Author name code: hall ADS astronomy entries on 2022-09-14 author:"Hall, Jeffrey C." ------------------------------------------------------------------------ Title: Snowmass 2021 Scintillating Bubble Chambers: Liquid-noble Bubble Chambers for Dark Matter and CE$\nu$NS Detection Authors: Alfonso-Pita, E.; Baker, M.; Behnke, E.; Bressler, M.; Broerman, B.; Clark, K.; Corbett, J.; Cripe, C.; Crisler, M.; Dahl, C. E.; Dering, K.; de St. Croix, A.; Durnford, D.; Foy, K.; Giampa, P.; Hall, J.; Harris, O.; Hawley-Herrera, H.; Jackson, C. M.; Ko, Y.; Lamb, N.; Laurin, M.; Levine, I.; Lippincott, W. H.; Liu, X.; Neilson, R.; Pal, S.; Piro, M. -C.; Priya, S.; Sheng, Z.; Sloss, A.; Struyk, X.; Vázquez-Jáuregui, E.; Westerdale, S.; Whitis, T. J.; Zha, W.; Zhang, R. Bibcode: 2022arXiv220712400A Altcode: The Scintillating Bubble Chamber (SBC) Collaboration is developing liquid-noble bubble chambers for the quasi-background-free detection of low-mass (GeV-scale) dark matter and coherent scattering (CE$\nu$NS) of low-energy (MeV-scale) neutrinos. The first physics-scale demonstrator of this technique, a 10-kg liquid argon bubble chamber dubbed SBC-LAr10, is now being commissioned at Fermilab. This device will calibrate the background discrimination power and sensitivity of superheated argon to nuclear recoils at energies down to 100 eV. A second functionally-identical detector with a focus on radiopure construction is being built for SBC's first dark matter search at SNOLAB. The projected spin-independent sensitivity of this search is approximately $10^{-43}$ cm$^2$ at 1 GeV$/c^2$ dark matter particle mass. The scalability and background discrimination power of the liquid-noble bubble chamber make this technique a compelling candidate for future dark matter searches to the solar neutrino fog at 1 GeV$/c^2$ particle mass (requiring a $\sim$ton-year exposure with non-neutrino backgrounds sub-dominant to the solar CE$\nu$NS signal) and for high-statistics CE$\nu$NS studies at nuclear reactors. Title: Ionization yield measurement in a germanium CDMSlite detector using photo-neutron sources Authors: Albakry, M. F.; Alkhatib, I.; Amaral, D. W. P.; Aralis, T.; Aramaki, T.; Arnquist, I. J.; Ataee Langroudy, I.; Azadbakht, E.; Banik, S.; Bathurst, C.; Bauer, D. A.; Bezerra, L. V. S.; Bhattacharyya, R.; Bowles, M. A.; Brink, P. L.; Bunker, R.; Cabrera, B.; Calkins, R.; Cameron, R. A.; Cartaro, C.; Cerdeño, D. G.; Chang, Y. -Y.; Chaudhuri, M.; Chen, R.; Chott, N.; Cooley, J.; Coombes, H.; Corbett, J.; Cushman, P.; De Brienne, F.; di Vacri, M. L.; Diamond, M. D.; Fascione, E.; Figueroa-Feliciano, E.; Fink, C. W.; Fouts, K.; Fritts, M.; Gerbier, G.; Germond, R.; Ghaith, M.; Golwala, S. R.; Hall, J.; Hines, B. A.; Hollister, M. I.; Hong, Z.; Hoppe, E. W.; Hsu, L.; Huber, M. E.; Iyer, V.; Jastram, A.; Kashyap, V. K. S.; Kelsey, M. H.; Kubik, A.; Kurinsky, N. A.; Lawrence, R. E.; Lee, M.; Li, A.; Liu, J.; Liu, Y.; Loer, B.; Lukens, P.; MacDonell, D.; MacFarlane, D. B.; Mahapatra, R.; Mandic, V.; Mast, N.; Mayer, A. J.; Meyer zu Theenhausen, H.; Michaud, É.; Michielin, E.; Mirabolfathi, N.; Mohanty, B.; Morales Mendoza, J. D.; Nagorny, S.; Nelson, J.; Neog, H.; Novati, V.; Orrell, J. L.; Osborne, M. D.; Oser, S. M.; Page, W. A.; Partridge, R.; Pedreros, D. S.; Podviianiuk, R.; Ponce, F.; Poudel, S.; Pradeep, A.; Pyle, M.; Rau, W.; Reid, E.; Ren, R.; Reynolds, T.; Roberts, A.; Robinson, A. E.; Saab, T.; Sadoulet, B.; Saikia, I.; Sander, J.; Sattari, A.; Scarff, A.; Schmidt, B.; Schnee, R. W.; Scorza, S.; Serfass, B.; Sincavage, D. J.; Stanford, C.; Street, J.; Thasrawala, F. K.; Toback, D.; Underwood, R.; Verma, S.; Villano, A. N.; von Krosigk, B.; Watkins, S. L.; Wen, O.; Williams, Z.; Wilson, M. J.; Winchell, J.; Wykoff, K.; Yellin, S.; Young, B. A.; Yu, T. C.; Zatschler, B.; Zatschler, S.; Zaytsev, A.; Zhang, E.; Zheng, L.; Zuber, S. Bibcode: 2022PhRvD.105l2002A Altcode: 2022arXiv220207043S Two photo-neutron sources, 88Y 9Be and 124Sb 9Be, have been used to investigate the ionization yield of nuclear recoils in the CDMSlite germanium detectors by the SuperCDMS collaboration. This work evaluates the yield for nuclear recoil energies between 1 and 7 keV at a temperature of ∼ 50 mK . We use a GEANT4 simulation to model the neutron spectrum assuming a charge yield model that is a generalization of the standard Lindhard model and consists of two energy dependent parameters. We perform a likelihood analysis using the simulated neutron spectrum, modeled background, and experimental data to obtain the best fit values of the yield model. The ionization yield between recoil energies of 1 and 7 keV is shown to be significantly lower than predicted by the standard Lindhard model for germanium. There is a general lack of agreement among different experiments using a variety of techniques studying the low energy range of the nuclear recoil yield, which is most critical for interpretation of direct dark matter searches. This suggests complexity in the physical process that many direct detection experiments use to model their primary signal detection mechanism and highlights the need for further studies to clarify underlying systematic effects that have not been well understood up to this point. Title: Effective Field Theory Analysis of CDMSlite Run 2 Data Authors: SuperCDMS Collaboration; Albakry, M. F.; Alkhatib, I.; Amaral, D. W. P.; Aralis, T.; Aramaki, T.; Arnquist, I. J.; Ataee Langroudy, I.; Azadbakht, E.; Banik, S.; Bathurst, C.; Bauer, D. A.; Bezerra, L. V. S.; Bhattacharyya, R.; Brink, P. L.; Bunker, R.; Cabrera, B.; Calkins, R.; Cameron, R. A.; Cartaro, C.; Cerdeño, D. G.; Chang, Y. -Y.; Chaudhuri, M.; Chen, R.; Chott, N.; Cooley, J.; Coombes, H.; Corbett, J.; Cushman, P.; De Brienne, F.; Dharani, S.; di Vacri, M. L.; Diamond, M. D.; Fascione, E.; Figueroa-Feliciano, E.; Fink, C. W.; Fouts, K.; Fritts, M.; Gerbier, G.; Germond, R.; Ghaith, M.; Golwala, S. R.; Hall, J.; Hassan, N.; Hines, B. A.; Hollister, M. I.; Hong, Z.; Hoppe, E. W.; Hsu, L.; Huber, M. E.; Iyer, V.; Jastram, A.; Kashyap, V. K. S.; Kelsey, M. H.; Kubik, A.; Kurinsky, N. A.; Lawrence, R. E.; Lee, M.; Li, A.; Liu, J.; Liu, Y.; Loer, B.; Lukens, P.; MacFarlane, D. B.; Mahapatra, R.; Mandic, V.; Mast, N.; Mayer, A. J.; Theenhausen, H. Meyer zu; Michaud, É.; Michielin, E.; Mirabolfathi, N.; Mohanty, B.; Nagorny, S.; Nelson, J.; Neog, H.; Novati, V.; Orrell, J. L.; Osborne, M. D.; Oser, S. M.; Page, W. A.; Partridge, R.; Pedreros, D. S.; Podviianiuk, R.; Ponce, F.; Poudel, S.; Pradeep, A.; Pyle, M.; Rau, W.; Reid, E.; Ren, R.; Reynolds, T.; Roberts, A.; Robinson, A. E.; Rogers, H. E.; Saab, T.; Sadoulet, B.; Saikia, I.; Sander, J.; Sattari, A.; Schmidt, B.; Schnee, R. W.; Scorza, S.; Serfass, B.; Poudel, S. S.; Sincavage, D. J.; Stanford, C.; Street, J.; Sun, H.; Thasrawala, F. K.; Toback, D.; Underwood, R.; Verma, S.; Villano, A. N.; von Krosigk, B.; Watkins, S. L.; Wen, O.; Williams, Z.; Wilson, M. J.; Winchell, J.; Wykoff, K.; Yellin, S.; Young, B. A.; Yu, T. C.; Zatschler, B.; Zatschler, S.; Zaytsev, A.; Zhang, E.; Zheng, L.; Zuber, S. Bibcode: 2022arXiv220511683S Altcode: CDMSlite Run 2 was a search for weakly interacting massive particles (WIMPs) with a cryogenic 600 g Ge detector operated in a high-voltage mode to optimize sensitivity to WIMPs of relatively low mass from 2 - 20 GeV/$c^2$. In this article, we present an effective field theory (EFT) analysis of the CDMSlite Run 2 data using an extended energy range and a comprehensive treatment of the expected background. A binned likelihood Bayesian analysis was performed on the recoil energy data, taking into account the parameters of the EFT interactions and optimizing the data selection with respect to the dominant background components. Energy regions within 5$\sigma$ of known activation peaks were removed from the analysis. The Bayesian evidences resulting from the different operator hypotheses show that the CDMSlite Run 2 data are consistent with the background-only models and do not allow for a signal interpretation assuming any additional EFT interaction. Consequently, upper limits on the WIMP mass and coupling-coefficient amplitudes and phases are presented for each EFT operator. These limits improve previous CDMSlite Run 2 bounds for WIMP masses above 5 GeV/$c^2$. Title: Investigating the sources of low-energy events in a SuperCDMS-HVeV detector Authors: SuperCDMS Collaboration; Albakry, M. F.; Alkhatib, I.; Amaral, D. W. P.; Aralis, T.; Aramaki, T.; Arnquist, I. J.; Ataee Langroudy, I.; Azadbakht, E.; Banik, S.; Bathurst, C.; Bauer, D. A.; Bhattacharyya, R.; Brink, P. L.; Bunker, R.; Cabrera, B.; Calkins, R.; Cameron, R. A.; Cartaro, C.; Cerdeño, D. G.; Chang, Y. -Y.; Chaudhuri, M.; Chen, R.; Chott, N.; Cooley, J.; Coombes, H.; Corbett, J.; Cushman, P.; De Brienne, F.; Dharani, S.; di Vacri, M. L.; Diamond, M. D.; Fascione, E.; Figueroa-Feliciano, E.; Fink, C. W.; Fouts, K.; Fritts, M.; Gerbier, G.; Germond, R.; Ghaith, M.; Golwala, S. R.; Hall, J.; Hassan, N.; Hines, B. A.; Hollister, M. I.; Hong, Z.; Hoppe, E. W.; Hsu, L.; Huber, M. E.; Iyer, V.; Jastram, A.; Kashyap, V. K. S.; Kelsey, M. H.; Kubik, A.; Kurinsky, N. A.; Lawrence, R. E.; Lee, M.; Li, A.; Liu, J.; Liu, Y.; Loer, B.; Lopez Asamar, E.; Lukens, P.; MacFarlane, D. B.; Mahapatra, R.; Mandic, V.; Mast, N.; Mayer, A. J.; Theenhausen, H. Meyer zu; Michaud, É.; Michielin, E.; Mirabolfathi, N.; Mohanty, B.; Nagorny, S.; Nelson, J.; Neog, H.; Novati, V.; Orrell, J. L.; Osborne, M. D.; Oser, S. M.; Page, W. A.; Partridge, R.; Pedreros, D. S.; Podviianiuk, R.; Ponce, F.; Poudel, S.; Pradeep, A.; Pyle, M.; Rau, W.; Reid, E.; Ren, R.; Reynolds, T.; Roberts, A.; Robinson, A. E.; Saab, T.; Sadoulet, B.; Saikia, I.; Sander, J.; Sattari, A.; Schmidt, B.; Schnee, R. W.; Scorza, S.; Serfass, B.; Poudel, S. S.; Sincavage, D. J.; Stanford, C.; Street, J.; Sun, H.; Thasrawala, F. K.; Toback, D.; Underwood, R.; Verma, S.; Villano, A. N.; von Krosigk, B.; Watkins, S. L.; Wen, O.; Williams, Z.; Wilson, M. J.; Winchell, J.; Wykoff, K.; Yellin, S.; Young, B. A.; Yu, T. C.; Zatschler, B.; Zatschler, S.; Zaytsev, A.; Zhang, E.; Zheng, L.; Zuber, S. Bibcode: 2022arXiv220408038S Altcode: Recent experiments searching for sub-GeV/$c^2$ dark matter have observed event excesses close to their respective energy thresholds. Although specific to the individual technologies, the measured excess event rates have been consistently reported at or below event energies of a few-hundred eV, or with charges of a few electron-hole pairs. In the present work, we operated a 1-gram silicon SuperCDMS-HVeV detector at three voltages across the crystal (0 V, 60 V and 100 V). The 0 V data show an excess of events in the tens of eV region. Despite this event excess, we demonstrate the ability to set a competitive exclusion limit on the spin-independent dark matter--nucleon elastic scattering cross section for dark matter masses of $\mathcal{O}(100)$ MeV/$c^2$, enabled by operation of the detector at 0 V potential and achievement of a very low $\mathcal{O}(10)$ eV threshold for nuclear recoils. Comparing the data acquired at 0 V, 60 V and 100 V potentials across the crystal, we investigated possible sources of the unexpected events observed at low energy. The data indicate that the dominant contribution to the excess is consistent with a hypothesized luminescence from the printed circuit boards used in the detector holder. Title: Composition and Density Stratification Observed by