) the
  estimated masses of the unobserved secondaries, and (3) the nature
  of the secondaries. The main observational properties and principal
  characteristics of the sources are summarized, their periodicities
  are analyzed, and it is suggested that rotation may be responsible for
  the periodicities. Ways to estimate the masses in the present systems
  are described, and approximate values are given for the masses of
  both components in each system. It is shown that Her X-1 and Cen X-3
  are probably neutron stars and that Cyg X-1 must be either a normal
  (nondegenerate) star or a black hole.

---------------------------------------------------------
Title: Solar neutrinos: A scientific puzzle.
Authors: Bahcall, J. N.; Davis, R., Jr.
1975PhyBl..31..609B    Altcode: 1975PhB....31..609B
  No abstract at ADS

---------------------------------------------------------
Title: Optical and near infrared observations of seven fields
    containing X-ray sources
Authors: Bahcall, J. N.; Bahcall, N. A.
1975xris.conf..535B    Altcode:
  Optical and near-IR observations are reported for seven fields
  containing strong, variable X-ray sources with small error boxes located
  near the galactic center. The sources include 3U 1709-23, 1728-24,
  1735-28, 1758-25, 1758-20, 1811-17, and 1837+04. The observational
  methods are described, and limits of detectability are estimated for
  various assumed models of optical counterparts. Two objects are found
  which are possible optical counterparts for 3U 1709-23 and 1728-24. It
  is noted that none of the fields contained stars within the estimated
  detectability limits which exhibited large variations during the period
  of observation.

---------------------------------------------------------
Title: Review of Publications: The Redshift Controversy
Authors: Field, George B.; Arp, Halton; Bahcall, John N.
1974JRASC..68..276F    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Neutral currents and stellar cooling
Authors: Bahcall, J. N.; Treiman, S. B.; Zee, A.
1974PhLB...52..275B    Altcode:
  If weak neutral currents couple with the strengths suggested by
  recent experiments, then stellar cooling via neutrino pair emission
  from thermally excited nuclear states may be significant in white
  dwarfs with central temperature &lt;~10<SUP>8°</SUP> K. At higher
  temperatures, other neutrino cooling processes are more important. In
  the sun, the decay of thermally excited <SUP>57</SUP>Fe nuclei may
  produce a moderately large, but probably unobservable, low-energy
  flux of ν<SUB>μ</SUB>, g¯n<SUB>μ</SUB>, ν<SUB>e</SUB>, and
  g¯n<SUB>e</SUB> neutrinos. <P />Alfred P. Sloan Foundation Fellow.

---------------------------------------------------------
Title: Mass Limits for the Centaurus X-3 System
Authors: Avni, Y.; Bahcall, J. N.
1974ApJ...192L.139A    Altcode:
  Constraints on the mass of Cen X-3 based on the observed amplitude of
  the optical light curve are discussed. A 2 sigma lower limit of 0.6
  solar mass is derived, assuming corotation and the interpretation of the
  ellipsoidal light variations as caused by gravity- and limb-darkening
  effects. Including the constraints imposed by the eclipse duration,
  it is found that the mass of Cen X-3 is equal to 0.6 to 1.1 solar mass,
  while the mass of its optical companion is equal to 16.5 to 18.5 solar
  masses. The sensitivity of the derived masses to the assumed geometry
  is demonstrated.

---------------------------------------------------------
Title: Optical properties of HZ Herculis.
Authors: Bahcall, J. N.; Joss, P. C.; Avni, Y.
1974ApJ...191..211B    Altcode:
  The optical properties of HZ Her are analyzed, and several parameters of
  the Her X-1-HZ Her binary system are estimated. The phase agreement of
  the X-ray and optical variations, the dependence of the average optical
  luminosity upon the 35-day X-ray cycle, and the energy budget of the
  optical variations are studied, using recent observational data. The
  period, amplitude, and phase of the small-scale optical light variations
  found by Jones et al. during times of extended optical inactivity are
  also investigated. The light curve and the radial-velocity variations
  of HZ Her are analyzed, using several simple models for the brightness
  distribution across the face of the star. The masses of Her X-1 and
  HZ Her are estimated by four different methods. Subject headings:
  binaries - stars, individual - X-ray sources

---------------------------------------------------------
Title: Short-time optical variability of X-ray sources.
Authors: Avni, Y.; Bahcall, J. N.
1974ApJ...191..221A    Altcode:
  A formalism for interpreting the short-time optical variability caused
  by X-ray heating in variable X-ray sources is presented and applied
  to the following systems: Her X-1, Cen X-3, Cyg X-1, 2U 0900-40, 2U
  1700-37, Sco X-1, and Cyg X-2. It is shown that the observed upper
  limit of 0.03 percent to regular optical pulsations from HZ Her can be
  understood if the time to convert X-ray energy to emitted optical light
  is of the order of 10 seconds or longer. An upper limit of 3 percent is
  derived for any rapid optical variability from the optical companions
  of 2U 0900-40, 2U 1700-37, and Cyg X-1; the expected fluctuations
  of optical light from HDE 226868 are less than 3 x 10- if the X-ray
  variability of Cyg X-1 has a shot-noise character. Subject headings:
  variable stars - X-ray sources

---------------------------------------------------------
Title: Faint envelopes of galaxies.
Authors: Kormendy, J.; Bahcall, J. N.
1974AJ.....79..671K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Multiple Star Systems and X-Ray Sources
Authors: Bahcall, J. N.; Dyson, F. J.; Katz, J. I.; Paczynski, B.
1974ApJ...189L..17B    Altcode:
  Two classes of triplestar models are proposed X-ray sources of the type
  of Cygnus X-1 to be interpreted without invoking a black hole. The large
  mass which is usually assigned to the X-ray source Cyg X-1 belongs in
  the models to a normal star. Subject headings: binary stars - black
  holes - stellar dynamics - X-ray sources

---------------------------------------------------------
Title: Upper Limit on 2.5-SECOND Pulsations from Hercules X-1
Authors: Avni, Y.; Bahcall, J. N.; Joss, P. C.; Lamb, D. Q.; Schreier,
   E.; Tananbaum, H.
1974ApJ...188L..35A    Altcode:
  No pulsed power is detected with a period of 2.5 seconds in the 1972
  January Uhuru observations of Her X-1. An upper limit of 7 percent
  is derived for the amount of 2.5-s pulsed modulation relative to the
  observed amount of 1. pulsed modulation (corresponding to an upper limit
  of 5 X 1(h for the ratio of signals in the power spectrum). Subject
  headings: binaries - collapsed stars - neutron stars - pulsation -
  X-ray sources

---------------------------------------------------------
Title: Near Infrared Observations of Cygnus X-3
Authors: Bahcall, John N.
1974Natur.247..446B    Altcode:
  THE system known as Cygnus X-3 has been extensively studied at radio
  wavelengths (where it exhibits extraordinary variability<SUP>1-3</SUP>),
  in X rays (where it exhibits a 4.8 h period<SUP>4-6</SUP>),
  and in the infrared at 1.6 and 2.2 µm (where it also displays
  a 4.8 h period as well as large flares<SUP>7,8</SUP>). Attempts
  have also been made to detect Cyg X-3 in visual and near infrared
  wavelengths<SUP>9,10</SUP>. Here we present the results of a series of
  observations made at near infrared wavelengths, λ<SUB>effective</SUB>
  ~=0.85 µm on ten nights in July and August 1973.

---------------------------------------------------------
Title: Some properties of X-ray binaries.
Authors: Bahcall, J. N.
1974ucyr.conf..343B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The redshift controversy. Papers from a symposium, Washington,
    D.C., December 1972.
Authors: Field, G. B.; Arp, H.; Bahcall, J. N.
1974rcpf.book.....F    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Close Pairs of QSOs
Authors: Bahcall, John N.
1974Natur.247...22B    Altcode:
  IT has recently been argued<SUP>1,2</SUP> that the observation of
  close pairs of QSOs with very different redshifts provides support
  for non-cosmological explanations of the redshifts. We show in this
  note that the pairs observed so far may be comfortably explained as
  random coincidences and that the small probabilities that are often
  quoted depend on the use of a posteriori statistics.

---------------------------------------------------------
Title: Optical properties of binary X-ray sources.
Authors: Bahcall, J. N.; Bahcall, N. A.
1974asgr.proc...73B    Altcode:
  The optical counterparts of six X-ray sources known to be in binary
  systems are discussed (HZ Her/Her X-1, ?/Cen X-3, HD 153919/3U 1700-37,
  HD 77581/Vela XR-1, Sk 160/SMC X-1, and HDE 226868/Cyg X-1). Detailed
  summaries of data for each system are presented and include X-ray
  and optical properties, establishment of optical identifications, and
  mass estimates. Significant facts noted include the unusual spectral
  type, optical luminosity and variations, and position of HZ Her;
  the difficulty in determining the counterpart of Cen X-3; and the
  substantial evidence that Cyg X-1 is a black hole. Attempts to locate
  an optical counterpart to Cyg X-3 are described, and uncertainties
  in determining the masses of X-ray sources with and without regular
  pulsations are noted.