SuperCam in the First 300 Sols in Jezero Crater Authors: Wiens, R. C.; Udry, A.; Mangold, N.; Beyssac, O.; Quantin, C.; Sautter, V.; Cousin, A.; Brown, A.; Bosak, T.; Mandon, L.; Forni, O.; Johnson, J. R.; McLennan, S.; Legett, C.; Maurice, S.; Mayhew, L.; Anderson, R. B.; Clegg, S. M.; Ollila, A. M.; Hall, J.; Meslin, P. -Y.; Kah, L. C.; Gabriel, T. S. J.; Gasda, P.; Simon, J. I.; Hausrath, E. M.; Horgan, B.; Poulet, F.; Beck, P.; Gupta, S.; Chide, B.; Clavé, E.; Connell, S.; Dehouck, E.; Dromart, G.; Fouchet, T.; Royer, C.; Frydenvang, J.; Gasnault, O.; Gibbons, E.; Kalucha, H.; Lanza, N.; Lasue, J.; Le Mouélic, S.; Leveille, R.; Cloutis, E.; Lopez Reyes, G.; Arana, G.; Castro, K.; Madariaga, J. M.; Manrique, J. -A.; Pilorget, C.; Pinet, P.; Laserna, J.; Sharma, S. K.; Acosta-Maeda, T.; Kelly, E.; Crumpler, L.; Montmessin, F.; Fischer, W.; Francis, R.; Stack, K.; Farley, K.; SuperCam Team Bibcode: 2022LPICo2678.2075W Altcode: Exploration to date shows three compositional regions with the stratigraphically lower 2 enriched in olivine (Séitah) and pyroxene (Artuby ridge), respectively. Title: Geology of the Latmikaik and Xcacau Coronae in the Henie (V-58) Quadrangle, Venus Authors: Shackman, J.; Boggs, K. J. E.; Ernst, R. E.; Bethell, E. M.; Wehnes, H. G. D.; Varg, E.; Pendleton, C.; Jans, W.; Hall, J.; Dietrich, R. C.; Dhami, L.; Demorcy, J.; Dear, B.; Chowdhury, M.; Bley, H. N.; Becerra De Rosales, M. Bibcode: 2022LPICo2678.2693S Altcode: This abstract examines the topography of the Latmikaik and Xcacau Coronae and their relationship with graben swarms and the Tellervo Chasma. Title: What is the Extent of the Influence of the Artemis Corona Across the Henie (V-58) Quadrangle, Southern Venus? Authors: Bley, H. N.; Boggs, K. J. E.; Ernst, R. E.; Bethell, E. M.; Becerra De Rosales, M.; Beckie, B.; Chowdhury, M.; Dear, B.; Demorcy, J.; Dhami, L.; Dietrich, R. C.; Hall, J.; Jans, W.; Pendleton, C.; Shackman, J.; Varg, E.; Wehnes, H. G. D. Bibcode: 2022LPICo2678.1765B Altcode: We examine the influence of the Artemis system across the Henie Quadrangle to assess whether the Artemis system is the largest in the solar system. Title: A Strategy for Low-Mass Dark Matter Searches with Cryogenic Detectors in the SuperCDMS SNOLAB Facility Authors: SuperCDMS Collaboration; Albakry, M. F.; Alkhatib, I.; Amaral, D. W. P.; Aralis, T.; Aramaki, T.; Arnquist, I. J.; Ataee Langroudy, I.; Azadbakht, E.; Banik, S.; Bathurst, C.; Bauer, D. A.; Bhattacharyya, R.; Brink, P. L.; Bunker, R.; Cabrera, B.; Calkins, R.; Cameron, R. A.; Cartaro, C.; Cerdeno, D. G.; Chang, Y. -Y.; Chaudhuri, M.; Chen, R.; Chott, N.; Cooley, J.; Coombes, H.; Corbett, J.; Cushman, P.; De Brienne, F.; Dharani, S.; di Vacri, M. L.; Diamond, M. D.; Fascione, E.; Figueroa-Feliciano, E.; Fink, C. W.; Fouts, K.; Fritts, M.; Gerbier, G.; Germond, R.; Ghaith, M.; Golwala, S. R.; Hall, J.; Hassan, N.; Hines, B. A.; Hollister, M. I.; Hong, Z.; Hoppe, E. W.; Hsu, L.; Huber, M. E.; Iyer, V.; Jastram, A.; Kashyap, V. K. S.; Kelsey, M. H.; Kubik, A.; Kurinsky, N. A.; Lawrence, R. E.; Lee, M.; Li, A.; Liu, J.; Liu, Y.; Loer, B.; Lukens, P.; MacFarlane, D. B.; Mahapatra, R.; Mandic, V.; Mast, N.; Mayer, A. J.; Theenhausen, H. Meyer zu; Michaud, E.; Michielin, E.; Mirabolfathi, N.; Mohanty, B.; Nagorny, S.; Nelson, J.; Neog, H.; Novati, V.; Orrell, J. L.; Osborne, M. D.; Oser, S. M.; Page, W. A.; Partridge, R.; Pedreros, D. S.; Podviianiuk, R.; Ponce, F.; Poudel, S.; Pradeep, A.; Pyle, M.; Rau, W.; Reid, E.; Ren, R.; Reynolds, T.; Roberts, A.; Robinson, A. E.; Saab, T.; Sadoulet, B.; Saikia, I.; Sander, J.; Sattari, A.; Schmidt, B.; Schnee, R. W.; Scorza, S.; Serfass, B.; Poudel, S. S.; Sincavage, D. J.; Stanford, C.; Street, J.; Sun, H.; Thasrawala, F. K.; Toback, D.; Underwood, R.; Verma, S.; Villano, A. N.; von Krosigk, B.; Watkins, S. L.; Wen, O.; Williams, Z.; Wilson, M. J.; Winchell, J.; Wyko, K.; Yellin, S.; Young, B. A.; Yu, T. C.; Zatschler, B.; Zatschler, S.; Zaytsev, A.; Zhang, E.; Zheng, L.; Zuber, S. Bibcode: 2022arXiv220308463S Altcode: The SuperCDMS Collaboration is currently building SuperCDMS SNOLAB, a dark matter search focused on nucleon-coupled dark matter in the 1-5 GeV mass range. Looking to the future, the Collaboration has developed a set of experience-based upgrade scenarios, as well as novel directions, to extend the search for dark matter using the SuperCDMS technology in the SNOLAB facility. The experienced-based scenarios are forecasted to probe many square decades of unexplored dark matter parameter space below 5 GeV, covering over 6 decades in mass: 1-100 eV for dark photons and axion-like particles, 1-100 MeV for dark-photon-coupled light dark matter, and 0.05-5 GeV for nucleon-coupled dark matter. They will reach the neutrino fog in the 0.5-5 GeV mass range and test a variety of benchmark models and sharp targets. The novel directions involve greater departures from current SuperCDMS technology but promise even greater reach in the long run, and their development must begin now for them to be available in a timely fashion. The experienced-based upgrade scenarios rely mainly on dramatic improvements in detector performance based on demonstrated scaling laws and reasonable extrapolations of current performance. Importantly, these improvements in detector performance obviate significant reductions in background levels beyond current expectations for the SuperCDMS SNOLAB experiment. Given that the dominant limiting backgrounds for SuperCDMS SNOLAB are cosmogenically created radioisotopes in the detectors, likely amenable only to isotopic purification and an underground detector life-cycle from before crystal growth to detector testing, the potential cost and time savings are enormous and the necessary improvements much easier to prototype. Title: Time evolution of magnetic activity cycles in young suns: The curious case of κ Ceti Authors: Boro Saikia, S.; Lüftinger, T.; Folsom, C. P.; Antonova, A.; Alecian, E.; Donati, J. -F.; Guedel, M.; Hall, J. C.; Jeffers, S. V.; Kochukhov, O.; Marsden, S. C.; Metodieva, Y. T.; Mittag, M.; Morin, J.; Perdelwitz, V.; Petit, P.; Schmid, M.; Vidotto, A. A. Bibcode: 2022A&A...658A..16B Altcode: 2021arXiv211006000B Context. A detailed investigation of the magnetic properties of young Sun-like stars can provide valuable information on our Sun's magnetic past and its impact on the early Earth.
Aims: We determine the properties of the moderately rotating young Sun-like star κ Ceti's magnetic and activity cycles using 50 yr of chromospheric activity data and six epochs of spectropolarimetric observations.
Methods: The chromospheric activity was determined by measuring the flux in the Ca II H and K lines. A generalised Lomb-Scargle periodogram and a wavelet decomposition were used on the chromospheric activity data to establish the associated periodicities. The vector magnetic field of the star was reconstructed using the technique of Zeeman Doppler imaging on the spectropolarimetric observations.
Results: Our period analysis algorithms detect a 3.1 yr chromospheric cycle in addition to the star's well-known ~6 yr cycle period. Although the two cycle periods have an approximate 1:2 ratio, they exhibit an unusual temporal evolution. Additionally, the spectropolarimetric data analysis shows polarity reversals of the star's large-scale magnetic field, suggesting a ~10 yr magnetic or Hale cycle.
Conclusions: The unusual evolution of the star's chromospheric cycles and their lack of a direct correlation with the magnetic cycle establishes κ Ceti as a curious young Sun. Such complex evolution of magnetic activity could be synonymous with moderately active young Suns, which is an evolutionary path that our own Sun could have taken. Title: Analysis of Coronal Mass Ejections Observed by Multiple Spacecraft, including by WISPR on Parker Solar Probe Authors: Liewer, Paulett; Hall, Jeffrey; Braga, Carlos; Hess, Phillip; Penteado, Paulo; Stenborg, Guillermo; Vourlidas, Angelos; Qiu, Jiong Bibcode: 2021AGUFMSH15A2019L Altcode: The Wide-field Imager for Solar Probe (WISPR) has provided high resolution images of multiple coronal mass ejections (CMEs) during its first seven encounters with the Sun and most of these have been observed by white-light instruments on either STEREO A or SOHO or both. The multiple viewpoints have been important in determining the source of the CMEs and their trajectories. Here we present results from the analysis of the origin and trajectories of several WISPR CMEs with some unexpected results. WISPR has a wide fixed angular field-of-view (FOV), extending radially from 13.5° to 108° from the Sun and approximately 50° in the transverse direction, but the physical extent of the imaged coronal region varies directly with the distance of the spacecraft from the Sun. We have developed tools for determining the trajectories of solar ejecta which take into account the rapid spacecraft motion. We have also developed tools to relate and compare the CMEs seen in the WISPR images to simultaneous observation from the other white light telescope (SOHO/LASCO or STEREO/SECCHI), making uses of the World Coordinate System information in the images FITS headers. This software allows us to project the trajectory determined from WISPR or features seen in the WISPR images onto images from the second white light telescope (or visa versa) to verify the trajectory determined from the WISPR data alone or to determine a CMEs location by triangulation. Utilizing the multiple viewpoints has led to a better understanding of the structure and evolution of the CMEs. Title: Satellite Constellation Issues Need Science Communicators Authors: Hall, J.; Walker, C.; Krafton, K. Bibcode: 2021ASPC..531..148H Altcode: Future large constellations of bright satellites in low-Earth orbit (LEOsats) will fundamentally change observational astronomy at optical wavelengths. Nighttime images without satellite trails will no longer be the norm. If the 100,000+ LEOsats proposed are deployed, no combination of mitigations can fully avoid the impacts of satellite trails on science programs of current and planned ground-based optical astronomical facilities. Astrophotography, amateur astronomy, and the human experience of a starry night sky are already affected. The report from the Satellite Constellations 1 (SATCON1) workshop (29 June-2 July 2020), as well as the report from the Dark and Quiet Skies for Science and Society (D&QS) workshop (October 5-9 2020), support these statements. The aim of SATCON1 and the Satellite Constellation Working Group of D&QS was to better quantify the impacts of LEOsat constellations, explore possible mitigations, and make recommendations.

Mitigation strategies for the most damaging impacts on scientific programs are being actively explored by astronomers worldwide. These investigations have benefited from collaboration with SpaceX, the first operator to launch satellite constellations. SpaceX has shown that operators can reduce reflected sunlight through satellite orientation, Sun shielding, and surface darkening. A joint effort to obtain higher accuracy public data on predicted locations of satellites (or ephemerides) could enable some pointing avoidance and mid-exposure shuttering during satellite passage. Observatories need to adopt more dynamic scheduling and observation management as the number of constellation satellites increases, though these measures may prove ineffective for many science programs.

To successfully implement these next steps, more buy-in is needed from our astronomy community and the general public. What if our community of science educators and communicators could create awareness of the issues and possible mitigations? Come to our session to learn more. Title: SATCON2: Observations Working Group Report Authors: Rawls, Meredith L.; Barron, Darcy; Birdwell, Ian; Cirkovic, Elena; Deck, Tim; Di Vruno, Federico; Gokhale, Vayujeet; Goodman, Matthew; Kafka, Stella; Kebe, Fatoumata; Knox, Doug; Krantz, Harrison; Kruk, Sandor; Lawler, Samantha; Monet, Dave; Peel, Mike; Tregloan-Reed, Jeremy; Zamora, Olga; Allen, Lori; Walker, Connie; Hall, Jeffrey Bibcode: 2021zndo...5608826R Altcode: No abstract at ADS Title: SATCON2: Policy Working Group Report Authors: Green, Richard; Allen, Lori; Andrade, Bohnlein, Jurgen; Boley, Aaron; Cooper, Patricia; Dunn, Mat; Falle, Andrew; Grunsfeld, John; Hanlon, Michelle; Hartley, Ruskin; Hofer, Chris; Jakhu, Jansson, Gerry; Jones, Therese; Knox, Doug; Krafton, Kelsie; Liszt, Harvey; Mishra, Nishith; Mudd, Charles; Parriott, Joel; Rosenberg, Erica; Puxley, Phil; Raval, Vikram; Rotola, Giuliana; Sedwick, Ray; Simon-Butler, Andrew; Smith, Joshua; Vanotti, Maurizio; Walker, Connie; Williams, Andrew; Walker, Constance; Hall, Jeffrey Bibcode: 2021zndo...5609224G Altcode: The charge to the SATCON2 Policy Working Group was to review existing national policies and legislative frameworks. With the SATCON1 recommendations as context, the group was charged to assess policy options to serve the diverse requirements of astronomy, the satellite industry, and other communities. Title: SATCON2: Algorithms Working Group Report Authors: McDowell, Jonathan; Seaman, Rob; Bassa, Cees; Galadí-Enríquez, David; Hainaut, Olivier; Hodgson, Courtney; Holman, Matt; Jah, Moriba; Kavelaars, JJ. Poletti, Keith; Schmitz, Morgan; Seitzer, Pat; Siminski, Jan; Street, Rachel; Teimoorinia, Hossen; Thiemann, Heidi; Walker, Connie; Walker, Constance; Hall, Jeffrey Bibcode: 2021zndo...5608843M Altcode: No abstract at ADS Title: SATCON2: Community Engagement Working Group Report Authors: Venkatesan, Aparna; Lowenthal, James; Arion, Doug; Avila Castro, Fernando; Bannister, Michele; Barentine, John; Begay, David; Chavez, Juan-Carlos; Carttar, Sally; Gering, Rick; Hartley, Ruskin; Hall, Jeffrey; Harvey, Alvin; Heim, Jessica; Kafka, Stella; Kimura, Ka'iu; Larsen, Kris; Lee, Annette; Maryboy, Nancy; Neilson, Hilding; Nesvold, Erika; Simons, Doug; Sweitzer, James; Umpierre, Diana; Walker, Connie; Wakker, Constance Walker Bibcode: 2021zndo...5608920V Altcode: No abstract at ADS Title: SATCON2: Executive Summary Authors: Hall, Jeffrey; Walker, Constance; Rawls, Meredith; McDowell, Jonathan; Seaman, Robert; Venkatesan, Aparna; Lowenthal, James; Green, Richard; Krafton, Kelsie; Parriott, Joel Bibcode: 2021BAAS...53b0205H Altcode: No abstract at ADS Title: The Sun as a young star: reproducing the X-ray cycle of ɛ Eridani with solar magnetic structures Authors: Coffaro, M.; Stelzer, B.; Orlando, S.; Hall, J.; Metcalfe, T. S.; Wolter, U.; Mittag, M.; Sanz-Forcada, J.; Ducci, L. Bibcode: 2021csss.confE..38C Altcode: Epsilon Eri is a young solar-like star with a ~3 yr X-ray activity cycle, detected by us for the first time in a dedicated XMM-Newton long-term monitoring campaign. The magnetic structures on the Sun are intimately linked to the 11-yr activity cycle and they were spatially and temporally resolved throughout the solar cycle. However, for other stars these structures can not be spatially resolved with present-day X-ray instruments. We have, thus, developed a new technique which allows us to reproduce the stellar X-ray variability in terms of time-variations in the coverage of the corona with the same kind of magnetic structures observed on the Sun: active regions (ARs), cores of active regions (COs) and flares (FLs). This poster presents this new method and the results we obtained for the case of Epsilon Eri. Our approach is to simulate a grid of emission measure distributions (EMDs) derived from the analysis of regions observed in the solar corona to artificially reproduce a solar-like corona with the physical characteristics of Epsilon Eri. The three magnetic structures are allowed to contribute to the total coronal EMD with varying area coverage fraction. Thus, from a comparison between these pseudo-solar EMDs and the observations of Epsilon Eri, we are able to associate to each state of the X-ray activity cycle of Epsilon Eri the percentage of ARs, COs and FLs on the corona of the star. The observed amplitude of the X-ray luminosity in the cycle of Epsilon Eri is much smaller than on the Sun. Our analysis provides a physical explanation for this: the simulated EMDs indicate that in all phases of the X-ray cycle a large portion of the corona of Epsilon Eri is covered by active structures. Therefore, there is little space for adding further magnetic structures in the cycle maximum. In the future, this method will be applied to other stars providing an important contribution to better understand the solar-stellar corona connection. Title: Color Properties at the Mars InSight Landing Site Authors: Maki, J. N.; Golombek, M.; Banerdt, W.; Smrekar, S.; Deen, R.; Abarca, H.; Lu, S.; Hall, J. Bibcode: 2021E&SS....801336M Altcode: The color properties observed at the InSight landing site by the lander cameras are spectral mixtures of two source materials: gray black rocky material with chromaticity values of x = 0.32, y = 0.32 (standard deviations of σx = 0.02 and σy = 0.03) and yellowish brown dust with chromaticity values of x = 0.42, y = 0.36 (standard deviations of σx = 0.02 and σy = 0.03). These results are consistent with published values from other Mars landed missions. The InSight measurements also include the first published value of the white point of Mars daylight, chromaticity of x = 0.35, y = 0.34 (standard deviations of σx = 0.01 and σy = 0.02), which is redder than earth daylight by δx = 0.04 and δy = 0.01. InSight measurements also show a small color difference (δx = 0.02 and δy = 0.01) between the near field terrain (within 20 m of the lander) and the far field area beyond. This color difference is believed to be caused by dust being blown off by near field terrain by the lander rockets during the landing event. The visual difference between these two regions is caused primarily by the brightness variation. Chromaticity measurements of the Martian sky also match previous missions with additional variability caused by differences in dust loading and the dynamic nature of the Martian atmosphere. Title: Scientific goals for the Venus Flagship Mission's aerobot Authors: Wilson, C. F.; Gilmore, M. S.; Beauchamp, P. M.; Atreya, S. K.; Baines, K.; Goolish, E.; Bullock, M.; Curry, S.; Hall, J.; Izraelevitz, J.; Jackson, J. M.; Nikolic, D. Bibcode: 2020AGUFMP050...03W Altcode: The Venus Flagship Mission (VFM), a Decadal mission concept study, includes a variable altitude balloon operating at altitudes from 52 km (where p = 0.8 bar, T = 60°C) to 62 km (p = 0.16 bar, T = -20°C). This range allows study both of the convective cloud, found at altitudes < 60 km, and of the convectively stable upper cloud at > 60 km. This range also includes the 20-40°C "habitable zone" of Venus' clouds, one of the most benign environments known beyond Earth.

The aerobot's payload is focused in three areas: composition, meteorology, and geophysics. For composition, the key instrument is an aerosol mass spectrometer with nephelometer. It measures both gas composition and aerosol/cloud composition, using dedicated inlets for each. Astrobiology is addressed by a dedicated fluorimetric microscope, which will examine cloud droplets for minute traces of constituents associated with past or present life. Meteorological sensors include air pressure & temperature sensors, radiometer, 3-D anemometer and a radiation dosimeter. Finally, the aerobot carries payloads addressing the geophysics of the solid planet below. An infrasound sensor will search for acoustic waves triggered by tectonic and volcanic activity. Magnetic field measurements will search for remnant crustal magnetism, constrain core size and properties from magnetic field draping, and search for E-M signatures of lightning. A visible imager, taking images of the balloon and Venus cloudscapes, completes the payload. Title: Venus Drill and Sample Delivery System Authors: Zacny, K.; Hall, J. Bibcode: 2020LPICo2356.8022Z Altcode: We present development and testing of Venus drill and sample delivery system. Title: Venus Corona and Tessera Explore (VeCaTEx) Mission Concept: Investigatin the Surface of Venus from Beneath the Clouds Authors: Cutts, J.; Baines, K.; Beauchamp, P.; Bower, C.; Dais, A.; Dorsky, L.; Dyar, D.; Fesq, L.; Freeman, A.; Ghail, R.; Gilmore, M.; Grimm, R.; Gulcher, A.; Head, J.; Helbert, J.; Jackson, J.; De Jong, M.; Hall, J.; Izraelevitz, J.; Krishnamoorthy, S.; Matthies, L.; Montesi, L.; Pauken, M.; Senske, D.; Sotin, C.; Sutin, B.; Wilson, C. Bibcode: 2020LPICo2356.8031C Altcode: VeCaTEx would use an aerobot to descend repeatedly beneath the dense clouds for imaging targeted area of the surface in the near infrared spectral region to address six of the prime investigations prioritized by VEXAG. Title: New-Frontiers Class Venus In-Situ Exploration: The Venus Climate and Geophysics Mission (VCGM) Concept Authors: Baines, K. H.; Cutts, J. A.; Dorsky, L.; Hall, J.; Akins, A.; Davis, A.; Komjathy, A.; Krishnamoorthy, S.; Nikolic, D.; Vergados, P.; Akins, A.; Atreya, S.; Bullock, M.; Hunter, G.; Lebonnois, S.; Lognonne, P.; Mousis, O.; O'Rourke, J.; Renard, J. -B.; Wilson, C. Bibcode: 2020LPICo2356.8005B Altcode: A class of prolonged global-scale, in-situ Venus New Frontiers missions is described. Via an instrumented variable-altitude balloon supported by a science/comm orbiter and probes, the mission class satisfies > 80% of VEXAG GOI investigations. Title: Dark & Quiet Skies I (2020) Authors: Walker, Connie; Di Pippo, Simona; Aubé, Martin; Barentine, John; Benkhaldoun, Zouhair; Benvenuti, Piero; Bouroussis, Costis; Green, Richard; Hearnshaw, John; Mackenzie, Aoraki; Liszt, Harvey; Lowenthal, James D.; Muñoz-Tuñón, Casiana; Nield, Kathryn; Ricard, Nathalie; Rodriguez Espinosa, Jose Miguel; Sanhueza, Pedro; Varela Pérez, Antonia M.; Williams, Andrew; Lau, Steve; Muñoz Tuñón, Casiana; Rodríguez Espinosa, José M.; Muñoz-Tuñon, Casiana; Armas, Juan Pablo; Benn, Chris; Blattner, Peter; Diaz-Castro, Javier; Donners, Maurice; Douglas, Bryan; Gašparovský, Dionýz; Hall, Jeffrey; Kolláth, Zoltán; Novak, Tomas; Ortolani, Sergio; Rodríguez Espinosa, José Miguel; Lowenthal, James; Bara, Salvador; Jägerbrand, Annika; Jechow, Andreas; Longcore, Travis; Motta, Mario; Schlangen, Luc; Schroer, Sibylle; Lucatello, Sara; Galadí-Enríquez, David; Micheva, Genoveva; Otarola, Angel; Allen, Lori; Bannister, Michelle; Barstow, Martin; Bassa, Cees; Davies, Roger; Devost, Daniel; Hainaut, Olivier; Jah, Moriba; Krafton, Kelsie; Krantz, Harry; Kucharski, Daniel; Maclay, Timothy; Massey, Robert; Mudd, Charles, Jr.; McDowell, Jonathan; Parriott, Joel; Pearce, Eric; Rawls, Meredith; Rotola, Giuliana; Seaman, Rob; Seitzer, Patrick; Siminski, Jan; Storrie-Lombardi, Lisa; Street, Rachel; Tregloan-Reed, Jeremy; Tyson, J. Anthony; Unda-Sanzana, Eduardo; Wainscoat, Richard; Zamora, Olga Bibcode: 2020dqs1.rept.....W Altcode: Upon request from the United Nations Committee on the Peaceful Uses of Outer Space (COPUOS), the UN Office of Outer Space Affairs, the International Astronomical Union and Spain are organising a Conference on "Dark and Quiet Skies for Science and Society", postponed to April 2021 [n.b. subsequently postponed to October 2021] due to the Covid-19 pandemic. An online Workshop took place from 5 to 9 October 2020 to discuss initial findings and draft recommendations. The present report is the outcome from this Workshop; the recommendations it contains will be reviewed during the forthcoming Conference with the aim to be presented to the COPUOS Meeting in June 2021.