---------------------------------------------------------
Title: A model for the light curve of HZ Herculis.
Authors: Joss, P. C.; Avni, Y.; Bahcall, J. N.
1973ApJ...186..767J    Altcode:
  The sharp minimum in the optical light curve of HZ Her is very different
  from the flat-bottomed X-ray eclipse of Her X-1. A simple model is
  presented which is consistent with the shapes of the minima of both the
  optical and X-ray light curves and which quantitatively reproduces the
  entire optical light curve (B-magnitudes). The essential feature of the
  model is the assumption that some of the incoming radiation from Her
  X-1 is absorbed well above the photosphere of HZ Her and is reradiated
  locally as optical light. Some possible observational consequences of
  this general class of models are discussed, including variations in
  the flux and spectrum of the X-rays at the beginning and end of the
  eclipse, optical emission lines, and UBV colors. Subject headings:
  eclipsing binaries stars, individual X-ray sources

---------------------------------------------------------
Title: Steady Energy Source in Her X-l?
Authors: Avni, Y.; Bahcall, J. N.; Joss, P. C.; Bahcall, N. A.; Lamb,
   F. K.; Pethick, C. J.; Pines, D.
1973NPhS..246...36A    Altcode: 1973Natur.246...36A
  OBSERVATIONS of the Her X-l system show that the X-ray emission
  above ~ 2 keV has three cycles : a pulsation period of 1.2 s; a 1.7-d
  orbital period associated with the motion of Her X-l about HZ Her;
  and a 35-d cycle during which the source is in a high, observable
  state for some 12 d, followed by a 23-d low period during which no X
  rays are observed<SUP>1,2</SUP>. Optical emission from HZ Her shows
  periodic brightness changes with a 1.7-d period, such that the phase
  of maximum brightness coincides with the maximum in the pulsed X-ray
  intensity<SUP>3,4</SUP>. These observations have been interpreted in
  terms of HZ Her as a late A or early F star which has a bright side
  as a result of heating due to radiation from Her X-l (refs 3 to 7).

---------------------------------------------------------
Title: Nuclear Fusion in Accreting Neutron Stars
Authors: Rosenbluth, M. N.; Ruderman, M.; Dyson, F.; Bahcall, J. N.;
   Shaham, J.; Ostriker, J.
1973ApJ...184..907R    Altcode:
  We note that the total energy release from hydrogen accreting onto
  a neutron star consists of two entirely distinct contributions: (1)
  the gravitational potential energy loss by bringing additional mass
  down to the stellar surface; (2) the energy released in the fusion
  of the added hydrogen to form helium and heavier nuclei, about 7 MeV
  per nucleon. The fusion energy source is sufficiently far below the
  relatively opaque stellar surface that it heats the entire star and the
  whole surface becomes an X-ray source considerably cooler than the more
  localized source from contribution 1. These cooler X-rays may persist
  for many years after accretion is interrupted. We suggest that these
  notions could be relevant to some X-ray sources, perhaps even to the
  optical X-ray binary in Hercules. Subject headings: neutron stars -
  nuclear reactions - X-ray sources

---------------------------------------------------------
Title: A Search for High-Excitation Redshift Systems in the Absorption
    Spectra of Five Quasars
Authors: Bahcall, J. N.; Joss, P. C.; Cohen, J. G.
1973ApJ...184...57B    Altcode:
  We have searched the absorption spectra of five quasars for the presence
  of redshift systems dominated by the highly ionized doublets C iv, N
  v, and 0 vi, which could be the strongest lines produced by absorbing
  clouds with collisional ionization temperatures between 10 and 106
  K. There is at most marginal evidence for one such system apiece in the
  spectra of PHL 957 and 4C 05.34, which are the two quasars with the
  largest known emission redshifts. Highly ionized redshift systems of
  this type are not widespread among the five quasars we investigated; the
  number of redshifts found in the observed spectra is not significantly
  larger than the number found in similar random-number spectra. Less
  than 5 percent of the observed absorption lines are identified in a
  statistically significant way by redshift systems of this type. Subject
  headings: quasi-stellar sources or objects - redshifts

---------------------------------------------------------
Title: Observations of QSOs in the direction of clusters of galaxies.
Authors: Bahcall, N. A.; Bahcall, J. N.; Schmidt, M.
1973ApJ...183..777B    Altcode:
  A search for QSOs in the direction of 66 Abell clusters of galaxies
  has yielded eight objects with redshifts ranging from 0.09 to
  2.06. Statistical arguments suggest that the ratio of bright QSOs to
  bright galaxies in clusters of galaxies is not more than 10 times
  that ratio in the field. The number of QSOs found is larger than
  expected from field surveys, but the apparent excess may be caused
  by systematic error in our magnitudes. Subject headings: galaxies,
  clusters of - quasi-stellar sources or objects - redshifts

---------------------------------------------------------
Title: Nonspherical Thermal Instabilities
Authors: Rosenbluth, Marshall N.; Bahcall, John N.
1973ApJ...184....9R    Altcode:
  General conditions for the existence of nonspherical thermal
  instabilities are derived. The instabilities are not present in
  numerical models of the Sun that have been tested. Subject headings:
  instabilities - interiors, solar

---------------------------------------------------------
Title: Radio Stars and X-ray Sources
Authors: Bahcall, John N.; Kellogg, Edwin M.
1973NPhS..244..135B    Altcode: 1973Natur.244..135B
  SEVERAL weak, highly variable radio sources have been shown by excellent
  optical-radio positional agreement (~ 1 arc s) to be associated with
  optically bright binary stars<SUP>1-13</SUP>. One of these radio stars,
  associated with the optical binary HDE-226868 (refs 10-16) has been
  suggested as the optical-radio counterpart of the strong variable
  X-ray source, Cyg X-1 (a frequently discussed candidate for a black
  hole). We report limits on the X-ray emission from the known radio
  stars that can be studied with Uhuru. These results are of interest
  because of the possible association between X-ray binaries and radio
  star binaries, and because limits or measurements of the X-ray fluxes
  can help determine the source of the radio emission. A strong limit
  (comparable to those reported here) on the X-ray emission from the
  optical-binary β Persei during periods of radio flaring has recently
  been reported by the MIT OSO-7 group<SUP>17</SUP>.

---------------------------------------------------------
Title: Solar Neutrinos.IV. Effect of Radiative Opacities on Calculated
    Neutrino Fluxes
Authors: Bahcall, John N.; Huebner, W. F.; Magee, N. H., Jr.; Merts,
   A. L.; Ulrich, Roger K.
1973ApJ...184....1B    Altcode:
  The effect of radiative opacities on the predicted capture rate for
  the 37Cl solar neutrino experiment is investigated with the aid of new
  opacities obtained from an improved Los Alamos code. Subject headings:
  interiors, solar - neutrinos - opacities

---------------------------------------------------------
Title: On the Temperature of the Microwave Background Radiation at
    a Large Redshift
Authors: Bahcall, John N.; Joss, Paul C.; Lynds, Roger
1973ApJ...182L..95B    Altcode:
  It is shown that the temperature of the microwave background radiation
  at a redshift of the order of 2.5 is certainly less than 200 K and
  probably less than 45 K. Further detailed studies of the absorption
  spectra of large-redshift quasars can improve these limits. Subject
  headings: cosmic background radiation - quasi-stellar sources or objects

---------------------------------------------------------
Title: Model for X-ray Sources Based on Magnetic Field Twisting
Authors: Bahcall, John N.; Rosenbluth, Marshall N.; Kulsrud, Russell M.
1973NPhS..243...27B    Altcode: 1973Natur.243...27B
  SEVERAL X-ray sources have been identified with binary stellar
  systems. It has been generally concluded that the presence of X-rays
  implies one of the stars must be a collapsed object (white dwarf,
  neutron star or black hole) which accretes matter from the other star,
  thus producing the X-rays. To a certain extent, this conclusion is
  based on the absence at present of any reasonable alternative model
  for the origin of X-rays. Because of the importance of establishing
  whether binary X-ray sources contain collapsed objects, we feel that
  it is worthwhile to attempt to construct alternative models and to
  derive their observational properties.

---------------------------------------------------------
Title: Optical and Near-Infrared Observations of the Nearby Spiral
    Galaxy Maffei 2
Authors: Spinrad, Hyron; Bahcall, J.; Becklin, E. E.; Gunn, James E.;
   Kristian, J.; Neugebauer, G.; Sargent, W. L. W.; Smith, H.
1973ApJ...180..351S    Altcode:
  Spectra, photographs, and photometric measurements have been
  used to show that Maffei 2 has a distance of 5 i 2 Mpc and that
  it has a morphological type near Sbc II in agreement with similar
  conclusions made earlier by radio observers. We discuss the possible
  relationships between Maffei 2 and the elliptical galaxy Maffei 1;
  there are serious inconsistencies in the existing data which bear on
  this question. Subject headings: galaxies, individual - infrared sources

---------------------------------------------------------
Title: The Hubble Diagram for the Brightest Quasars
Authors: Bahcall, John N.; Hills, Richard E.
1973ApJ...179..699B    Altcode:
  The slope of the magnitude-redshift relation for the optically most
  luminous quasars with redshifts ranging from 0.2 to more than 2 is
  consistent with the value of 5 expected from the expansion of the
  universe if luminosities are evaluated assuming quasars are at the
  cosmological distances implied by their redshifts. Subject headings:
  cosmology - quasi-stellar sources or objects - redshifts - relativity

---------------------------------------------------------
Title: An analysis of the absorption spectrum of PHL 957.
Authors: Bahcall, J. N.; Joss, P. C.
1973ApJ...179..381B    Altcode:
  Five absorption redshifts ranging from z = 2.67 to z = 2.22 are
  identified in the observed spectrum of PHL 957, in good agreement
  with the earlier analysis of Lowrance et al. Our results are to be
  compared with an average of 1.0 i 0.9 redshifts found in random-number
  spectra having the same essential characteristics as the observed
  spectrum. The distribution of identified absorption redshifts is
  presented and discussed for five quasars, whose rich absorption
  spectra have all been studied with the same methods as those used in
  the present investigation. Subject headings: line identifications -
  quasi-stellar sources or objects - redshifts