The purpose and scope of the Conference and Workshop is to propose to COPUOS a set of recommendations, to be acted upon either by local governments or agreed to at an international level, aimed at protecting the science of astronomy. (It is not intended to include these recommendations into wider Space Treaties, their scope being solely confined to the protection of the science of astronomy.) Title: Velocity independent constraints on spin-dependent DM-nucleon interactions from IceCube and PICO Authors: Aartsen, M. G.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Alispach, C.; Andeen, K.; Anderson, T.; Ansseau, I.; Anton, G.; Argüelles, C.; Auffenberg, J.; Axani, S.; Backes, P.; Bagherpour, H.; Bai, X.; Balagopal V., A.; Barbano, A.; Barwick, S. W.; Bastian, B.; Baum, V.; Baur, S.; Bay, R.; Beatty, J. J.; Becker, K. -H.; Becker Tjus, J.; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Bohm, C.; Börner, M.; Böser, S.; Botner, O.; Böttcher, J.; Bourbeau, E.; Bourbeau, J.; Bradascio, F.; Braun, J.; Bron, S.; Brostean-Kaiser, J.; Burgman, A.; Buscher, J.; Busse, R. S.; Carver, T.; Chen, C.; Cheung, E.; Chirkin, D.; Choi, S.; Classen, L.; Coleman, A.; Collin, G. H.; Conrad, J. M.; Coppin, P.; Correa, P.; Cowen, D. F.; Cross, R.; Dave, P.; De Clercq, C.; DeLaunay, J. J.; Dembinski, H.; Deoskar, K.; De Ridder, S.; Desiati, P.; de Vries, K. D.; de Wasseige, G.; de With, M.; DeYoung, T.; Diaz, A.; Díaz-Vélez, J. C.; Dujmovic, H.; Dunkman, M.; Dvorak, E.; Eberhardt, B.; Ehrhardt, T.; Eller, P.; Engel, R.; Evenson, P. A.; Fahey, S.; Fazely, A. R.; Felde, J.; Filimonov, K.; Finley, C.; Franckowiak, A.; Friedman, E.; Fritz, A.; Gaisser, T. K.; Gallagher, J.; Ganster, E.; Garrappa, S.; Gerhardt, L.; Ghorbani, K.; Glauch, T.; Glüsenkamp, T.; Goldschmidt, A.; Gonzalez, J. G.; Grant, D.; Griffith, Z.; Griswold, S.; Günder, M.; Gündüz, M.; Haack, C.; Hallgren, A.; Halve, L.; Halzen, F.; Hanson, K.; Haungs, A.; Hebecker, D.; Heereman, D.; Heix, P.; Helbing, K.; Hellauer, R.; Henningsen, F.; Hickford, S.; Hignight, J.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Hoinka, T.; Hokanson-Fasig, B.; Hoshina, K.; Huang, F.; Huber, M.; Huber, T.; Hultqvist, K.; Hünnefeld, M.; Hussain, R.; In, S.; Iovine, N.; Ishihara, A.; Japaridze, G. S.; Jeong, M.; Jero, K.; Jones, B. J. P.; Jonske, F.; Joppe, R.; Kang, D.; Kang, W.; Kappes, A.; Kappesser, D.; Karg, T.; Karl, M.; Karle, A.; Katz, U.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; Kim, J.; Kintscher, T.; Kiryluk, J.; Kittler, T.; Klein, S. R.; Koirala, R.; Kolanoski, H.; Köpke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Kowalski, M.; Krings, K.; Krückl, G.; Kulacz, N.; Kurahashi, N.; Kyriacou, A.; Labare, M.; Lanfranchi, J. L.; Larson, M. J.; Lauber, F.; Lazar, J. P.; Leonard, K.; Leszczynska, A.; Leuermann, M.; Liu, Q. R.; Lohfink, E.; Lozano Mariscal, C. J.; Lu, L.; Lucarelli, F.; Lünemann, J.; Luszczak, W.; Lyu, Y.; Ma, W. Y.; Madsen, J.; Maggi, G.; Mahn, K. B. M.; Makino, Y.; Mallik, P.; Mallot, K.; Mancina, S.; Mariş, I. C.; Maruyama, R.; Mase, K.; Maunu, R.; McNally, F.; Meagher, K.; Medici, M.; Medina, A.; Meier, M.; Meighen-Berger, S.; Menne, T.; Merino, G.; Meures, T.; Micallef, J.; Momenté, G.; Montaruli, T.; Moore, R. W.; Morse, R.; Moulai, M.; Muth, P.; Nagai, R.; Naumann, U.; Neer, G.; Niederhausen, H.; Nowicki, S. C.; Nygren, D. R.; Pollmann, A. Obertacke; Oehler, M.; Olivas, A.; O'Murchadha, A.; O'Sullivan, E.; Palczewski, T.; Pandya, H.; Pankova, D. V.; Park, N.; Peiffer, P.; Pérez de los Heros, C.; Philippen, S.; Pieloth, D.; Pinat, E.; Pizzuto, A.; Plum, M.; Porcelli, A.; Price, P. B.; Przybylski, G. T.; Raab, C.; Raissi, A.; Rameez, M.; Rauch, L.; Rawlins, K.; Rea, I. C.; Reimann, R.; Relethford, B.; Renschler, M.; Renzi, G.; Resconi, E.; Rhode, W.; Richman, M.; Robertson, S.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk, D.; Safa, I.; Sanchez Herrera, S. E.; Sandrock, A.; Sandroos, J.; Santander, M.; Sarkar, S.; Sarkar, S.; Satalecka, K.; Schaufel, M.; Schieler, H.; Schlunder, P.; Schmidt, T.; Schneider, A.; Schneider, J.; Schröder, F. G.; Schumacher, L.; Sclafani, S.; Seckel, D.; Seunarine, S.; Shefali, S.; Silva, M.; Snihur, R.; Soedingrekso, J.; Soldin, D.; Song, M.; Spiczak, G. M.; Spiering, C.; Stachurska, J.; Stamatikos, M.; Stanev, T.; Stein, R.; Steinmüller, P.; Stettner, J.; Steuer, A.; Stezelberger, T.; Stokstad, R. G.; Stössl, A.; Strotjohann, N. L.; Stürwald, T.; Stuttard, T.; Sullivan, G. W.; Taboada, I.; Tenholt, F.; Ter-Antonyan, S.; Terliuk, A.; Tilav, S.; Tomankova, L.; Tönnis, C.; Toscano, S.; Tosi, D.; Trettin, A.; Tselengidou, M.; Tung, C. F.; Turcati, A.; Turcotte, R.; Turley, C. F.; Ty, B.; Unger, E.; Unland Elorrieta, M. A.; Usner, M.; Vandenbroucke, J.; Van Driessche, W.; van Eijk, D.; van Eijndhoven, N.; Vanheule, S.; van Santen, J.; Vraeghe, M.; Walck, C.; Wallace, A.; Wallraff, M.; Wandkowsky, N.; Watson, T. B.; Weaver, C.; Weindl, A.; Weiss, M. J.; Weldert, J.; Wendt, C.; Werthebach, J.; Whelan, B. J.; Whitehorn, N.; Wiebe, K.; Wiebusch, C. H.; Wille, L.; Williams, D. R.; Wills, L.; Wolf, M.; Wood, J.; Wood, T. R.; Woschnagg, K.; Wrede, G.; Xu, D. L.; Xu, X. W.; Xu, Y.; Yanez, J. P.; Yodh, G.; Yoshida, S.; Yuan, T.; Zöcklein, M.; IceCube Collaboration; Amole, C.; Ardid, M.; Arnquist, I. J.; Asner, D. M.; Baxter, D.; Behnke, E.; Bressler, M.; Broerman, B.; Cao, G.; Chen, C. J.; Chowdhury, U.; Clark, K.; Collar, J. I.; Cooper, P. S.; Crisler, M.; Crowder, G.; Cruz-Venegas, N. A.; Dahl, C. E.; Das, M.; Fallows, S.; Farine, J.; Felis, I.; Filgas, R.; Girard, F.; Giroux, G.; Hall, J.; Hardy, C.; Harris, O.; Hoppe, E. W.; Jin, M.; Klopfenstein, L.; Krauss, C. B.; Laurin, M.; Lawson, I.; Leblanc, A.; Levine, I.; Lippincott, W. H.; Mamedov, F.; Maurya, D.; Mitra, P.; Moore, C.; Nania, T.; Neilson, R.; Noble, A. J.; Oedekerk, P.; Ortega, A.; Piro, M. -C.; Plante, A.; Podviyanuk, R.; Priya, S.; Robinson, A. E.; Sahoo, S.; Scallon, O.; Seth, S.; Sonnenschein, A.; Starinski, N.; Štekl, I.; Sullivan, T.; Tardif, F.; Vázquez-Jáuregui, E.; Walkowski, N.; Wichoski, U.; Yan, Y.; Zacek, V.; Zhang, J.; PICO Collaboration Bibcode: 2020EPJC...80..819A Altcode: 2019arXiv190712509I Adopting the Standard Halo Model (SHM) of an isotropic Maxwellian velocity distribution for dark matter (DM) particles in the Galaxy, the most stringent current constraints on their spin-dependent scattering cross-section with nucleons come from the IceCube neutrino observatory and the PICO-60 C3F8 superheated bubble chamber experiments. The former is sensitive to high energy neutrinos from the self-annihilation of DM particles captured in the Sun, while the latter looks for nuclear recoil events from DM scattering off nucleons. Although slower DM particles are more likely to be captured by the Sun, the faster ones are more likely to be detected by PICO. Recent N-body simulations suggest significant deviations from the SHM for the smooth halo component of the DM, while observations hint at a dominant fraction of the local DM being in substructures. We use the method of Ferrer et al. (JCAP 1509: 052, 2015) to exploit the complementarity between the two approaches and derive conservative constraints on DM-nucleon scattering. Our results constrain σSD≲3 ×10-39cm2 (6 ×10-38cm2 ) at ≳90 % C.L. for a DM particle of mass 1 TeV annihilating into τ+τ- (b b ¯ ) with a local density of ρDM=0.3 GeV/cm 3 . The constraints scale inversely with ρDM and are independent of the DM velocity distribution. Title: Impact of Satellite Constellations on Optical Astronomy and Recommendations Toward Mitigations Authors: Walker, Constance; Hall, Jeffrey; Allen, Lori; Green, Richard; Seitzer, Patrick; Tyson, Tony; Bauer, Amanda; Krafton, Kelsie; Lowenthal, James; Parriott, Joel; Puxley, Phil; Abbott, Tim; Bakos, Gaspar; Barentine, John; Bassa, Cees; Blakeslee, John; Bradshaw, Andrew; Cooke, Jeff; Devost, Daniel; Galadí-Enríquez, David; Haase, Flynn; Hainaut, Olivier; Heathcote, Steve; Jah, Moriba; Krantz, Harrison; Kucharski, Daniel; McDowell, Jonathan; Mróz, Przemek; Otarola, Angel; Pearce, Eric; Rawls, Meredith; Saunders, Clare; Seaman, Rob; Siminski, Jan; Snyder, Adam; Storrie-Lombardi, Lisa; Tregloan-Reed, Jeremy; Wainscoat, Richard; Williams, Andrew; Yoachim, Peter Bibcode: 2020BAAS...52.0206W Altcode: 2020BAAS...52b0206W In May 2019 SpaceX launched its first batch of 60 Starlink communication satellites, which surprised astronomers and laypeople with their appearance in the night sky. Astronomers have only now, a little over a year later, accumulated enough observations of constellation satellites like those being launched by SpaceX and OneWeb, and run computer simulations of their likely impact when fully deployed, to thoroughly understand the magnitude and complexity of the problem. This research informed the discussion at the Satellite Constellations 1 (SATCON1) workshop held virtually 29 June to 2 July 2020 and led to recommendations for observatories and constellation operators. The SATCON1 report concludes that the effects on astronomical research and on the human experience of the night sky range from "negligible" to "extreme." Title: An X-ray activity cycle on the young solar-like star ɛ Eridani Authors: Coffaro, M.; Stelzer, B.; Orlando, S.; Hall, J.; Metcalfe, T. S.; Wolter, U.; Mittag, M.; Sanz-Forcada, J.; Schneider, P. C.; Ducci, L. Bibcode: 2020A&A...636A..49C Altcode: 2020arXiv200211009C Chromospheric Ca II activity cycles are frequently found in late-type stars, but no systematic programs have been created to search for their coronal X-ray counterparts. The typical time scale of Ca II activity cycles ranges from years to decades. Therefore, long-lasting missions are needed to detect the coronal counterparts. The XMM-Newton satellite has so far detected X-ray cycles in five stars. A particularly intriguing question is at what age (and at what activity level) X-ray cycles set in. To this end, in 2015 we started the X-ray monitoring of the young solar-like star ɛ Eridani, previously observed on two occasions: in 2003 and in early 2015, both by XMM-Newton. With an age of 440 Myr, it is one of the youngest solar-like stars with a known chromospheric Ca II cycle. We collected the most recent Mount Wilson S-index data available for ɛ Eridani, starting from 2002, including previously unpublished data. We found that the Ca II cycle lasts 2.92 ± 0.02 yr, in agreement with past results. From the long-term XMM-Newton lightcurve, we find clear and systematic X-ray variability of our target, consistent with the chromospheric Ca II cycle. The average X-ray luminosity is 2 × 1028erg s-1, with an amplitude that is only a factor of 2 throughout the cycle. We apply a new method to describe the evolution of the coronal emission measure distribution of ɛ Eridani in terms of solar magnetic structures: active regions, cores of active regions, and flares covering the stellar surface at varying filling fractions. Combinations of these three types of magnetic structures can only describe the observed X-ray emission measure of ɛ Eridani if the solar flare emission measure distribution is restricted to events in the decay phase. The interpretation is that flares in the corona of ɛ Eridani last longer than their solar counterparts. We ascribe this to the lower metallicity of ɛ Eridani. Our analysis also revealed that the X-ray cycle of ɛ Eridani is strongly dominated by cores of active regions. The coverage fraction of cores throughout the cycle changes by the same factor as the X-ray luminosity. The maxima of the cycle are characterized by a high percentage of covering fraction of the flares, consistent with the fact that flaring events are seen in the corresponding short-term X-ray lightcurves predominately at the cycle maxima. The high X-ray emission throughout the cycle of ɛ Eridani is thus explained by the high percentage of magnetic structures on its surface. Title: Geology of the InSight landing site on Mars Authors: Golombek, M.; Warner, N. H.; Grant, J. A.; Hauber, E.; Ansan, V.; Weitz, C. M.; Williams, N.; Charalambous, C.; Wilson, S. A.; DeMott, A.; Kopp, M.; Lethcoe-Wilson, H.; Berger, L.; Hausmann, R.; Marteau, E.; Vrettos, C.; Trussell, A.; Folkner, W.; Le Maistre, S.; Mueller, N.; Grott, M.; Spohn, T.; Piqueux, S.; Millour, E.; Forget, F.; Daubar, I.; Murdoch, N.; Lognonné, P.; Perrin, C.; Rodriguez, S.; Pike, W. T.; Parker, T.; Maki, J.; Abarca, H.; Deen, R.; Hall, J.; Andres, P.; Ruoff, N.; Calef, F.; Smrekar, S.; Baker, M. M.; Banks, M.; Spiga, A.; Banfield, D.; Garvin, J.; Newman, C. E.; Banerdt, W. B. Bibcode: 2020NatCo..11.1014G Altcode: The Interior Exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) spacecraft landed successfully on Mars and imaged the surface to characterize the surficial geology. Here we report on the geology and subsurface structure of the landing site to aid in situ geophysical investigations. InSight landed in a degraded impact crater in Elysium Planitia on a smooth sandy, granule- and pebble-rich surface with few rocks. Superposed impact craters are common and eolian bedforms are sparse. During landing, pulsed retrorockets modified the surface to reveal a near surface stratigraphy of surficial dust, over thin unconsolidated sand, underlain by a variable thickness duricrust, with poorly sorted, unconsolidated sand with rocks beneath. Impact, eolian, and mass wasting processes have dominantly modified the surface. Surface observations are consistent with expectations made from remote sensing data prior to landing indicating a surface composed of an impact-fragmented regolith overlying basaltic lava flows. Title: The SNOLAB underground laboratory Authors: Hall, J. Bibcode: 2020JPhCS1468a2252H Altcode: The SNOLAB laboratory is 2 kilometers undeground in Sudbury, Ontario, Canada. The depth of this location results in a reduction of cosmic-radiation induced muons to the negligible level of one muon per square meter per day. The laboratory maintains cleanliness standards to control the radioactivity from dust falling out of the air, from human activity, and from research equipment brought into the lab. The resulting low-radiation environment enables a variety of research, and SNOLAB is focused on rare-event searches such as dark matter searches and nuclear decay studies. In order to enable and advance these research topics, SNOLAB is conducting research and development into cleanliness, low-level assay, radioactive gasses and cryogenics. SNOLAB collaborates, and competes, with other underground laboratories on these research and development topics, as well as operational topics, to support the global research community. Title: Flagstaff's Dark Sky Heritage Authors: Hall, J. Bibcode: 2020AAS...23518106H Altcode: Flagstaff, Arizona has a 60-year tradition of dark sky preservation, beginning with a 1958 ordinance to ban advertising searchlights. The current ordinance, enacted in 1989, is the most comprehensive in the world; it specifies not only shielding and maximum illumination requirements, but strict control of the emission spectrum via use of low pressure sodium (LPS) lamps. As of the end of May 2019, LPS lamps have been discontinued by lighting manufacturers, so Flagstaff, like many cities worldwide, will be switching its outdoor street lighting system to LEDs. We have spent several years working with City staff to develop what will again be world-leading standards in outdoor illumination, making extensive use of narrow band amber (NBA) and phosphor-converted amber (PCA) LEDs rather than white LEDs. We have already installed NBA and PCA test fixtures in several areas around town, and retrofit of all 3,700 fixtures in Flagstaff should occur in the next 2-5 years. These standards will set the precedent for other applications such as commercial properties and parking lots (pictured below). In this iPoster, I will review the history of dark sky preservation in Flagstaff, the current state of affairs in outdoor lighting, the types of LEDs available, their impact on the night sky, and how Flagstaff will preserve its exceptionally dark sky in the LED era. Title: Data-driven modeling of electron recoil nucleation in PICO C3F8 bubble chambers Authors: Amole, C.; Ardid, M.; Arnquist, I. J.; Asner, D. M.; Baxter, D.; Behnke, E.; Bressler, M.; Broerman, B.; Cao, G.; Chen, C. J.; Chen, S.; Chowdhury, U.; Clark, K.; Collar, J. I.; Cooper, P. S.; Coutu, C. B.; Cowles, C.; Crisler, M.; Crowder, G.; Cruz-Venegas, N. A.; Dahl, C. E.; Das, M.; Fallows, S.; Farine, J.; Filgas, R.; Fuentes, J.; Girard, F.; Giroux, G.; Hackett, B.; Hagen, A.; Hall, J.; Hardy, C.; Harris, O.; Hillier, T.; Hoppe, E. W.; Jackson, C. M.; Jin, M.; Klopfenstein, L.; Kozynets, T.; Krauss, C. B.; Laurin, M.; Lawson, I.; Leblanc, A.; Levine, I.; Licciardi, C.; Lippincott, W. H.; Loer, B.; Mamedov, F.; Mitra, P.; Moore, C.; Nania, T.; Neilson, R.; Noble, A. J.; Oedekerk, P.; Ortega, A.; Pal, S.; Piro, M. -C.; Plante, A.; Priya, S.; Robinson, A. E.; Sahoo, S.; Scallon, O.; Seth, S.; Sonnenschein, A.; Starinski, N.; Štekl, I.; Sullivan, T.; Tardif, F.; Tiwari, D.; Vázquez-Jáuregui, E.; Wagner, J. M.; Walkowski, N.; Weima, E.; Wichoski, U.; Wierman, K.; Woodley, W.; Yan, Y.; Zacek, V.; Zhang, J.; PICO Collaboration Bibcode: 2019PhRvD.100h2006A Altcode: 2019arXiv190512522A The primary advantage of moderately superheated bubble chamber detectors is their simultaneous sensitivity to nuclear recoils from weakly interacting massive particle (WIMP) dark matter and insensitivity to electron recoil backgrounds. A comprehensive analysis of PICO gamma calibration data demonstrates for the first time that electron recoils in C3F8 scale in accordance with a new nucleation mechanism, rather than one driven by a hot spike as previously supposed. Using this semiempirical model, bubble chamber nucleation thresholds may be tuned to be sensitive to lower energy nuclear recoils while maintaining excellent electron recoil rejection. The PICO-40L detector will exploit this model to achieve thermodynamic thresholds as low as 2.8 keV while being dominated by single-scatter events from coherent elastic neutrino-nucleus scattering of solar neutrinos. In one year of operation, PICO-40L can improve existing leading limits from PICO on spin-dependent WIMP-proton coupling by nearly an order of magnitude for WIMP masses greater than 3 GeV c-2 and will have the ability to surpass all existing non-xenon bounds on spin-independent WIMP-nucleon coupling for WIMP masses from 3 to 40 GeV c-2 . Title: Light Pollution, Radio Interference, and Space Debris: Threats and Opportunities in the 2020s Authors: Hall, Jeffrey; Allen, Lori; Arion, Douglas; Barentine, John; Caton, Daniel; Liszt, Harvey; Lowenthal, James; McKenna, Dan; Pipkin, Ashley; Seitzer, Patrick; Walker, Constance Bibcode: 2019BAAS...51g..97H Altcode: 2019astro2020U..97H In this white paper, we will outline threats to astronomy in the areas of light pollution, radio interference, and space debris, and we will specify key principles and policy points that the AAS and other advocates can use in mitigating these threats. Title: Dark matter search results from the complete exposure of the PICO-60 C3F8 bubble chamber Authors: Amole, C.; Ardid, M.; Arnquist, I. J.; Asner, D. M.; Baxter, D.; Behnke, E.; Bressler, M.; Broerman, B.; Cao, G.; Chen, C. J.; Chowdhury, U.; Clark, K.; Collar, J. I.; Cooper, P. S.; Coutu, C. B.; Cowles, C.; Crisler, M.; Crowder, G.; Cruz-Venegas, N. A.; Dahl, C. E.; Das, M.; Fallows, S.; Farine, J.; Felis, I.; Filgas, R.; Girard, F.; Giroux, G.; Hall, J.; Hardy, C.; Harris, O.; Hillier, T.; Hoppe, E. W.; Jackson, C. M.; Jin, M.; Klopfenstein, L.; Kozynets, T.; Krauss, C. B.; Laurin, M.; Lawson, I.; Leblanc, A.; Levine, I.; Licciardi, C.; Lippincott, W. H.; Loer, B.; Mamedov, F.; Mitra, P.; Moore, C.; Nania, T.; Neilson, R.; Noble, A. J.; Oedekerk, P.; Ortega, A.; Piro, M. -C.; Plante, A.; Podviyanuk, R.; Priya, S.; Robinson, A. E.; Sahoo, S.; Scallon, O.; Seth, S.; Sonnenschein, A.; Starinski, N.; Štekl, I.; Sullivan, T.; Tardif, F.; Vázquez-Jáuregui, E.; Walkowski, N.; Weima, E.; Wichoski, U.; Wierman, K.; Yan, Y.; Zacek, V.; Zhang, J.; PICO Collaboration Bibcode: 2019PhRvD.100b2001A Altcode: 2019arXiv190204031A Final results are reported from operation of the PICO-60 C3F8 dark matter detector, a bubble chamber filled with 52 kg of C3 F8 located in the SNOLAB underground laboratory. The chamber was operated at thermodynamic thresholds as low as 1.2 keV without loss of stability. A new blind 1404-kg-day exposure at 2.45 keV threshold was acquired with approximately the same expected total background rate as the previous 1167-kg-day exposure at 3.3 keV. This increased exposure is enabled in part by a new optical tracking analysis to better identify events near detector walls, permitting a larger fiducial volume. These results set the most stringent direct-detection constraint to date on the weakly interacting massive particle (WIMP)-proton spin-dependent cross section at 3.2 ×1 0-41 cm2 for a 25 GeV WIMP, improving on previous PICO results for 3-5 GeV WIMPs by an order of magnitude. Title: An Overview of Imaging from the InSight Lander Authors: Maki, J. N.; Trebi-Ollennu, A.; Banerdt, W. B.; Sorice, C.; Bailey, P.; Khan, O.; Kim, W.; Ali, K.; Lim, G.; Deen, R.; Abarca, H.; Ruoff, N.; Hollins, G.; Andres, P.; Hall, J.; InSight Operations Team; InSight Science Team Bibcode: 2019LPICo2089.6403M Altcode: After landing on Mars on November 2018, the InSight lander began returning image data from two color cameras. This overview talk will provide a summary of the image data acquired. Title: The PDS 110 observing campaign - photometric and spectroscopic observations reveal eclipses are aperiodic Authors: Osborn, H. P.; Kenworthy, M.; Rodriguez, J. E.; de Mooij, E. J. W.; Kennedy, G. M.; Relles, H.; Gomez, E.; Hippke, M.; Banfi, M.; Barbieri, L.; Becker, I. S.; Benni, P.; Berlind, P.; Bieryla, A.; Bonnoli, G.; Boussier, H.; Brincat, S. M.; Briol, J.; Burleigh, M. R.; Butterley, T.; Calkins, M. L.; Chote, P.; Ciceri, S.; Deldem, M.; Dhillon, V. S.; Dose, E.; Dubois, F.; Dvorak, S.; Esquerdo, G. A.; Evans, D. F.; Ferratfiat, S.; Fossey, S. J.; Günther, M. N.; Hall, J.; Hambsch, F. -J.; Herrero, E.; Hills, K.; James, R.; Jayawardhana, R.; Kafka, S.; Killestein, T. L.; Kotnik, C.; Latham, D. W.; Lemay, D.; Lewin, P.; Littlefair, S.; Lopresti, C.; Mallonn, M.; Mancini, L.; Marchini, A.; McCormac, J. J.; Murawski, G.; Myers, G.; Papini, R.; Popov, V.; Quadri, U.; Quinn, S. N.; Raynard, L.; Rizzuti, L.; Robertson, J.; Salvaggio, F.; Scholz, A.; Sfair, R.; Smith, A. M. S.; Southworth, J.; Tan, T. G.; Vanaverbeke, S.; Waagen, E. O.; Watson, C. A.; West, R. G.; Winter, O. C.; Wheatley, P. J.; Wilson, R. W.; Zhou, G. Bibcode: 2019MNRAS.485.1614O Altcode: 2019arXiv190107981O; 2019MNRAS.tmp..287O PDS 110 is a young disc-hosting star in the Orion OB1A association. Two dimming events of similar depth and duration were seen in 2008 (WASP) and 2011 (KELT), consistent with an object in a closed periodic orbit. In this paper, we present data from a ground-based observing campaign designed to measure the star both photometrically and spectroscopically during the time of predicted eclipse in 2017 September. Despite high-quality photometry, the predicted eclipse did not occur, although coherent structure is present suggesting variable amounts of stellar flux or dust obscuration. We also searched for radial velocity (RV) oscillations caused by any hypothetical companion and can rule out close binaries to 0.1Ms. A search of Sonneberg plate archive data also enabled us to extend the photometric baseline of this star back more than 50 yr, and similarly does not re-detect any deep eclipses. Taken together, they suggest that the eclipses seen in WASP and KELT photometry were due to aperiodic events. It would seem that PDS 110 undergoes stochastic dimmings that are shallower and of shorter duration than those of UX Ori variables, but may have a similar mechanism. Title: Imaging from the InSight Lander Authors: Maki, J. N.; Trebi-Ollennu, A.; Banerdt, W. B.; Sorice, C.; Bailey, P.; Khan, O.; Kim, W.; Ali, K.; Lim, G.; Deen, R.; Abarca, H.; Ruoff, N.; Hollins, G.; Andres, P.; Hall, J. Bibcode: 2019LPI....50.2176M Altcode: A view from the Mars InSight lander, as seen from the Instrument Deployment Camera (IDC) and Instrument Context Camera (ICC). Title: VizieR Online Data Catalog: 24 years monitoring of Sun and Sun-like stars (Radick+, 2018) Authors: Radick, R. R.; Lockwood, G. W.; Henry, G. W.; Hall, J. C.; Pevtsov, A. A. Bibcode: 2019yCat..18550075R Altcode: Starting in the late 1970s, variations in total solar irradiance (TSI) have been monitored by radiometers aboard a series of spacecraft, including the Total Irradiance Monitor (TIM) instrument on the SOlar Radiation and Climate Experiment (SORCE) satellite from 2003 to the present.

Observations to monitor relatively bright stars very similar to the Sun have been made with the Solar-Stellar Spectrograph (SSS) at Lowell Observatory and automatic photometric telescopes (APTs) at Fairborn Observatory beginning in 1992 and 1993, respectively. In all, 72 stars, including 18 from the broader R98-L07 (1998ApJS..118..239R and 2007ApJS..171..260L) sample, have been observed at both locations, some for as long as 24 seasons. These joint observations provide the primary stellar data for this paper.