---------------------------------------------------------
Title: The Hubble Diagram for the Brightest Quasars
Authors: Hills, Richard E.; Bahcall, John N.
1973NYASA.224...58H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Quasar Variability as a Function of Absolute Luminosity
Authors: Ames, Susan; Bahcall, John N.
1973ApL....14..199A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The redshift controversy
Authors: Field, George B.; Arp, Halton C.; Bahcall, John N.
1973reco.book.....F    Altcode: 1973QB465.F53......
  No abstract at ADS

---------------------------------------------------------
Title: HZ Herculis.
Authors: Goldsmith, S.; Bahcall, J. N.; Bahcall, N. A.
1973IAUC.2529....1G    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The solar neutrino problem.
Authors: Bahcall, J. N.
1973NucIM..11..381B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Redshifts as distance indicators.
Authors: Bahcall, J. N.; Arp, H.
1973reco.conf...61B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On the Luminosity Functions of Giant Stars in Globular Clusters
Authors: Bahcall, John N.; Yahil, Amos
1972ApJ...177..647B    Altcode:
  The observed luminosity function for stars on the giant branch of
  M15, as determined by Sandage, Katem, and Kristian, is compared with
  simulated luminosity functions generated from a smooth curve. Apparent
  features are seen in both the observed and simulated luminosity
  functions. A crude fit to the observed differential luminosity function
  is given by N(L) cc L -26

---------------------------------------------------------
Title: The Period and Light Curve of HZ Herculis
Authors: Bahcall, John N.; Bahcall, Neta A.
1972ApJ...178L...1B    Altcode:
  It is shown that HZ Hercutis has an eclipse period and phase equal to
  the eclipse period and phase of the pulsating X-ray source Hercules
  X-1. Data for HZ Hercutis are also given for the light curve, colors,
  proper motIon, and the influence of the 35 day X-ray cycle on the
  optical light. A model for the binary system is described and the
  optical light curve is calculated.

---------------------------------------------------------
Title: The Estimation of Masses of Individual Galaxies in Clusters
    of Galaxies
Authors: Wolf, Richard A.; Bahcall, John N.
1972ApJ...176..559W    Altcode:
  Expressions are derived for approximate limits on the mass of an
  individual galaxy or quasi-stellar object that is a member of a group
  or cluster of galaxies. Two different approaches are used: first, a
  perturbation method that yields approximate limits on the mass of any
  observed object in a cluster provided only that the positions of cluster
  galaxies around the unknown mass are measured and redshifts are known
  for several galaxies in the cluster; and second, an extension of Page's
  method that gives approximate mass limits for any bound pair of galaxies
  whose positions and redshifts are known. The uncertainties in the mass
  estimates, arising from both observational and statistical effects,
  are estimated analytically. An "upper estimate," 80 percent certain
  to be greater than the actual mass of the galaxy, can be obtained in
  every case. A "best guess," at least 50 percent certain to be greater
  than the actual mass of the galaxy, and a "lower estimate," 80 percent
  certain to be less than the actual galaxy mass, can be obtained in
  some cases. The analytically derived formulae for the upper, lower,
  and best-guess estimates are then verified by comparison with computer
  simulatinas of the dynamical evolution of clusters of galaxies, using
  the numerical methods of Aarseth. Estimates are made of the masses
  of NGC 6166 ( 3C 338), NGC 4874 and 4889 (the giant ellipticals near
  the center of the Coma cluster), B264, TON 256, PKS 2251+11, and 10
  supergiant galaxies that have double nuclei. We obtain the following:
  for NGC 6166, 8 X 1011 M0 &lt;M &lt;4 X 10' M0 and 8 &lt; AI/L &lt;400 g
  s for NGC 4874, Al &lt;= 2 X 1014 Al0 and M/L &lt;2000g s erg-1 for NGC
  4889, Al &lt;3 X 1014 Al0 and Al/L &lt; 2100 g s for B264, Al &lt; 7 X
  tOll Al0 and Al/L &lt; 3000 g s 256, Al &lt; 4 X 1011 Al0 and Al/L &lt;
  300 g s and for PKS 2251+11, Al &lt; 3 X 1013 Al0 and Al/L &lt; 40 g s .

---------------------------------------------------------
Title: On Identifying New Kinds of Astronomical Objects
Authors: Bahcall, John N.; Yahil, Amos
1972NPhS..238...92B    Altcode: 1972Natur.238...92B
  WE wish to draw attention to a statistical problem that arises in an
  especially acute form when the data from a number of new sources are
  analysed to try to find evidence for a particular kind of object, for
  example, a neutron star or a black hole. We wish to emphasize that a
  statistical analysis of the data on any particular source must include
  consideration of the data on other sources that were found.

---------------------------------------------------------
Title: Are Galaxies Formed by Material Flowing Out of Singularities?
Authors: Bahcall, J. N.; Joss, P. C.
1972CoASP...4...95B    Altcode: 1972ComAp...4...95B
  No abstract at ADS

---------------------------------------------------------
Title: Quarks as a Thermometer for Cosmologies
Authors: Frautschi, Steven; Steigman, Gary; Bahcall, John
1972ApJ...175..307F    Altcode:
  If physical quarks exist, their density relative to ordinary baryons
  (nq/flB) depends sensitively on the highest temperatures reached
  during cosmological evolution. Zel'dovich has pointed out that in
  the conventional hot big bang with a limited spectrum of elementary
  particles the quark density flq/flB predicted for the present time is
  much larger than the experimental upper bound. In the present paper we
  derive the consequences for conventional cosmologies of the Hagedorn
  type of hadron spectrum which implies a "warm" limiting temperature of
  order kT 160 MeV. With initial temperatures of this order, the predicted
  flq/flB is consistent with present experimental limits if the quark
  mass exceeds 9 GeV. In the Hagedorn model, quarks with rn, &gt; 9 GeV
  would be very difficult to produce in accelerator experiments because of
  statistical competition; searches for fossil quarks in bulk matter seem
  to offer the only hope of detection. We also discuss predictions for
  the quark density in several less conventional cosmologies (mix master,
  Brans-Dicke, Lemaitre, steady state, and Klein-Alfven) and with forms of
  the hadron density of states that differ from Hagedorn's proposed form

---------------------------------------------------------
Title: Some Observational Distinctions Among Models of Pulsing
    X-Ray Binaries
Authors: Arons, J.; Bahcall, J. N.
1972ApL....11..191A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Galaxy Distributions in the Zwicky Catalogue.
Authors: Hauser, M. G.; Bahcall, J. N.
1972BAAS....4R.239H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Models for the Cosmic Evolution of Radio Galaxies and Quasars.
Authors: Bahcall, John N.
1972ApJ...172..265B    Altcode:
  The observational distinctions between various explanations
  of radio-source evolution are exhibited with the aid of simple
  models. These models are derived by using a formalism that enables one
  to calculate, on the basis of explicit hypotheses, the number of sources
  that are present at a given cosmic time. Particular attention is given
  to "ultraconservative" and "symmetric" models. In the ultraconservative
  models, the total number of galaxies that have been radio galaxies is
  constant in time (after some creation period), but most of what are
  today "normal" galaxies were powerful radio sources when they were
  younger. In the symmetric models, the evolution of radio galaxies
  and quasars is treated in the same way by using coupled equations
  that suggest a mean life for the primordial bright ellipticals of 10
  years. Both the ultraconservative and the symmetric models suggest that
  there may be significant departures from the usually predicted relations
  in the diagram of apparent magnitude versus redshift for largeredshift
  radio galaxies because the usual relations are calculated for objects
  with typical luminosities that are independent of cosmic time. The
  observational basis for some of the evolutionary models considered is
  strengthened by the application of the luminosity-volume test to an
  essentially complete sample of 3C R radio galaxies for which redshifts
  and accurate optical magnitudes are available. The results confirm and
  strengthen the conclusions of revious investigators regarding the lack
  of evolution among radio galaxies with an intrinsic power at 1 8 MHx
  of less than 1026 V .

---------------------------------------------------------
Title: On the Time Dependence of Emission-Line Strengths from a
    Photoionized Nebula
Authors: Bahcall, John N.; Kozlovsky, Ben-Zion; Salpeter, E. E.
1972ApJ...171..467B    Altcode:
  Discussions are given for the time dependence of emission-line
  intensities from nebulae that are photoionized by a central source
  with a variable continuum flux. Explicit calculations are carried
  out for some cases (especially when the nebula can be considered
  a thin shell) for a temporary increase of continuum flux of simple
  "square-wave hump" shape. In some cases, changes in line intensities
  are predicted over times that are small compared with the light travel
  time across the nebula. The observational situation is described and
  further measurements are suggested for a number of objects that are
  relatively easy to study and whose further investigations seem likely to
  lead to important conclusions regarding the nebular parameters. These
  promising objects include QSOs, and N-type, Seyfert, and compact
  galaxies, as well as some X-ray sources and old novae.

---------------------------------------------------------
Title: Are Quasars Associated with Bright Galaxies?
Authors: Bahcall, J. N., Mckee, C. F.; Bahcall, N. A.
1972ApL....10..147B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: HZ Herculis.
Authors: Bahcall, J. N.; Bahcall, N. A.; Crampton, D.; Morbey, C. L.
1972IAUC.2428....1B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The solar neutrino problem.
Authors: Bahcall, J. N.
1972CNPPh...5...59B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Neutrinos
Authors: Bahcall, John N.; Sears, R. L.
1972ARA&A..10...25B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Are Neutrinos Stable Particles?
Authors: Bahcall, John N.; Cabibbo, Nicola; Yahil, Amos
1972PhRvL..28..316B    Altcode:
  It is pointed out that neutrinos with a finite mass could be
  unstable. We discuss the consequences of this possibility for
  solar-neutrino experiments.

---------------------------------------------------------
Title: HZ Herculis.
Authors: Bahcall, J. N.; Bahcall, N. A.; Liller, W.; Jones, C.;
   Forman, W.; Shao, C. Y.
1972IAUC.2427....1B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Hadron Barrier in Cosmology and Gravitational Collapse
Authors: Bahcall, John N.; Frautschi, Steven
1971ApJ...170L..81B    Altcode:
  It is shown that the early stages of a big-bang cosmology are
  hadron-dominated if the density of hadron states per unit mass
  interval, p (m), increases at least as fast as m ' and if the initial
  gravitational anisotropy is not large. It is further shown that if these
  conditions are satisfied, then quantum effects must modify the classical
  equations of general relativity at times t 1(t23 5 before the attainment
  of the singularities predicted in classical relativistic cosmologies
  and stellar collapse (i.e., before the well- known modifications due
  to quantum fluctuations of the metric at times l0- s).

---------------------------------------------------------
Title: Solar Neutrinos. III. Composition and Magnetic-Field Effects
    and Related Inferences
Authors: Bahcall, John N.; Ulrich, Roger K.
1971ApJ...170..593B    Altcode:
  An improved solar model is shown to yield a calculated capture rate
  for the 27CI neutrino experiment that is a factor of 6 larger than the
  observed rate reported by Davis, Rogers, and Radeha. The 5B branch
  must occur a factor of 10 less often than expected on the basis of
  standard solar models. The effects on the calculated capture rates of
  a variety of composition uncertainties are considered. The effects of
  a strong primordial magnetic field are also investigated. The results
  obtained by several investigators who used different stellar-evolution
  programs are compared, and it is concluded that the different programs
  give consistent, but observationally incorrect, results.

---------------------------------------------------------
Title: On the Absorption-Line Spectrum of 4c 05.34
Authors: Bahcall, John N.; Goldsmith, Samuel
1971ApJ...170...17B    Altcode:
  Eight acceptable absorption redshifts are found in the spectrum of
  4C 05.34 reported by Lynds. The absorption redshifts range from z =
  2.875 to z = 1.776. An average nonsense spectrum has 1.4 acceptable
  redshifts. The absence of absorption from excited fine-structure states
  implies that the absorbing region has an electron density &lt;102 and
  is at a distance &gt;1 kpc from the continuum source of the QSO.

---------------------------------------------------------
Title: Ultradense Matter
Authors: Frautschi, S.; Bahcall, J. N.; Steigman, G.; Wheeler, J. C.
1971CoASP...3..121F    Altcode: 1971ComAp...3..121F
  No abstract at ADS

---------------------------------------------------------
Title: Relative Correlation of - and Small-Redshift Quasi-Stellar
    Objects with Clusters of Galaxies
Authors: Bahcall, John N.; Bahcall, Neta A.; Burbidge, G. R.
1971ApJ...166L..77B    Altcode:
  The importance of investigating the relative probability that large-
  and small-redshift QS0s appear in the direction of catalogued clusters
  of galaxies is discussed. This relative probability is determined for
  a large sample of QS0s with respect to both Zwicky and Abell clusters
  of galaxies. The results are summarized in three general conclusions.

---------------------------------------------------------
Title: The Ionization Structure of a Nebula Photoionized by a Flat
    Spectrum
Authors: Bahcall, J. N.; Bahcall, N. A.; Kozlovsky, B. -Z.
1971A&A....13....1B    Altcode:
  Analytic approximations are developed in this paper for the ionization
  structure of a medium that is photoionized by a flat spectrum. The
  presence of a diffuse ionization zone depends on the precise form of the
  ultraviolet ionization spectrum. For a photon number spectrum that falls
  off as -1 there is a diffuse ionization structure and for a spectrum
  that falls off like v- there is a more classical Stro. mgren-like
  behavior with a halfwidth an order of magnitude smaller than in the v-1
  case. The basic equations are also presented for a more general class of
  spectral indices as well as a power law behavior of the total density
  on distance from the ionization source. Key words: photoionization -
  flat spectrum - Seyfert galaxies - quasars - spectral index.

---------------------------------------------------------
Title: Some Unsolved Problems in Astrophysics
Authors: Bahcall, John N.
1971AJ.....76..283B    Altcode:
  The theoretical and observational situation with regard to solar
  neutrinos is reviewed and some of the implications of the discrepancy
  between theory and observation are discussed. A definition is suggested
  for compact luminous objects (CLO's) and various proposals for the
  energy source of CLO's are reviewed. The observational situation and
  opportunities with regard to the association of CLO's (or QSO's) with
  galaxies is outlined. The absorption lines observed in large-redshift
  CLO's are divided tentatively into two classes whose origin is
  discussed. A number of critical observations are suggested to test
  various unorthodox ideas.

---------------------------------------------------------
Title: Upper Limit on Neutrino Energy Associated with Weber Pulses
Authors: Bahcall, John N.; Davis, Raymond
1971PhRvL..26..662B    Altcode:
  An upper limit is established on the fraction of energy associated
  with the gravitational pulses reported by Weber that could be in the
  form of neutrinos with energies between 0.9 and 100 MeV.

---------------------------------------------------------
Title: Quark Fusion in Quasi-Stellar Objects?
Authors: Bahcall, John N.; Callan, C. G., Jr.; Dashen, Roger
1971ApJ...163..239B    Altcode:
  The rates of the most likely quark-fusion reactions are estimated. An
  approximate formula is derived for the efficiency (&gt;50 percent)
  of converting rest mass into photons by quark fusion. The temperature
  at which quarks might fuse is crudely estimated to be a few million
  degrees Kelvin. Several ways are discussed that quark-electron atoms
  could conceivably be detected in astronomical objects.

---------------------------------------------------------
Title: Some Inferences from Spectrophotometry of Quasi-Stellar Sources
Authors: Bahcall, John N.; Oke, J. B.
1971ApJ...163..235B    Altcode:
  Limits are placed on the amount of neutral and ionized hydrogen gas
  that can be in the vicinity of 4C OS 34 (and three other QSSs); these
  results place severe restraints on models of quasi-stellar radio sources
  in which the QSS phenomenon is supposed to occur within a galaxy A
  limit on the electron temperature is also established (1 x 10 &lt;
  &lt; 2 X 10 K) The relative abundance of C++ to C+++ is determined
  approximately in five QSSs, and the ratio of helium to hydrogen is
  estimated for fourteen QSSs.

---------------------------------------------------------
Title: Solar Neutrinos
Authors: Bahcall, J. N.
1971AIPC....2..243B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Extragalactic Pulsars
Authors: Bahcall, John N.; Rees, Martin J.; Salpeter, E. E.
1970ApJ...162..737B    Altcode:
  Newly formed pulsars might be detectable out to distances 10 Mpc by
  searching for millisecond optical or X-ray pulses from the sites of
  newly reported supernovae.

---------------------------------------------------------
Title: On the Bowen Resonance Fluorescence Lines in Quasi-Stellar
    Objects
Authors: Bahcall, John N.; Kozlovsky, Ben-Zion
1970ApJ...162..789B    Altcode:
  It is shown that the Bowen resonance fluorescence lines are expected
  to be weak in QSOs even if the nebula is photoionized.

---------------------------------------------------------
Title: Galaxies in the Direction of QSO's With Small Redshifts
Authors: Bahcall, Neta A.; Bahcall, John N.
1970PASP...82.1276B    Altcode:
  Accurate positions are given for the brightest galaxies that are likely
  to be associated with all known QSO's with redshifts less than or equal
  to 0.2. Special attention is drawn to the galaxies in the direction of
  3C 273. It is shown that the probabili is small that purely by chance
  coincidence a galaxy redshift will be measure to be approximately
  equal to that of a quasar in its direction.