(3 data files). Title: Nuclear-recoil energy scale in CDMS II silicon dark-matter detectors Authors: Agnese, R.; Anderson, A. J.; Aramaki, T.; Baker, W.; Balakishiyeva, D.; Banik, S.; Barker, D.; Basu Thakur, R.; Bauer, D. A.; Binder, T.; Borgland, A.; Bowles, M. A.; Brink, P. L.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Calkins, R.; Cartaro, C.; Cerdeño, D. G.; Chang, Y. -Y.; Chagani, H.; Chen, Y.; Cooley, J.; Cornell, B.; Cushman, P.; Daal, M.; Doughty, T.; Dragowsky, E. M.; Esteban, L.; Fallows, S.; Fascione, E.; Figueroa-Feliciano, E.; Fritts, M.; Gerbier, G.; Germond, R.; Ghaith, M.; Godfrey, G. L.; Golwala, S. R.; Hall, J.; Harris, H. R.; Holmgren, D.; Hong, Z.; Hsu, L.; Huber, M. E.; Iyer, V.; Jardin, D.; Jastram, A.; Jena, C.; Kelsey, M. H.; Kennedy, A.; Kubik, A.; Kurinsky, N. A.; Leder, A.; Lopez Asamar, E.; Lukens, P.; MacDonell, D.; Mahapatra, R.; Mandic, V.; Mast, N.; McCarthy, K. A.; Miller, E. H.; Mirabolfathi, N.; Moffatt, R. A.; Mohanty, B.; Moore, D.; Morales Mendoza, J. D.; Nelson, J.; Oser, S. M.; Page, K.; Page, W. A.; Partridge, R.; Penalver Martinez, M.; Pepin, M.; Phipps, A.; Poudel, S.; Pyle, M.; Qiu, H.; Rau, W.; Redl, P.; Reisetter, A.; Roberts, A.; Rogers, H. E.; Robinson, A. E.; Saab, T.; Sadoulet, B.; Sander, J.; Schneck, K.; Schnee, R. W.; Scorza, S.; Senapati, K.; Serfass, B.; Speller, D.; Di Stefano, P. C. F.; Stein, M.; Street, J.; Tanaka, H. A.; Toback, D.; Underwood, R.; Villano, A. N.; von Krosigk, B.; Welliver, B.; Wilson, J. S.; Wilson, M. J.; Wright, D. H.; Yellin, S.; Yen, J. J.; Young, B. A.; Zhang, X.; Zhao, X. Bibcode: 2018NIMPA.905...71A Altcode: 2018arXiv180302903A The Cryogenic Dark Matter Search (CDMS II) experiment aims to detect dark matter particles that elastically scatter from nuclei in semiconductor detectors. The resulting nuclear-recoil energy depositions are detected by ionization and phonon sensors. Neutrons produce a similar spectrum of low-energy nuclear recoils in such detectors, while most other backgrounds produce electron recoils. The absolute energy scale for nuclear recoils is necessary to interpret results correctly. The energy scale can be determined in CDMS II silicon detectors using neutrons incident from a broad-spectrum 252Cf source, taking advantage of a prominent resonance in the neutron elastic scattering cross section of silicon at a recoil (neutron) energy near 20 (182) keV. Results indicate that the phonon collection efficiency for nuclear recoils is 4.8-0.9+0.7 % lower than for electron recoils of the same energy. Comparisons of the ionization signals for nuclear recoils to those measured previously by other groups at higher electric fields indicate that the ionization collection efficiency for CDMS II silicon detectors operated at ∼4 V/cm is consistent with 100% for nuclear recoils below 20 keV and gradually decreases for larger energies to ∼75% at 100 keV. The impact of these measurements on previously published CDMS II silicon results is small. Title: Many interesting things are afoot at the Navy Precision Optical Interferometer Authors: van Belle, G. T.; Armstrong, J. T.; Benson, J. A.; Baines, E. K.; Bevilacqua, R. G.; Buschmann, T.; Clark, J. H.; DeGroff, W. T.; Hall, J. C.; Hindsley, R. L.; Jorgensen, A.; Lindgren, A.; Mozurkewich, D.; Muterspaugh, M.; Pooler, S. T.; Restaino, S. R.; Schmitt, H. R.; Shankland, P.; Zavala, R. T. Bibcode: 2018SPIE10701E..05V Altcode: The Navy Precision Optical Interferometer (NPOI) is currently undergoing a fundamental renaissance in its functionality and capabilities. Operationally, its fast delay line (FDL) infrastructure is completing its upgrade from a VME/VxWorks foundation to a modern PC/RTLinux core. The Classic beam combiner is being upgraded with the New Classic FPGA-based backend, and the VISION beam combiner has been upgraded over this past summer with low-noise EMCCD cameras, resulting in substantial gains in sensitivity. Building on those infrastructure improvements, substantial upgrades are also in progress. Three 1-meter PlaneWave CDK1000 telescopes are being delivered to the site, along with their relocatable enclosure-transporters, and stations are being commissioned for those telescopes with baselines ranging from 8 meters to 432 meters. Baseline-wavelength bootstrapping will be implemented on the facility back-end with a near-infrared beam combiner under development. Collectively, these improvements mark substantial progress in taking the facility towards realizing its full intrinsic potential. Title: Patterns of Variation for the Sun and Sun-like Stars Authors: Radick, Richard R.; Lockwood, G. Wesley; Henry, Gregory W.; Hall, Jeffrey C.; Pevtsov, Alexei A. Bibcode: 2018ApJ...855...75R Altcode: We compare patterns of variation for the Sun and 72 Sun-like stars by combining total and spectral solar irradiance measurements between 2003 and 2017 from the SORCE satellite, Strömgren b, y stellar photometry between 1993 and 2017 from Fairborn Observatory, and solar and stellar chromospheric Ca II H+K emission observations between 1992 and 2016 from Lowell Observatory. The new data and their analysis strengthen the relationships found previously between chromospheric and brightness variability on the decadal timescale of the solar activity cycle. Both chromospheric H+K and photometric b, y variability among Sun-like stars are related to average chromospheric activity by power laws on this timescale. Young active stars become fainter as their H+K emission increases, and older, less active, more Sun-age stars tend to show a pattern of direct correlation between photometric and chromospheric emission variations. The directly correlated pattern between total solar irradiance and chromospheric Ca II emission variations shown by the Sun appears to extend also to variations in the Strömgren b, y portion of the solar spectrum. Although the Sun does not differ strongly from its stellar age and spectral class mates in the activity and variability characteristics that we have now studied for over three decades, it may be somewhat unusual in two respects: (1) its comparatively smooth, regular activity cycle, and (2) its rather low photometric brightness variation relative to its chromospheric activity level and variation, perhaps indicating that facular emission and sunspot darkening are especially well-balanced on the Sun. Title: Development of the Venera-D Mission Concept, from Science Objectives to Mission Architecture Authors: Senske, D.; Zasova, L.; Burdanov, A.; Economou, T.; Eismont, N.; Gerasimov, M.; Gorinov, D.; Hall, J.; Ignatiev, N.; Ivanov, M.; Lea Jessup, K.; Khatuntsev, I.; Korablev, O.; Kremic, T.; Limaye, S.; Lomakin, I.; Martynov, M.; Ocampo, A.; Teselkin, S.; Vaisberg, O.; Voronstsov, V. Bibcode: 2018LPI....49.1243S Altcode: The development of the Venera-D concept is ongoing, focusing on science goals and mission architecture. Title: LED Street Lighting Solutions: Flagstaff, Arizona as a Case Study Authors: Hall, Jeffrey C. Bibcode: 2018AAS...23112207H Altcode: Dark-sky protection in Flagstaff, Arizona extends back to 1958, with the first ordinance in the City banning advertising floodlights. The current ordinance, adopted in 1989, is comprehensive and has played a critical role in maintaining the quality of the night sky for astronomy, tourism, public enjoyment, and other purposes. Flagstaff, like many communities around the world, is now working on a transition from legacy bulb-based technology to LED for its outdoor lighting. The City, Lowell Observatory, the U. S. Naval Observatory, and the Flagstaff Dark Skies Coalition have been working intensively for two years to identify an LED-based street lighting solution that will preserve the City's dark skies while meeting municipal needs. We will soon be installing test fixtures for an innovative solution incorporating narrow-band amber LED and modest amounts of low-CCT white LED. In this talk, I will review the types of LEDs available for outdoor lighting and discuss the plans for Flagstaff's street lighting in the LED era, which we hope will be a model for communities worldwide. Title: Protecting Dark Skies as a State-Wide Resource Authors: Allen, Lori E.; Walker, Constance E.; Hall, Jeffrey C.; Larson, Steve; Williams, Grant; Falco, Emilio; Hinz, Joannah; Fortin, Pascal; Brocious, Dan; Corbally, Christopher; Gabor, Paul; Veillet, Christian; Shankland, Paul; Jannuzi, Buell; Cotera, Angela; Luginbuhl, Christian Bibcode: 2018AAS...23114208A Altcode: The state of Arizona contains the highest concentration of research telescopes in the continental United States, contributing more than a quarter of a billion dollars annually to the state's economy. Protecting the dark skies above these observatories is both good for astronomy and good for the state's economy. In this contribution we describe how a coalition of Arizona observatories is working together to protect our dark skies. Efforts date back to the creation of one of the first Outdoor Lighting Codes in the United States and continue today, including educational outreach, public policy engagement, and consensus building. We review some proven strategies, highlight recent successes and look at current threats. Title: A Regional, Multi-Stakeholder Collaboration for Dark-Sky Protection in Flagstaff, Arizona Authors: Hall, Jeffrey C. Bibcode: 2018AAS...23114204H Altcode: Flagstaff, Arizona is home to almost $200M in astronomical assets, including Lowell Observatory's 4.3-meter Discovery Channel Telescope and the Navy Precision Optical Interferometer, a partnership of Lowell, the U. S. Naval Observatory, and the Naval Research Laboratory. The City of Flagstaff and surrounding Coconino County have comprehensive and effective dark-sky ordinances, but continued regional growth has the potential to degrade the area's dark skies to a level at which observatory missions could be compromised. As a result, a wide array of stakeholders (the observatories, the City, the County, local dark-sky advocates, the business and tourism communities, the national parks and monuments, the Navajo Nation, the U. S. Navy, and others) have engaged in three complementary efforts to ensure that Flagstaff and Coconino County protect the area's dark skies while meeting the needs of the various communities and providing for continued growth and development. In this poster, I will present the status of Flagstaff's conversion to LED outdoor lighting, the Mission Compatibility Study carried out by the Navy to evaluate the dark-sky effects of buildout in Flagstaff, and the Joint Land Use Study (JLUS) presently underway among all the aforementioned stakeholders. Taken in sum, the efforts represent a comprehensive and constructive approach to dark-sky preservation region-wide, and they show what can be achieved when a culture of dark-sky protection is present and deliberate efforts are undertaken to maintain it for decades to come. Title: Low-mass dark matter search with CDMSlite Authors: Agnese, R.; Anderson, A. J.; Aralis, T.; Aramaki, T.; Arnquist, I. J.; Baker, W.; Balakishiyeva, D.; Barker, D.; Basu Thakur, R.; Bauer, D. A.; Binder, T.; Bowles, M. A.; Brink, P. L.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Calkins, R.; Cartaro, C.; Cerdeño, D. G.; Chang, Y.; Chagani, H.; Chen, Y.; Cooley, J.; Cornell, B.; Cushman, P.; Daal, M.; Di Stefano, P. C. F.; Doughty, T.; Esteban, L.; Fascione, E.; Figueroa-Feliciano, E.; Fritts, M.; Gerbier, G.; Ghaith, M.; Godfrey, G. L.; Golwala, S. R.; Hall, J.; Harris, H. R.; Hong, Z.; Hoppe, E. W.; Hsu, L.; Huber, M. E.; Iyer, V.; Jardin, D.; Jastram, A.; Jena, C.; Kelsey, M. H.; Kennedy, A.; Kubik, A.; Kurinsky, N. A.; Leder, A.; Loer, B.; Lopez Asamar, E.; Lukens, P.; MacDonell, D.; Mahapatra, R.; Mandic, V.; Mast, N.; Miller, E. H.; Mirabolfathi, N.; Moffatt, R. A.; Mohanty, B.; Morales Mendoza, J. D.; Nelson, J.; Orrell, J. L.; Oser, S. M.; Page, K.; Page, W. A.; Partridge, R.; Pepin, M.; Peñalver Martinez, M.; Phipps, A.; Poudel, S.; Pyle, M.; Qiu, H.; Rau, W.; Redl, P.; Reisetter, A.; Reynolds, T.; Roberts, A.; Robinson, A. E.; Rogers, H. E.; Saab, T.; Sadoulet, B.; Sander, J.; Schneck, K.; Schnee, R. W.; Scorza, S.; Senapati, K.; Serfass, B.; Speller, D.; Stein, M.; Street, J.; Tanaka, H. A.; Toback, D.; Underwood, R.; Villano, A. N.; von Krosigk, B.; Welliver, B.; Wilson, J. S.; Wilson, M. J.; Wright, D. H.; Yellin, S.; Yen, J. J.; Young, B. A.; Zhang, X.; Zhao, X.; SuperCDMS Collaboration Bibcode: 2018PhRvD..97b2002A Altcode: The SuperCDMS experiment is designed to directly detect weakly interacting massive particles (WIMPs) that may constitute the dark matter in our Galaxy. During its operation at the Soudan Underground Laboratory, germanium detectors were run in the CDMSlite mode to gather data sets with sensitivity specifically for WIMPs with masses <10 GeV /c2 . In this mode, a higher detector-bias voltage is applied to amplify the phonon signals produced by drifting charges. This paper presents studies of the experimental noise and its effect on the achievable energy threshold, which is demonstrated to be as low as 56 eVee (electron equivalent energy). The detector-biasing configuration is described in detail, with analysis corrections for voltage variations to the level of a few percent. Detailed studies of the electric-field geometry, and the resulting successful development of a fiducial parameter, eliminate poorly measured events, yielding an energy resolution ranging from ∼9 eVee at 0 keV to 101 eVee at ∼10 keVee . New results are derived for astrophysical uncertainties relevant to the WIMP-search limits, specifically examining how they are affected by variations in the most probable WIMP velocity and the Galactic escape velocity. These variations become more important for WIMP masses below 10 GeV /c2 . Finally, new limits on spin-dependent low-mass WIMP-nucleon interactions are derived, with new parameter space excluded for WIMP masses ≲3 GeV /c2. Title: Performance Characterization of HT Actuator for Venus Authors: Rehnmark, F.; Bailey, J.; Cloninger, E.; Zacny, K.; Hall, J.; Sherrill, K.; Melko, J.; Kriechbaum, K.; Wilcox, B. Bibcode: 2017LPICo2061.8038R Altcode: A high temperature (HT) actuator capable of operating in the harsh environment found on the surface of Venus has been built and tested in rock drilling trials at JPL’s Venus Materials Test Facility. Title: The Venera-D Mission Concept, Report on the Activities of the Joint Science Definition Team Authors: Senske, D.; Zasova, L.; Economou, T.; Eismont, N.; Gerasimov, M.; Gorinov, D.; Hall, J.; Ignatiev, N.; Ivanov, M.; Lea Jessup, K.; Khatuntsev, I.; Korablev, O.; Kremic, T.; Limaye, S.; Lomakin, I.; Martynov, A.; Ocampo, A.; Vaisberg, O.; Burdanov, A.; Teselkin, S.; Vorontsov, V. Bibcode: 2017LPICo2061.8014S Altcode: This report will summarize the activities of the Venera-D Joint Science Definition Team. The focus will be on the mission architecture and the outcome of a Venus modeling workshop held in Moscow. Title: Evolution of Long Term Variability in Solar Analogs Authors: Egeland, Ricky; Soon, Willie; Baliunas, Sallie; Hall, Jeffrey C.; Henry, Gregory W. Bibcode: 2017IAUS..328..329E Altcode: 2017arXiv170402388E Earth is the only planet known to harbor life, therefore we may speculate on how the nature of the Sun-Earth interaction is relevant to life on Earth, and how the behavior of other stars may influence the development of life on their planetary systems. We study the long-term variability of a sample of five solar analog stars using composite chromospheric activity records up to 50 years in length and synoptic visible-band photometry about 20 years long. This sample covers a large range of stellar ages which we use to represent the evolution in activity for solar mass stars. We find that young, fast rotators have an amplitude of variability many times that of the solar cycle, while old, slow rotators have very little variability. We discuss the possible impacts of this variability on young Earth and exoplanet climates. Title: VizieR Online Data Catalog: Calibrated solar S-index time series (Egeland+, 2017) Authors: Egeland, R.; Soon, W.; Baliunas, S.; Hall, J. C.; Pevtsov, A. A.; Bertello, L. Bibcode: 2017yCat..18350025E Altcode: The Mount Wilson HK Program observed the Moon with both the HKP-1 and HKP-2 instruments. After removing 11 obvious outliers, there are 162 HKP-1 observations taken from 1966 September 2 to 1977 June 4 with the Mount Wilson 100 inch reflector, covering the maximum of cycle 20 and the cycle 20-21 minimum. As mentioned in Baliunas+ (1995ApJ...438..269B), observations of the Moon resumed in 1993 with the HKP-2 instrument. After removing 10 obvious outliers, there are 75 HKP-2 observations taken from 1994 March 27 to 2002 November 23 with the Mount Wilson 60 inch reflector, covering the end of cycle 22 and the cycle 23 minimum, extending just past the cycle 23 maximum. The end of observations coincides with the unfortunate termination of the HK Project in 2003.