---------------------------------------------------------
Title: Comet Gunn (1970p)
Authors: Schmidt, M.; Gunn, J. E.; Bahcall, J. N.; Young, J. W.;
   Marsden, B. G.
1970IAUC.2294....1S    Altcode:
  Dr. M. Schmidt, California Institute of Technology, reports that a
  comet was discovered by James E. Gunn on a plate exposed with the
  122-cm Schmidt telescope at Palomar on October 27. From the trailed
  image the daily motion was determined as dR.A. = -0m71, dDecl. =
  -2'. Further images of the comet were located on plates exposed with
  the same telescope on November 22 and 23 by J. N. Bahcall. The comet was
  diffuse, with central condensation and a small tail. Dr. Gunn measured
  accurate positions from the three plates, as shown below. The comet
  was also recorded on November 6 by J. W. Young on three plates exposed
  with the 61-cm reflector at Table Mountain Observatory, Wrightwood,
  California. 1970 UT R.A. (1950) Decl. m1 Observer Oct. 27.22500 1
  23 41.6 - 2 01 45 16 Gunn Nov. 6.31250 1 17 11.7 - 2 14 03 15 Young
  6.34722 1 17 09.9 - 2 13 56 " 22.27014 1 09 29.5 - 2 10 00 16 Bahcall
  23.30486 1 09 08.3 - 2 08 48 16 " The elliptical elements below, by
  the undersigned, are very uncertain, but the ephemeris should help
  observers to locate the comet. Differential residuals of 8" and 11"
  remain between the second and third, and the fourth and fifth positions,
  respectively. T = 1969 Mar. 14.47 ET Peri. = 195.70 e = 0.2931 Node =
  66.91 1950.0 a = 3.5599 AU Incl. = 10.62 n = 0.14674 q = 2.5164 AU P =
  6.72 years 1970/71 R. A. (1950) Decl. Delta r m1 Dec. 10 1 05.75 - 1
  32.4 20 1 05.97 - 0 57.7 3.518 3.925 16.7 30 1 07.78 - 0 15.0 Jan. 9
  1 11.05 + 0 34.5 3.866 3.969 16.9 19 1 15.61 + 1 29.4 29 1 21.30 +
  2 28.4 4.212 4.013 17.2 m1 = 8.0 + 5 log Delta + 10 log r

---------------------------------------------------------
Title: Multiple Absorption Redshifts in Quasars
Authors: Bahcall, J. N.
1970CoASP...2..221B    Altcode: 1970ComAp...2..221B
  No abstract at ADS

---------------------------------------------------------
Title: Photon Splitting in a Strong Magnetic Field
Authors: Adler, S. L.; Bahcall, J. N.; Callan, C. G.; Rosenbluth, M. N.
1970PhRvL..25.1061A    Altcode:
  We determine the absorption coefficient and polarization selection
  rules for photon splitting in a strong magnetic field, and describe
  the possible application of our results to pulsars.

---------------------------------------------------------
Title: On the Rich Absorption Spectra of Three Quasi-Stellar Objects
Authors: Bahcall, John N.; Feldman, Uri
1970ApJ...161..389B    Altcode:
  The absorption spectra of PHL 938, TON 1530, and PKS 0237-23 have
  been searched in a systematic way for redshifts that may include lines
  arising from metastable states, interstellar lines, and Balmer lines. A
  search for blueshifts was also carried out for the first time. The
  statistical significance of the redshift system I = 0.6128 in PIlL
  938 was established by analyzing random-number spectra. It is shown
  that the electron density is less than 50 T4112 in the vicinity of
  this absorption system and that the minimum separation between PHL 938
  and the absorption system is about 100 pc. A critical test of the idea
  that normal galaxies produce the absorption lines is described. Nine
  interstellar lines observed in the spectra of stars in the galaxy might
  appear in the.observationally accessible region between 4956 and 6400
  A for the redshift system I = 0.6128 of PHL 938.

---------------------------------------------------------
Title: On the Galaxies in the Direction of Ton 256 and B 264
Authors: Bahcall, John N.; Bahcall, Neta A.
1970PASP...82..721B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar-Neutrino Fluxes with Recent Corrections to Opacity
Authors: Bahcall, John N.; Ulrich, Roger K.
1970ApJ...160L..57B    Altcode:
  Improved calculations of the rate of solar-neutrino capture for
  experiments with 87Cl and 7Li are presented. There is a sizable
  discrepancy between the calculated values and the experimental upper
  limit of Davis et at. The primordial helium abundance inferred from the
  relevant solar models ranges from Y = 0.22 to Y = 0.26. The expected
  neutrino capture rates in the 87Cl and 7Li experiments and the inferred
  primordial helium abundance are sensitive to the presentday photospheric
  abundance ratio of iron to hydrogen.

---------------------------------------------------------
Title: Upper Limits on the Masses of Quasi-Stellar Sources
Authors: Bahcall, John N.; Salpeter, E. E.
1970ApJ...159L.135B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Some Models for the Emission-Line Region of 3c 48
Authors: Bahcall, John N.; Kozlovsky, Ben-Zion
1969ApJ...158..529B    Altcode:
  Models for the emission-line region of 3C 48 are derived by using
  calculated ionization distributions. Estimates are given of the
  parameters that characterize the emission-line region and of the
  relative abun- dance of H, He, 0, Ne, and Mg

---------------------------------------------------------
Title: Quasi-Stellar Objects in the Direction of Rich Clusters
    of Galaxies
Authors: Bahcall, John N.
1969ApJ...158L..87B    Altcode:
  Fourteen quasi-stellar objects are listed that are in the direction of
  rich clusters of galaxies in Abell's catalog. The importance of making
  redshift measurements of galaxies with small angular separations from
  quasi-stellar objects with redshifts &lt;0.2 is discussed

---------------------------------------------------------
Title: On the Masses of Quasi-Stellar Sources
Authors: Bahcall, John N.; Salpeter, E. E.
1969ApJ...158L..15B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Quasi-Stellar Objects in the Direction of Clusters of Galaxies
Authors: Bahcall, John N.
1969ApJ...157L.151B    Altcode:
  Twenty-one quasi-stellar objects are listed that are in the direction
  of clusters of galaxies. These objects are interesting candidates for
  absorption experiments

---------------------------------------------------------
Title: Review Paper: Solar Neutrinos.
Authors: Davis, Raymond, Jr.; Bahcall, John N.
1969BAAS....1Q.339D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On the Possibility of Detecting Redshifted 21-CM Absorption
    Lines in the Spectra of Quasi-Stellar Sources
Authors: Bahcall, John N.; Ekers, Ronald D.
1969ApJ...157.1055B    Altcode:
  The expected strengths of redshifted 21-cm absorption lines are
  estimated by using the properties of the observed optical absorption
  lines in quasi-stellar sources. It is shown that the absence of 0 i
  and N i absorption lines in the observed optical absorption spectra of
  quasi-stellar radio sources indicates that 21-cm absorption lines wider
  than 100 kllz are likely to be weak unless the heavy-element abundance
  in the absorbing material is low. Lines narrower than 100 kETz may be
  strong; their optical counterparts would have escaped detection. A
  general expression is given for the spin temperature of neutral
  hydrogen when (following Field) Ly a excitation and de-excitation, 21-cm
  absorption and emission, and particle collisions are all included. The
  results are expressed simply in terms of the strength and distance of
  the radio source and the separation between absorber and emitter. It
  is shown that the spin temperature of neutral hydrogen is large near
  a quasi-stellar radio source and is determined either by the ambient
  21-cm flux or the ambient Ly a flux for separations between absorber
  and emitter of less than about 1O~ It-yr. The expected absorption
  (and emission) strengths of redshifted 21-cm lines are compared with
  observa- tional capabilities at radio observatories. Some interesting
  candidates for study are listed

---------------------------------------------------------
Title: Are Some Quasi-Stellar Objects Associated with Clusters
    of Galaxies?
Authors: Bahcall, John N.; Schmidt, Maarten; Gunn, James E.
1969ApJ...157L..77B    Altcode:
  Five small-redshift quasi-stellar objects are listed that are within
  the approximate geometrica] boundaries of catalogued clusters of
  galaxies. Spectra of four galaxies in one of the clusters show the
  same redshift as the associated quasi-stellar object B264

---------------------------------------------------------
Title: What Next with Solar Neutrinos?
Authors: Bahcall, John N.
1969PhRvL..23..251B    Altcode:
  The capture rate of solar neutrinos is estimated for a number of targets
  that have been suggested previously as possible detectors of solar
  neutrinos. It is shown that the most important feasible experiment to
  be carried out in the future employs <SUP>7</SUP>Li as a detector.

---------------------------------------------------------
Title: Neutrinos from the Sun
Authors: Bahcall, John N.
1969SciAm.221a..28B    Altcode: 1969SciAm.221...29B
  No abstract at ADS

---------------------------------------------------------
Title: Solar Neutrinos
Authors: Bahcall, John N.; Bahcall, Neta A.; Ulrich, Roger K.
1969BAAS....1Q.272B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Sensitivity of the Solar-Neutrino Fluxes
Authors: Bahcall, John N.; Bahcall, Neta A.; Ulrich, Roger K.
1969ApJ...156..559B    Altcode:
  The sensitivity of the solar-neutrino fluxes to localized changes in
  the opacity and the equation of state is calculated. The sensitivity
  to changes in the equation of state reaches a maximum near 8 X 106
  °K and is in general much larger than the sensitivity to opacity
  changes. The effect of various parameters on the predicted rate of
  neutrino capture in the 37C1 experiment is summarized in equation
  (8). The char- acteristic numerical properties of a standard solar
  model are then presented. Several general conclusions are justified on
  the basis of the variations considered. In particular, an assessment
  is given of the relation between the theory of solar models and the
  experimental results of Davis, Harmer, and Hoffman

---------------------------------------------------------
Title: Absorption Lines Produced by Galactic Halos
Authors: Bahcall, John N.; Spitzer, Lyman, Jr.
1969ApJ...156L..63B    Altcode:
  We propose that most of the absorption lines observed in quasi-stellar
  sources with multiple absorp- tion redshifts are caused by gas in
  extended halos of normal galaxies

---------------------------------------------------------
Title: ON the Absorption Spectrum of Ton 1530
Authors: Bahcall, John N.; Osmer, Patrick S.; Schmidt, Maarten
1969ApJ...156L...1B    Altcode:
  An analysis of the absorption-line spectrum of Ton 1530 is reported. The
  line widths are less than 4 A in the observed frame. Three acceptable
  absorption redshifts, z = 1.9365, z = 1.9215, and z = 1.8866, and one
  plausible absorption redshift, z = 1.9800, are identified. Only 0.1
  acceptable redshift was found per random-number spectrum constructed
  to have the same essential characteristics as the observed spectrum

---------------------------------------------------------
Title: Statistical Tests for the Origin of Absorption Lines Observed
    in Quasi-Stellar Sources
Authors: Bahcall, John N.; Peebles, P. J. E.
1969ApJ...156L...7B    Altcode:
  Two statistical tests are described for the hypothesis that the
  multiple absorption redshifts observed in the spectra of at least some
  quasi-stellar sources arise in intervening material that is randomly
  distrib- uted in patches along the line of sight between us and the
  quasi-stellar sources

---------------------------------------------------------
Title: Some Models of the Emission-Line Region of 3c 273
Authors: Bahcall, John N.; Kozlovsky, Ben-Zion
1969ApJ...155.1077B    Altcode:
  Models for the emission-line region of 3C 273 are derived by using
  ionization distributions calculated with extrapolated forms of the
  observed photon flux. The calculated ionization distributions, which
  are different from those assumed by previous workers, are used to
  make estimates of the relative abundances of H, He, 0, Ne, Mg, and Fe
  Estimates are also given of the physical parameters that characterize
  the emission-line region

---------------------------------------------------------
Title: The ^{7}Be Electron-Capture Rate
Authors: Bahcall, John N.; Moeller, Charles P.
1969ApJ...155..511B    Altcode:
  The effect of plasma and bound-electron screening on the continuum
  capture rate of 7Be(e,~)7Li is calculated and shown to be negligible
  for situations in which the proton-proton chain is likely to be im-
  portant. A more accurate expression for the continuum capture rate
  is then derived, making use of the numerical work of Bahcall and
  May. Convenient formulae are presented for use in stellar-model calcula-
  tions. The average effect of bound-electron capture is also evaluated
  for several solar models

---------------------------------------------------------
Title: Fine-Structure Transitions and the Background Microwave
    Radiation
Authors: Petrosian, Vahé; Bahcall, John N.; Salpeter, E. E.
1969ApJ...155L..57P    Altcode:
  The contribution to the background microwave radiation from decays
  of excited fine-structure states of the more abundant ions is
  calculated. Transitions occurring in the Galaxy, in distant galaxies,
  and in the intergalactic medium are considered. It is shown that the
  intensity of radiation from fine-structure transitions in the Galaxy
  and in nearby galaxies exceeds the intensity of a 2.7° K black body
  for wave- lengths less than 0.05 cm

---------------------------------------------------------
Title: The Rate of the Proton-Proton Reaction and Some Related
    Reactions
Authors: Bahcall, John N.; May, Robert M.
1969ApJ...155..501B    Altcode:
  The results of detailed calculations of the rate of the proton-proton
  reaction, p + p -~ 2D + e+ + v, and the related electron-capture
  reaction, P + e + P -~ 2D + v, are presented. Estimates of the likely
  errors are given. The rates of some other electron-capture reactions
  that are of interest in connection with solar-neutrino experiments
  are also calculated

---------------------------------------------------------
Title: The Effect of the Brans-Dicke Cosmology on Solar Evolution
    and Neutrino Fluxes
Authors: Shaviv, G.; Bahcall, J. N.
1969ApJ...155..135S    Altcode:
  The effect of the Brans-Dicke theory of gravitation on the evolution
  of the Sun and the solar neu- trino flux is investigated Our results,
  for fashionable values of the scalar field coupling constant, the Hubble
  constant, and the heavy-element abundance, are (1) the solar luminosity
  decreased by about 10-50 per cent during the last 4 7 billion years; and
  (2) the solar neutrino flux for the Brans-Dicke theory is greater than
  the corresponding flux for constant-G theories by a factor of about 2

---------------------------------------------------------
Title: Observational Neutrino Astronomy: A ν-Review
Authors: Bahcall, John N.
1969tsra.conf..321B    Altcode: 1969qhea.conf..321B
  No abstract at ADS

---------------------------------------------------------
Title: The Absorption-Line Spectrum of the Quasi-Stellar Radio Source
    PKS 0237-23
Authors: Bahcall, John N.; Greenstein, Jesse L.; Sargent, Wallace L. W.
1968ApJ...153..689B    Altcode:
  We present in Table 2 the wavelengths of 49 absorption lines measured in
  the wavelength range XX3300-4800 in the spectrum of the quasi-stellar
  radio source PKS 0237- 23. Equivalent widths, half- widths, and
  central depths are given for thirty-eight of these lines having X&gt;
  3650 A. A systematic proce- dure has been used by Bahcall (1968) to
  identify twenty-eight of the lines with five absorption redshifts,
  namely, z = 2.2015, 1.6706, 1.6560, 1.5132, and 1.3642. There is
  no strong evidence for an absorption redshift of z = 1.95, found
  by earlier workers. It is presumed that the absorption lines in PKS
  0237-23 arise either in intergalactic space or in clouds which are near
  the object and moving at speeds of up to 0 3 c relative to the source
  of the emission lines. At present there is no compelling argument or
  observation to distinguish between these two hypotheses

---------------------------------------------------------
Title: A Systematic Method for Identifying Absorption Lines as
    Applied to PKS 0237-23
Authors: Bahcall, John N.
1968ApJ...153..679B    Altcode:
  A systematic method for identifying the absorption lines in
  quasi-stellar sources with rich absorption spectra is described, and
  the lines that are expected on theoretical grounds to have the highest
  probability of appearing in absorption in quasi-stellar sources are
  listed. The computational scheme that was devel- oped for recognizing
  and analyzing candidate redshifts is then described; this computationa'
  scheme is supplemented by a set of rules used to determine if a
  candidate redshift is acceptable The computational scheme and formal
  rules were applied to a set of nonsense spectra, i.e, random-number
  spectra, with the same main characteristics as the absorption spectrum
  of PKS 0237-23 determined by Greenstein and Sargent The average number
  of acceptable redshifts per nonsense spectrum was 0.7. Five acceptable
  redshifts were found in the real spectrum: z = 2 2015, 1.671, 1 656,
  1.513, and 1.364 No acceptable redshift was found at z = 1 95. A list
  of additional lines that should be detectable if the identifications
  proposed here are correct is given for slightly longer and shorter
  wavelengths than covered in the observa- tions of Greenstein and
  Sargent Some characteristics of the identifications are also described

---------------------------------------------------------
Title: Solar Models and Neutrino Fluxes
Authors: Bahcall, John N.; Shaviv, Giora
1968ApJ...153..113B    Altcode:
  We have derived a set of accurate models for the interior of the
  present Sun by varying within their accepted limits all the parameters,
  except the gravitational constant, at our disposal. Our principal
  con- clusions are: (1) the 8B neutrino flux is 1.3(1 ± 0.6) X 10~
  neutrinos cm2 sec1 at Earth's surface if the uncertainties are assumed
  to combine like statistical errors; (2) the primordial helium mass
  fraction probably lies in the range 0.24-0.28; (3) the primordial
  heavy-element mass fraction probably lies in the range 0.018-0.036;
  (4) the fraction of energy generated by the CNO cycle is 0.03 ± 0.02;
  and (5) the luminosity of the Sun has increased by about 35 per cent in
  the last 4.7 billion years. We also present three numerical models for
  the solar interior and discuss some of their principal characteristics

---------------------------------------------------------
Title: Neutrino absorption by deuterium
Authors: Ellis, S. D.; Bahcall, J. N.
1968NuPhA.114..636E    Altcode:
  The cross section for the reaction <SUP>2</SUP>H(ν,e<SUP>-</SUP>)2p
  has been calculated as a function of neutrino energy using the
  effective range method to approximate the required nuclear matrix
  element. The cross section was averaged over the shape of the neutrino
  spectra from the decay of <SUP>15</SUP>O and <SUP>8</SUP>B. The
  results are σ<SUB>av</SUB>(<SUP>15</SUP>O)=1.05× 10 <SUP>-47</SUP>
  cm<SUP>2</SUP> and σ<SUB>av</SUB>(<SUP>8</SUP>B)=1.20×10<SUP>-42</SUP>
  cm<SUP>2</SUP>. The uncertainty of both values is estimated to be
  +/-10%. <P />Alfred P. Sloan Foundation Fellow.

---------------------------------------------------------
Title: Fine-Structure Transitions
Authors: Bahcall, John N.; Wolf, Richard A.
1968ApJ...152..701B    Altcode:
  We calculate collision cross-sections and photon transition
  probabilities for many cases of practical interest. Using the calculated
  rates, we show how the fine structure of absorption lines can be used
  as an indicator of the density of the absorbing medium or the ambient
  intensity of a strong photon flux. For densities much greater than a
  critical value, ~ or for very high photon fluxes, the fine-structure
  levels of the ground state of a given ion are populated according
  to a Boltzmann distribution (which for most practical cases means
  according to the ratio of degeneracies) For densities much less than
  Ncr and moderate photon fluxes, only the lowest fine structure state
  is populated The value of N0~ is calculated for the most abundant ions
  that have resonant absorption lines with wavelengths greater than 950
  A by evaluating the rates of the photon and collisional transitions
  among the fine structure levels. Cross-sec- tions for collisional
  excitation by protons have been calculated by numerical integration
  of the relevant time-dependent Schroedinger equation for six ions of
  interest and these detailed calculations are used to obtain accurate
  estimates of the proton-excitation cross-sections for a number of
  other cases. The prob- ability of exciting fine-structure levels of
  both neutral and charged ions by collisions with hydrogen atoms has
  been estimated. The rates of magnetic-dipole photon decays, as well
  as cross-sections for colli- sional excitation of fine-structure
  levels by electrons, have been calculated from previously published
  results. Applications are made to problems involving the interstellar
  medium, circumstellar envelopes of giant stars, the solar corona,
  planetary nebulae, the intergalactic medium, and quasi-stellar source

---------------------------------------------------------
Title: Present Status of the Theoretical Predictions for the
    <SUP>36</SUP>Cl Solar-Neutrino Experiment
Authors: Bahcall, John N.; Bahcall, Neta A.; Shaviv, Giora
1968PhRvL..20.1209B    Altcode:
  The theoretical predictions for the <SUP>37</SUP>Cl solar-neutrino
  experiment are summarized and compared with the experimental results
  of Davis, Harmer, and Hoffman. Three important conclusions about the
  sun are shown to follow.