We seek to extend our time series of solar variability beyond cycle 23 by establishing a proxy to the NSO Sacramento Peak (NSO/SP) observations taken from 1976 to 2016, covering cycles 21 to 24. The spectral intensity scale is set by integrating a 0.53Å band centered at 3934.869Å in the K-line wing and setting it to the fixed value of 0.162.

We extend the S-index record back to cycle 20 using the composite K time series of Bertello+ (2016SoPh..291.2967B). See section 3 for further explanations.

(1 data file). Title: Low-Mass Dark Matter Search with CDMSlite Authors: SuperCDMS Collaboration; Agnese, R.; Anderson, A. J.; Aralis, T.; Aramaki, T.; Arnquist, I. J.; Baker, W.; Balakishiyeva, D.; Barker, D.; Basu Thakur, R.; Bauer, D. A.; Binder, T.; Bowles, M. A.; Brink, P. L.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Calkins, R.; Cartaro, C.; Cerdeno, D. G.; Chang, Y.; Chagani, H.; Chen, Y.; Cooley, J.; Cornell, B.; Cushman, P.; Daal, M.; Di Stefano, P. C. F.; Doughty, T.; Esteban, L.; Fascione, E.; Figueroa-Feliciano, E.; Fritts, M.; Gerbier, G.; Ghaith, M.; Godfrey, G. L.; Golwala, S. R.; Hall, J.; Harris, H. R.; Hong, Z.; Hoppe, E. W.; Hsu, L.; Huber, M. E.; Iyer, V.; Jardin, D.; Jastram, A.; Jena, C.; Kelsey, M. H.; Kennedy, A.; Kubik, A.; Kurinsky, N. A.; Leder, A.; Loer, B.; Lopez Asamar, E.; Lukens, P.; MacDonell, D.; Mahapatra, R.; Mandic, V.; Mast, N.; Miller, E. H.; Mirabolfathi, N.; Moffatt, R. A.; Mohanty, B.; Morales Mendoza, J. D.; Nelson, J.; Orrell, J. L.; Oser, S. M.; Page, K.; Page, W. A.; Partridge, R.; Pepin, M.; Penalver Martinez, M.; Phipps, A.; Poudel, S.; Pyle, M.; Qiu, H.; Rau, W.; Redl, P.; Reisetter, A.; Reynolds, T.; Roberts, A.; Robinson, A. E.; Rogers, H. E.; Saab, T.; Sadoulet, B.; Sander, J.; Schneck, K.; Schnee, R. W.; Scorza, S.; Senapati, K.; Serfass, B.; Speller, D.; Stein, M.; Street, J.; Tanaka, H. A.; Toback, D.; Underwood, R.; Villano, A. N.; von Krosigk, B.; Welliver, B.; Wilson, J. S.; Wilson, M. J; Wright, D. H.; Yellin, S.; Yen, J. J.; Young, B. A.; Zhang, X.; Zhao, X. Bibcode: 2017arXiv170701632S Altcode: The SuperCDMS experiment is designed to directly detect weakly interacting massive particles (WIMPs) that may constitute the dark matter in our Galaxy. During its operation at the Soudan Underground Laboratory, germanium detectors were run in the CDMSlite mode to gather data sets with sensitivity specifically for WIMPs with masses ${<}$10 GeV/$c^2$. In this mode, a higher detector-bias voltage is applied to amplify the phonon signals produced by drifting charges. This paper presents studies of the experimental noise and its effect on the achievable energy threshold, which is demonstrated to be as low as 56 eV$_{\text{ee}}$ (electron equivalent energy). The detector-biasing configuration is described in detail, with analysis corrections for voltage variations to the level of a few percent. Detailed studies of the electric-field geometry, and the resulting successful development of a fiducial parameter, eliminate poorly measured events, yielding an energy resolution ranging from ${\sim}$9 eV$_{\text{ee}}$ at 0 keV to 101 eV$_{\text{ee}}$ at ${\sim}$10 eV$_{\text{ee}}$. New results are derived for astrophysical uncertainties relevant to the WIMP-search limits, specifically examining how they are affected by variations in the most probable WIMP velocity and the Galactic escape velocity. These variations become more important for WIMP masses below 10 GeV/$c^2$. Finally, new limits on spin-dependent low-mass WIMP-nucleon interactions are derived, with new parameter space excluded for WIMP masses $\lesssim$3 GeV/$c^2$ Title: Dark Matter Search Results from the PICO -60 C 3F8 Bubble Chamber Authors: Amole, C.; Ardid, M.; Arnquist, I. J.; Asner, D. M.; Baxter, D.; Behnke, E.; Bhattacharjee, P.; Borsodi, H.; Bou-Cabo, M.; Campion, P.; Cao, G.; Chen, C. J.; Chowdhury, U.; Clark, K.; Collar, J. I.; Cooper, P. S.; Crisler, M.; Crowder, G.; Dahl, C. E.; Das, M.; Fallows, S.; Farine, J.; Felis, I.; Filgas, R.; Girard, F.; Giroux, G.; Hall, J.; Harris, O.; Hoppe, E. W.; Jin, M.; Krauss, C. B.; Laurin, M.; Lawson, I.; Leblanc, A.; Levine, I.; Lippincott, W. H.; Mamedov, F.; Maurya, D.; Mitra, P.; Nania, T.; Neilson, R.; Noble, A. J.; Olson, S.; Ortega, A.; Plante, A.; Podviyanuk, R.; Priya, S.; Robinson, A. E.; Roeder, A.; Rucinski, R.; Scallon, O.; Seth, S.; Sonnenschein, A.; Starinski, N.; Štekl, I.; Tardif, F.; Vázquez-Jáuregui, E.; Wells, J.; Wichoski, U.; Yan, Y.; Zacek, V.; Zhang, J.; PICO Collaboration Bibcode: 2017PhRvL.118y1301A Altcode: 2017arXiv170207666A New results are reported from the operation of the PICO-60 dark matter detector, a bubble chamber filled with 52 kg of C3 F8 located in the SNOLAB underground laboratory. As in previous PICO bubble chambers, PICO -60 C 3F8 exhibits excellent electron recoil and alpha decay rejection, and the observed multiple-scattering neutron rate indicates a single-scatter neutron background of less than one event per month. A blind analysis of an efficiency-corrected 1167-kg day exposure at a 3.3-keV thermodynamic threshold reveals no single-scattering nuclear recoil candidates, consistent with the predicted background. These results set the most stringent direct-detection constraint to date on the weakly interacting massive particle (WIMP)-proton spin-dependent cross section at 3.4 ×10-41 cm2 for a 30 -GeV c-2 WIMP, more than 1 order of magnitude improvement from previous PICO results. Title: VISAGE Rock Sampling Drill Authors: Rehnmark, F.; Cloninger, E.; Hyman, C.; Zacny, K.; Kriechbaum, K.; Hall, J.; Melko, J.; Bailey, J.; Wilcox, B.; Sherrill, K. Bibcode: 2017LPICo2022.8038R Altcode: A rock sampling drill capable of operating in the high temperature and pressure environment found on the surface of Venus has been built and tested at JPL’s Venus Materials Test Facility (VMTF). Title: Projected sensitivity of the SuperCDMS SNOLAB experiment Authors: Agnese, R.; Anderson, A. J.; Aramaki, T.; Arnquist, I.; Baker, W.; Barker, D.; Basu Thakur, R.; Bauer, D. A.; Borgland, A.; Bowles, M. A.; Brink, P. L.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Calkins, R.; Cartaro, C.; Cerdeño, D. G.; Chagani, H.; Chen, Y.; Cooley, J.; Cornell, B.; Cushman, P.; Daal, M.; Di Stefano, P. C. F.; Doughty, T.; Esteban, L.; Fallows, S.; Figueroa-Feliciano, E.; Fritts, M.; Gerbier, G.; Ghaith, M.; Godfrey, G. L.; Golwala, S. R.; Hall, J.; Harris, H. R.; Hofer, T.; Holmgren, D.; Hong, Z.; Hoppe, E.; Hsu, L.; Huber, M. E.; Iyer, V.; Jardin, D.; Jastram, A.; Kelsey, M. H.; Kennedy, A.; Kubik, A.; Kurinsky, N. A.; Leder, A.; Loer, B.; Lopez Asamar, E.; Lukens, P.; Mahapatra, R.; Mandic, V.; Mast, N.; Mirabolfathi, N.; Moffatt, R. A.; Morales Mendoza, J. D.; Orrell, J. L.; Oser, S. M.; Page, K.; Page, W. A.; Partridge, R.; Pepin, M.; Phipps, A.; Poudel, S.; Pyle, M.; Qiu, H.; Rau, W.; Redl, P.; Reisetter, A.; Roberts, A.; Robinson, A. E.; Rogers, H. E.; Saab, T.; Sadoulet, B.; Sander, J.; Schneck, K.; Schnee, R. W.; Serfass, B.; Speller, D.; Stein, M.; Street, J.; Tanaka, H. A.; Toback, D.; Underwood, R.; Villano, A. N.; von Krosigk, B.; Welliver, B.; Wilson, J. S.; Wright, D. H.; Yellin, S.; Yen, J. J.; Young, B. A.; Zhang, X.; Zhao, X.; SuperCDMS Collaboration Bibcode: 2017PhRvD..95h2002A Altcode: 2016arXiv161000006A SuperCDMS SNOLAB will be a next-generation experiment aimed at directly detecting low-mass particles (with masses ≤10 GeV /c2 ) that may constitute dark matter by using cryogenic detectors of two types (HV and iZIP) and two target materials (germanium and silicon). The experiment is being designed with an initial sensitivity to nuclear recoil cross sections ∼1 ×10-43 cm2 for a dark matter particle mass of 1 GeV /c2 , and with capacity to continue exploration to both smaller masses and better sensitivities. The phonon sensitivity of the HV detectors will be sufficient to detect nuclear recoils from sub-GeV dark matter. A detailed calibration of the detector response to low-energy recoils will be needed to optimize running conditions of the HV detectors and to interpret their data for dark matter searches. Low-activity shielding, and the depth of SNOLAB, will reduce most backgrounds, but cosmogenically produced <mml:mmultiscripts>H 3 </mml:mmultiscripts> and naturally occurring <mml:mmultiscripts>Si 32 </mml:mmultiscripts> will be present in the detectors at some level. Even if these backgrounds are 10 times higher than expected, the science reach of the HV detectors would be over 3 orders of magnitude beyond current results for a dark matter mass of 1 GeV /c2 . The iZIP detectors are relatively insensitive to variations in detector response and backgrounds, and will provide better sensitivity for dark matter particles with masses ≳5 GeV /c2 . The mix of detector types (HV and iZIP), and targets (germanium and silicon), planned for the experiment, as well as flexibility in how the detectors are operated, will allow us to maximize the low-mass reach, and understand the backgrounds that the experiment will encounter. Upgrades to the experiment, perhaps with a variety of ultra-low-background cryogenic detectors, will extend dark matter sensitivity down to the "neutrino floor," where coherent scatters of solar neutrinos become a limiting background. Title: Sample Acquisition Drill for Venus In Situ Explorer (VISE) Authors: Rehnmark, F.; Zacny, K.; Hall, J.; Cloninger, E.; Hyman, C.; Kriechbaum, K.; Melko, J.; Rabinovitch, J.; Wilcox, B.; Lambert, J.; Traeden, N.; Bailey, J. Bibcode: 2017LPI....48.1367R Altcode: We present development and testing of Venus drill for New Frontiers Venus In Situ Explorer (VISE). Title: Lowell Observatory's Discovery Channel Telescope Authors: Hall, Jeffrey C. Bibcode: 2017AAS...22912601H Altcode: Lowell Observatory broke ground on its 4.3-meter Discovery Channel Telescope (DCT) in July 2005 and celebrated first light for the telescope in July 2012. In this overview to this special session, I will discuss the origin and development of the project, the telescope's general specifications and performance, its current operating status, and the initial instrument suite. Title: The Mount Wilson Observatory S-index of the Sun Authors: Egeland, Ricky; Soon, Willie; Baliunas, Sallie; Hall, Jeffrey C.; Pevtsov, Alexei A.; Bertello, Luca Bibcode: 2017ApJ...835...25E Altcode: 2016arXiv161104540E The most commonly used index of stellar magnetic activity is the instrumental flux scale of singly ionized calcium H & K line core emission, S, developed by the Mount Wilson Observatory (MWO) HK Project, or the derivative index {R}{HK}\prime . Accurately placing the Sun on the S scale is important for comparing solar activity to that of the Sun-like stars. We present previously unpublished measurements of the reflected sunlight from the Moon using the second-generation MWO HK photometer during solar cycle 23 and determine cycle minimum {S}23,\min =0.1634+/- 0.0008, amplitude {{Δ }}{S}23=0.0143+/- 0.0012, and mean < {S}23> =0.1701+/- 0.0005. By establishing a proxy relationship with the closely related National Solar Observatory Sacramento Peak calcium K emission index, itself well correlated with the Kodaikanal Observatory plage index, we extend the MWO S time series to cover cycles 15-24 and find on average < {S}\min > =0.1621+/- 0.0008, < {{Δ }}{S}{cyc}> =0.0145+/- 0.0012, < {S}{cyc}> =0.1694+/- 0.0005. Our measurements represent an improvement over previous estimates that relied on stellar measurements or solar proxies with non-overlapping time series. We find good agreement from these results with measurements by the Solar-Stellar Spectrograph at Lowell Observatory, an independently calibrated instrument, which gives us additional confidence that we have accurately placed the Sun on the S-index flux scale. Title: A solar-like magnetic cycle on the mature K-dwarf 61 Cygni A (HD 201091) Authors: Boro Saikia, S.; Jeffers, S. V.; Morin, J.; Petit, P.; Folsom, C. P.; Marsden, S. C.; Donati, J. -F.; Cameron, R.; Hall, J. C.; Perdelwitz, V.; Reiners, A.; Vidotto, A. A. Bibcode: 2016A&A...594A..29B Altcode: 2016arXiv160601032B Context. The long-term monitoring of magnetic cycles in cool stars is a key diagnostic in understanding how dynamo generation and amplification of magnetic fields occur in stars similar in structure to the Sun.