---------------------------------------------------------
Title: The Rate of the Proton-Proton Reaction
Authors: Bahcall, John N.; May, Robert M.
1968ApJ...152L..17B    Altcode:
  The rate of the proton-proton reaction has been recalculated. Our value
  for the low-energy cross- section factor is S(E = 0) = (3.78 ± 0.15)
  X 10-25 MeV barns, which is 12.5 per cent larger than the value in
  current usage. The effect of our larger calculated S(E = 0) on the
  8fi solar neutrino flux and on the rate of nuclear-energy generation
  in the proton-proton chain is briefly discussed

---------------------------------------------------------
Title: Electron Scattering and Tests of Cosmological Models
Authors: Bahcall, John N.; May, Robert M.
1968ApJ...152...37B    Altcode:
  We discuss the effect of photon scattering by electrons on the
  magnitude-redshift, count-magnitude, and number-redshift relationships
  in Friedmann cosmologies. I. INTRODUCTIO

---------------------------------------------------------
Title: Mixing in the Sun and Neutrino Fluxes
Authors: Bahcall, J. N.; Bahcall, N. A.; Ulrich, R. K.
1968ApL.....2...91B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Does the Fine-Structure Constant Vary with Cosmic Time?
Authors: Bahcall, John N.; Schmidt, Maarten
1967PhRvL..19.1294B    Altcode:
  The fine structure constant at red shifts Δλλ~0.2, corresponding
  to an epoch around two billion years ago, has been determined using
  the wavelengths of a pair of O III emission lines measured in the
  spectra of five radio galaxies. We find α(z=0.2)α(lab)=1.001+/-0.002
  probable error.

---------------------------------------------------------
Title: Dependence of the ^8{B} Solar Neutrino Flux on the Rate of
    the Reaction ^3He(^3He,2p)<SUP>4</SUP>He
Authors: Shaviv, Giora; Bahcall, John N.; Fowler, William A.
1967ApJ...150..725S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Dependence of the ^8{B} Solar Neutrino Flux on Heavy Element
    Composition
Authors: Bahcall, John N.; Cooper, Martin; Demarque, Pierre
1967ApJ...150..723B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Carbon to Silicon Ratio in 3C 191
Authors: Bahcall, J. N.; Kozlovsky, B. Z.; Sargent, W. L. W.;
   Schmidt, M.
1967PASP...79..425B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Brans-Dicke Cosmology and the Solar Neutrino Flux
Authors: Shaviv, G.; Bahcall, J. N.
1967PASP...79..438S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Phenomenological Limits on the Absorbing Regions of
    Quasi-Stellar Sources
Authors: Bahcall, John N.
1967ApJ...149L...7B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: An Analysis of the Absorption Spectrum of 3c 191
Authors: Bahcall, John N.; Sargent, Wallace L. W.; Schmidt, Maarten
1967ApJ...149L..11B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Predicted Emission Spectra of Quasi-Stellar Sources in the
    Far Ultraviolet
Authors: Bahcall, John N.; Sargent, Wallace L. W.
1967ApJ...148L..65B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On the fine structure of absorption lines
Authors: Bahcall, J. N.; Wolf, R. A.; Salpeter, E. E.
1967AJ.....72Q.290B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: An Interpretation of the Absorption Spectrum of 3c 191
Authors: Bahcall, John N.
1966ApJ...146..615B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On Some Predicted and Observed Features of Quasi-Stellar
    Sources
Authors: Bahcall, John N.
1966ApJ...145..684B    Altcode:
  Some observed features of quasi-stellar sources are correlated in a way
  that enables one to predict with simple models the relative strengths of
  the Lyman lines and the optical depth of the nebulae beyond the Lyman
  continuum. The relative strengths of the Lyman lines are calculated
  first for an optically thin nebula, and then expressions are derived
  for the amount by which the intensities of the more energetic Lyman
  lines are attenuated in an optically thick nebula. The probability
  that resonant radiation escapes from an optically thick nebula is
  estimated with a diffusion equation and is found to be much larger than
  previously estimated if some emission originates near the surface of
  the nebula. Three possible causes for the observed emission widths are
  discussed, and it is concluded that the most likely cause is random
  motions of gas clumps or filaments. A suggestion due to Schmidt for
  constructing models of quasi-stellar sources that are optically thin
  to electron scattering is developed quantitatively. The average degree
  of ionization of the hydrogen in a quasi-stellar source and the optical
  depth beyond the Lyman continuum are expressed in terms of the unknown
  ionizing flux. A plausible guess for the strength of the ionizing flux
  indicates that some quasi-stellar sources may be optically thin beyond
  the Lyman continuum. A possible correlation is suggested between the
  age (and luminosity) of the nebula of a quasi-stellar source and the
  value of its optical depth beyond the Lyman continuum. Several other
  observational consequences of our discussion are also described. In
  particular the predictions are shown to depend sensitively on whether
  or not quasi-stellar sources are, like the nuclei of Seyfert galaxies,
  surrounded by an appreciable amount of neutral hydrogen.

---------------------------------------------------------
Title: Solar Neutrinos
Authors: Bahcall, John N.
1966PhRvL..17..398B    Altcode:
  The predicted capture rate in the Cl<SUP>37</SUP> experiment for
  detecting solar neutrinos is calculated using the results of recent
  nuclear experiments and solar-model investigations. It is shown that
  additional experiments (e.g., with H<SUP>2</SUP>, Li<SUP>7</SUP>,
  B<SUP>11</SUP>, or ν-e scattering) are necessary to establish the
  relative contributions of the proton-proton chain and the CNO cycle
  to solar energy generation.

---------------------------------------------------------
Title: On the Absorption Spectrum of 1116+12
Authors: Bahcall, John N.; Peterson, Bruce A.; Schmidt, Maarten
1966ApJ...145..369B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Absorption Lines in the Spectra of Distant Sources
Authors: Bahcall, John N.; Salpeter, E. E.
1966ApJ...144..847B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On the Problem of Detecting Solar Neutrinos
Authors: Bahcall, John N.; Davis, Raymond, Jr.
1966stev.conf..241B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Non-Resonant Nuclear Reactions at Stellar Temperatures.
Authors: Bahcall, John N.
1966ApJ...143..259B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Neutron Stars. II. Neutrino-Cooling and Observability
Authors: Bahcall, John N.; Wolf, Richard A.
1965PhRv..140.1452B    Altcode:
  Calculations of the rates of the cooling reactions
  n+n--&gt;n+p+e<SUP>-</SUP>+ν<SUB>e</SUB> and
  n+π<SUP>-</SUP>--&gt;n+e<SUP>-</SUP>+ν<SUB>e</SUB> are presented;
  the rates of the closely related muon-producing reactions and the
  four inverse processes are also given. Several different arguments
  are used to obtain estimates of the relavant matrix elements. The
  nucleons are assumed to form a normal Fermi fluid with a continuous
  excitation spectrum. The calculated cooling rates indicate that
  a neutron star containing quasifree pions would cool within a few
  days to a temperature so low that the star would be unobservable. The
  surface of a star that does not contain quasifree pions would cool to
  10<SUP>7</SUP> °K in a few months and would reach 4×10<SUP>6</SUP>
  °K in about 100 years. The calculated cooling rates strongly indicate
  that the discrete x-ray sources located in the direction of the galactic
  center are not neutron stars.

---------------------------------------------------------
Title: Neutron Stars. I. Properties at Absolute Zero Temperature
Authors: Bahcall, John N.; Wolf, Richard A.
1965PhRv..140.1445B    Altcode:
  The properties of a neutron star at absolute zero temperature are
  discussed. The problem of determining the ground state of a neutron
  star is formulated in a general way and the conditions are described
  under which one might reasonably hope that an individual-particle model
  (which we adopt) is valid. The effects of the strong interactions on
  the number densities and production thresholds of the various hadrons
  are illustrated with several examples. The modification of the energy
  spectrum of neutrons and protons in a neutron star is calculated using
  an effective-mass approximation adapted from the theory of nuclear
  matter. Crude estimates are made of the contributions of hadrons other
  than nucleons to the equation of state and specific heat.

---------------------------------------------------------
Title: On the Interaction of Radiation from Distant Sources with
    the Intervening Medium.
Authors: Bahcall, John N.; Salpeter, E. E.
1965ApJ...142.1677B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: An Observational Test of Theories of Neutron-Star Cooling.
Authors: Bahcall, John N.; Wolf, Richard A.
1965ApJ...142.1254B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Neutron Stars
Authors: Bahcall, John N.; Wolf, Richard A.
1965PhRvL..14..343B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Observational Neutrino Astronomy
Authors: Bahcall, John N.
1965Sci...147..115B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Neutrino-spectroscopy of the solar interior
Authors: Bahcall, J. N.
1964PhL....13..332B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Neutrino Opacity. II. Neutrino-Nucleon Interactions
Authors: Bahcall, John N.; Frautschi, Steven C.
1964PhRv..136.1547B    Altcode:
  The contribution of neutrino-nucleon interactions to the neutrino
  opacity of matter is studied, special attention being paid to possible
  astrophysical applications such as supernova explosions. The results
  of recent accelerator experiments with high-energy neutrinos are
  used to show that nonresonant neutrino-nucleon scattering does
  not make a significant contribution to the neutrino opacity for
  astrophysically important conditions. The results of deep-mine
  cosmic-ray studies are then used to show that, (a) there are no
  resonances in the ν<SUB>μ</SUB>-nucleon and ν¯<SUB>μ</SUB>-nucleon
  systems with masses less than 60 BeV (laboratory neutrino energies
  &lt;2×10<SUP>+3</SUP> BeV), and (b) there are no resonances in the
  ν<SUB>e</SUB>-neucleon and ν¯<SUB>e</SUB>-nucleon systems with masses
  less than 7 BeV (laboratory neutrino energies &lt;30 BeV). Neutrino
  absorption by bound nucleons is also discussed and a sum rule is
  proved for neutrino capture that is sufficiently accurate for most
  astrophysical applications. The effect of the exclusion principle on the
  capture cross sections is described and some applications to specific
  nuclei are presented. The accelerator experiments with high-energy
  neutrinos are then used to show that neutrino radioactivity, i.e.,
  nuclear de-excitation by emission of a neutrino-antineutrino pair,
  is a substantially less important mechanism for stellar energy loss
  than was suggested by some previous estimates.

---------------------------------------------------------
Title: Neutrino Opacity I. Neutrino-Lepton Scattering
Authors: Bahcall, John N.
1964PhRv..136.1164B    Altcode:
  The contribution of neutrino-lepton scattering to the total neutrino
  opacity of matter is investigated; it is found that, contrary
  to previous beliefs, neutrino scattering dominates the neutrino
  opacity for many astrophysically important conditions. The rates for
  neutrino-electron scattering and antineutrino-electron scattering
  are given for a variety of conditions, including both degenerate and
  nondegenerate gases; the rates for some related reactions are also
  presented. Formulas are given for the mean scattering angle and the mean
  energy loss in neutrino and antineutrino scattering. Applications are
  made to the following problems: (a) the detection of solar neutrinos;
  (b) the escape of neutrinos from stars; (c) neutrino scattering in
  cosmology; and (d) energy deposition in supernova explosions.

---------------------------------------------------------
Title: Neutrino Astronomy and Intermediate Bosons
Authors: Bahcall, John N.; Frautschi, Steven C.
1964PhRv..135..788B    Altcode:
  Neutrino fluxes from strong radio sources are
  estimated, assuming the neutrino-production mechanism:
  p+p--&gt;nucleons+mesons--&gt;nucleons+electrons, gamma rays, and
  neutrinos. The neutrino fluxes calculated on the basis of this mechanism
  are too small to be easily detected unless there are resonances in
  neutrino processes associated with the production of intermediate
  bosons. It is shown that a resonance in the antineutrino-electron
  system, associated with the usually hypothesized W<SUP>-</SUP>
  resonance, could be used to test, with standard experimental techniques,
  whether strong radio sources emit high-energy neutrinos in the
  quantities estimated in this paper. Two kinds of observational tests
  are described and counting rates are estimated. Observational tests
  of the kind we propose would provide important information about:
  (1) the mechanism for production of high-energy electrons in strong
  radio sources, and (2) the magnetic fields in such sources. Some
  comments concerning other logically possible neutrino resonances are
  also included.

---------------------------------------------------------
Title: Termination of the Proton-Proton Chain in Stellar Interiors.
Authors: Parker, Peter D.; Bahcall, John N.; Fowler, William A.
1964ApJ...139..602P    Altcode:
  The roles of the various H2-burning and He3-burning reactions in
  the termination of the proto proton chain in stellar interiors have
  been re-examined using (1) recent experimental determinations the
  cross-sections for the H2(p, )He3 and He3(a, )Be7 reactions, (2)
  theoretical studies of the rates the relevant beta-decay reactions,
  and (3) a re-examination of the previous cross-section factor detern
  nations for the other possible reactions in the proton-proton chain.

---------------------------------------------------------
Title: Terminating the Proton-Proton Chain at High Densities.
Authors: Bahcall, John N.; Wolf, Richard A.
1964ApJ...139..622B    Altcode:
  The rate of the He3(e , ) reaction is calculated as a function
  of stellar temperature and den. using the modern theory of nuclear
  beta-decay. Three tritium-burning sequences of nuclear reactions also
  studied. Some possible applications are discussed briefly.

---------------------------------------------------------
Title: Electron Capture in Stellar Interiors.
Authors: Bahcall, John N.
1964ApJ...139..318B    Altcode:
  The reasons why nuclear electron-capture rates in stars depend
  on temperature and density are discussed, and some astrophysical
  applications of continuum electron-capture rates are reviewed. The
  modern theory of nuclear P-decay is then used to calculate
  stellar-continuum electron-capture rates for transitions of an
  arbitrary degree of forbiddenness. The equations that are most useful
  for astrophysical applications are discussed in detail; particular
  emphasis is placed upon methods for predicting stellar rates that
  utilize, whenever possible, terrestrial measurements. Three examples are
  discussed that illustrate the use of the formulae given in this paper;
  the examples are: (a) the electron-capture lifetime of a proton, (b)
  the stellar p-decay of K40, and (c) the effect of forbidden transitions
  on the abundances of elements in the iron peak.

---------------------------------------------------------
Title: Exclusion Principle Inhibition of Beta Decay in Stellar
    Interiors.
Authors: Peterson, Vern L.; Bahcall, John N.
1963ApJ...138..437P    Altcode:
  Beta decay in a high-density electron gas is investigated. It is shown
  that the exclusion principle can play an important role in determining
  the decay rate Tables describing allowed, flrst4orbidden non- unique,
  and first-forbidden unique decays are presented; these tables give
  the dependence of the beta- decay rate on the local temperature,
  electron density, and beta-decay energy. If the Fermi energy of
  the free electrons exceeds the beta-decay energy, the decay rate is
  strongly inhibited; the amount of inhibition decreases with increasing
  temperature. The relativistic dependence of the degeneracy parameter
  on temperature and electron density is also tabulated.

---------------------------------------------------------
Title: Solar Neutrino Flux.
Authors: Bahcall, J. N.; Fowler, William A.; Iben, I., Jr.; Sears,
   R. L.
1963ApJ...137..344B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Exclusion principle inhibition of beta decay in stellar
    interiors
Authors: Peterson, Vern Leroy; Bahcall, John N.
1963PGLO...54..437P    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Exclusion Principle and Photobeta Reactions in
    Nucleogenesis.
Authors: Bahcall, John N.
1962ApJ...136..445B    Altcode:
  The effects of the exclusion principle and photobeta reactions on the
  formation of heavy elements by slow-neutron capture are discussed. It
  is shown that a measurement of the isotopic abundance of Zr93 in giant
  stars exhibiting technetium lines would permit inferences concerning
  the temperature of the nuclear reacting core in which the heavy elements
  were produced.

---------------------------------------------------------
Title: Beta Decay in Stellar Interiors
Authors: Bahcall, John N.
1962PhRv..126.1143B    Altcode:
  A study is made of the temperature and density dependence of beta-decay
  rates as they are affected by electron capture from continuum orbits,
  the absence of atomic binding energies, screening, and the exclusion
  principle. The rate of allowed electron capture from continuum orbits
  in a Fermi gas is calculated using the V-A law; Coulomb corrections
  are included and nuclear matrix elements occur as parameters that can
  frequently be determined from terrestrial experiments. There is no
  atomic binding-energy contribution to the total beta-decay energy
  for completely ionized atoms and this causes a decrease in decay
  rates for low-energy electron emitters in stars relative to their
  terrestrial values. Screening will usually not affect beta-decay rates
  significantly. The exclusion principle inhibits beta decay in stellar
  interiors because many of the low-momentum states are occupied prior
  to the decay; the amount by which a decay rate is decreased can be
  calculated in terms of the known beta spectrum and the temperature
  and density of the medium surrounding the radioactive nucleus. Beta
  decay for some normally radioactive nuclei is almost impossible in the
  interior of very dense stars, such as white dwarfs, since the Fermi
  energy can equal or exceed the maximum beta-decay energy available. Some
  applications to the theory of element formation in stars are suggested.

---------------------------------------------------------
Title: Theory of Bound-State Beta Decay
Authors: Bahcall, John N.
1961PhRv..124..495B    Altcode:
  The theory of beta-decay processes in which an electron is
  created in a bound atomic state is developed in the allowed
  approximation. The correlations and total decay rate are calculated
  with the renormalized V-A theory and the results are valid for atoms
  of arbitrary electronic configuration. The relative probability of
  bound-state to continuum-state decay is shown to be independent of
  nuclear matrix elements; some bound-state decay rates are presented
  that were calculated by making use of this fact. The possibility of
  experimentally detecting bound-state decay is also briefly examined. The
  beta decay of nuclei in stellar interiors is discussed and a number
  of examples are presented for which bound-state decay is more likely
  than continuum-state decay under the conditions that obtain in stellar
  interiors.