Aims: We investigated the temporal evolution of a possible magnetic cycle of 61 Cyg A. The magnetic cycle is determined from 61 Cyg A's large-scale field over its activity cycle using spectropolarimetric observations and compared to the solar large-scale magnetic field.
Methods: We used the tomographic technique of Zeeman Doppler imaging (ZDI) to reconstruct the large-scale magnetic geometry of 61 Cyg A over multiple observational epochs spread over a time span of nine years. We investigated the time evolution of the different components of the large-scale field and compared it with the evolution of the star's chromospheric activity by measuring the flux in three different chromospheric indicators: Ca II H&K, Hα and Ca II infrared triplet lines. We also compared our results with the star's coronal activity using XMM-Newton observations.
Results: The large-scale magnetic geometry of 61 Cyg A exhibits polarity reversals in both poloidal and toroidal field components, in phase with its chromospheric activity cycle. We also detect weak solar-like differential rotation with a shear level similar to that of the Sun. During our observational time span of nine years, 61 Cyg A exhibits solar- like variations in its large-scale field geometry as it evolves from minimum activity to maximum activity and vice versa. During its activity minimum in epoch 2007.59, ZDI reconstructs a simple dipolar geometry which becomes more complex when it approaches activity maximum in epoch 2010.55. The radial field flips polarity and reverts back to a simple geometry in epoch 2013.61. The field is strongly dipolar and the evolution of the dipole component of the field is reminiscent of solar behaviour. The polarity reversal of the large-scale field indicates a magnetic cycle that is in phase with the chromospheric and coronal cycle. Title: Dynamo Sensitivity In Solar Analogs With 50 Years Of Ca II H & K Activity Authors: Egeland, Ricky; Soon, Willie; Baliunas, Sallie; Hall, Jeffrey C.; Pevtsov, Alexei A.; Henry, Gregory W. Bibcode: 2016csss.confE...6E Altcode: 2016csss.confE..73E; 2016arXiv160904756E The Sun has a steady 11-year cycle in magnetic activity most well-known by the rising and falling in the occurrence of dark sunspots on the solar disk in visible bandpasses. The 11-year cycle is also manifest in the variations of emission in the Ca II H & K line cores, due to non-thermal (i.e. magnetic) heating in the lower chromosphere. The large variation in Ca II H & K emission allows for study of the patterns of long-term variability in other stars thanks to synoptic monitoring with the Mount Wilson Observatory HK photometers (1966-2003) and Lowell Observatory Solar-Stellar Spectrograph (1994-present). Overlapping measurements for a set of 27 nearby solar-analog (spectral types G0-G5) stars were used to calibrate the two instruments and construct time series of magnetic activity up to 50 years in length. Precise properties of fundamental importance to the dynamo are available from Hipparcos, the Geneva-Copenhagen Survey, and CHARA interferometry. Using these long time series and measurements of fundamental properties, we do a comparative study of stellar "twins" to explore the sensitivity of the stellar dynamo to small changes to structure, rotation, and composition. We also compare this sample to the Sun and find hints that the regular periodic variability of the solar cycle may be rare among its nearest neighbors in parameter space. Title: The Solar Dynamo Zoo Authors: Egeland, Ricky; Soon, Willie; Baliunas, Sallie; Hall, Jeffrey C.; Pevtsov, Alexei A.; Henry, Gregory W. Bibcode: 2016csss.confE..72E Altcode: We present composite time series of Ca II H & K line core emission indices of up to 50 years in length for a set of 27 solar-analog stars (spectral types G0-G5; within 10% of the solar mass) and the Sun. These unique data are available thanks to the long-term dedicated efforts of the Mount Wilson Observatory HK project, the Lowell Observatory Solar-Stellar Spectrograph, and the National Solar Observatory/Air Force Research Laboratory/Sacramento Peak K-line monitoring program. The Ca II H & K emission originates in the lower chromosphere and is strongly correlated with the presence of magnetic plage regions in the Sun. These synoptic observations allow us to trace the patterns long-term magnetic variability and explore dynamo behavior over a wide range of rotation regimes and stellar evolution timescales.In this poster, the Ca HK observations are expressed using the Mount Wilson S-index. Each time series is accompanied by a Lomb-Scargle periodogram, fundemental stellar parameters derived from the Geneva-Copenhagen Survey, and statistics derived from the time series including the median S-index value and seasonal and long-term amplitudes. Statistically significant periodogram peaks are ranked according to a new cycle quality metric. We find that clear, simple, Sun-like cycles are the minority in this sample. Title: Dynamo Sensitivity in Solar Analogs with 50 Years of Ca II H & K Activity Authors: Egeland, Ricky; Soon, Willie H.; Baliunas, Sallie L.; Hall, Jeffrey C.; Pevtsov, Alexei A.; Henry, Gregory W. Bibcode: 2016SPD....4720307E Altcode: The Sun has a steady 11-year cycle in magnetic activity most well-known by the rising and falling in the occurrence of dark sunspots on the solar disk in visible bandpasses. The 11-year cycle is also manifest in the variations of emission in the Ca II H & K line cores, due to non-thermal (i.e. magnetic) heating in the lower chromosphere. The large variation in Ca II H & K emission allows for study of the patterns of long-term variability in other stars thanks to synoptic monitoring with the Mount Wilson Observatory HK photometers (1966-2003) and Lowell Observatory Solar-Stellar Spectrograph (1994-present). Overlapping measurements for a set of 27 nearby solar-analog (spectral types G0-G5) stars were used to calibrate the two instruments and construct time series of magnetic activity up to 50 years in length. Precise properties of fundamental importance to the dynamo are available from Hipparcos, the Geneva-Copenhagen Survey, and CHARA interferometry. Using these long time series and measurements of fundamental properties, we do a comparative study of stellar "twins" to explore the sensitivity of the stellar dynamo to small changes to structure, rotation, and composition. We also compare this sample to the Sun and find hints that the regular periodic variability of the solar cycle may be rare among its nearest neighbors in parameter space. Title: The Solar Dynamo Zoo Authors: Egeland, Ricky; Soon, Willie H.; Baliunas, Sallie L.; Hall, Jeffrey C.; Pevtsov, Alexei A.; Henry, Gregory W. Bibcode: 2016SPD....47.1103E Altcode: We present composite time series of Ca II H & K line core emission indices of up to 50 years in length for a set of 27 solar-analog stars (spectral types G0-G5; within ~10% of the solar mass) and the Sun. These unique data are available thanks to the long-term dedicated efforts of the Mount Wilson Observatory HK project, the Lowell Observatory Solar-Stellar Spectrograph, and the National Solar Observatory/Air Force Research Laboratory/Sacremento Peak K-line monitoring program. The Ca II H & K emission originates in the lower chromosphere and is strongly correlated with the presence of magnetic plage regions in the Sun. These synoptic observations allow us to trace the patterns long-term magnetic variability and explore dynamo behavior over a wide range of rotation regimes and stellar evolution timescales. Title: Improved dark matter search results from PICO-2L Run 2 Authors: Amole, C.; Ardid, M.; Arnquist, I. J.; Asner, D. M.; Baxter, D.; Behnke, E.; Bhattacharjee, P.; Borsodi, H.; Bou-Cabo, M.; Brice, S. J.; Broemmelsiek, D.; Clark, K.; Collar, J. I.; Cooper, P. S.; Crisler, M.; Dahl, C. E.; Das, M.; Debris, F.; Fallows, S.; Farine, J.; Felis, I.; Filgas, R.; Fines-Neuschild, M.; Girard, F.; Giroux, G.; Hall, J.; Harris, O.; Hoppe, E. W.; Jackson, C. M.; Jin, M.; Krauss, C. B.; Lafrenière, M.; Laurin, M.; Lawson, I.; Leblanc, A.; Levine, I.; Lippincott, W. H.; Mann, E.; Martin, J. P.; Maurya, D.; Mitra, P.; Olson, S.; Neilson, R.; Noble, A. J.; Plante, A.; Podviianiuk, R. B.; Priya, S.; Robinson, A. E.; Ruschman, M.; Scallon, O.; Sonnenschein, A.; Starinski, N.; Štekl, I.; Vázquez-Jáuregui, E.; Wells, J.; Wichoski, U.; Zacek, V.; Zhang, J.; PICO Collaboration Bibcode: 2016PhRvD..93f1101A Altcode: 2016arXiv160103729A New data are reported from a second run of the 2-liter PICO-2L C3 F8 bubble chamber with a total exposure of 129 kg-days at a thermodynamic threshold energy of 3.3 keV. These data show that measures taken to control particulate contamination in the superheated fluid resulted in the absence of the anomalous background events observed in the first run of this bubble chamber. One single nuclear-recoil event was observed in the data, consistent both with the predicted background rate from neutrons and with the observed rate of unambiguous multiple-bubble neutron scattering events. The chamber exhibits the same excellent electron-recoil and alpha decay rejection as was previously reported. These data provide the most stringent direct detection constraints on weakly interacting massive particle (WIMP)-proton spin-dependent scattering to date for WIMP masses <50 GeV /c2 . Title: Dark matter search results from the PICO-60 CF3 I bubble chamber Authors: Amole, C.; Ardid, M.; Asner, D. M.; Baxter, D.; Behnke, E.; Bhattacharjee, P.; Borsodi, H.; Bou-Cabo, M.; Brice, S. J.; Broemmelsiek, D.; Clark, K.; Collar, J. I.; Cooper, P. S.; Crisler, M.; Dahl, C. E.; Daley, S.; Das, M.; Debris, F.; Dhungana, N.; Fallows, S.; Farine, J.; Felis, I.; Filgas, R.; Girard, F.; Giroux, G.; Grandison, A.; Hai, M.; Hall, J.; Harris, O.; Jin, M.; Krauss, C. B.; Lafrenière, M.; Laurin, M.; Lawson, I.; Levine, I.; Lippincott, W. H.; Mann, E.; Maurya, D.; Mitra, P.; Neilson, R.; Noble, A. J.; Plante, A.; Podviianiuk, R. B.; Priya, S.; Ramberg, E.; Robinson, A. E.; Rucinski, R.; Ruschman, M.; Scallon, O.; Seth, S.; Simon, P.; Sonnenschein, A.; Štekl, I.; Vázquez-Jáuregui, E.; Wells, J.; Wichoski, U.; Zacek, V.; Zhang, J.; Shkrob, I. A.; PICO Collaboration Bibcode: 2016PhRvD..93e2014A Altcode: 2015arXiv151007754A New data are reported from the operation of the PICO-60 dark matter detector, a bubble chamber filled with 36.8 kg of CF3 I and located in the SNOLAB underground laboratory. PICO-60 is the largest bubble chamber to search for dark matter to date. With an analyzed exposure of 92.8 livedays, PICO-60 exhibits the same excellent background rejection observed in smaller bubble chambers. Alpha decays in PICO-60 exhibit frequency-dependent acoustic calorimetry, similar but not identical to that reported recently in a C3 F8 bubble chamber. PICO-60 also observes a large population of unknown background events, exhibiting acoustic, spatial, and timing behaviors inconsistent with those expected from a dark matter signal. These behaviors allow for analysis cuts to remove all background events while retaining 48.2% of the exposure. Stringent limits on weakly interacting massive particles interacting via spin-dependent proton and spin-independent processes are set, and most interpretations of the DAMA/LIBRA modulation signal as dark matter interacting with iodine nuclei are ruled out. Title: VizieR Online Data Catalog: S-index and Stroemgren LC of HD30495 (Egeland+, 2015) Authors: Egeland, R.; Metcalfe, T. S.; Hall, J. C.; Henry, G. W. Bibcode: 2016yCat..18120012E Altcode: We analyze a combined 47-year time series of the Mount Wilson S-index shown in Figure 1. The combined S time series contains 1285 measurements from five different instruments. The majority of the measurements (624 measurements from 1967 to 2003) come from the original Mount Wilson survey, calibrated as described in Baliunas et al. (1995ApJ...438..269B). The next largest portion of the measurements are from the solar-stellar spectrograph (SSS) at Lowell Observatory (364 measurements from 1993 to 2014). Observations from the SMARTS Southern HK survey using the RC Spec R~2500 spectrograph at 1.5m telescope at CTIO are the third largest contribution (140 measurements from 2008 to 2013). We add 108 measurements from 2011 to 2015 derived from HARPS R~120000 spectra. Finally, we add 49 observations from 2002 to 2008 derived from R~55000 spectra of the Hamilton Spectrometer at Lick Observatory.

We also examined the 22-year time series of differential photometry acquired with the T4 0.75m APT at Fairborn Observatory, shown in Figure 1(c). These measurements, made in the Stroemgren b (467nm) and y (547nm) bands, are a difference with respect to the mean brightness of two stable comparison stars, HD 31414 and HD 30606.

(2 data files). Title: Sun-like Magnetic Cycles in the Rapidly-rotating Young Solar Analog HD 30495 Authors: Egeland, Ricky; Metcalfe, Travis S.; Hall, Jeffrey C.; Henry, Gregory W. Bibcode: 2015ApJ...812...12E Altcode: 2015arXiv150703611E A growing body of evidence suggests that multiple dynamo mechanisms can drive magnetic variability on different timescales, not only in the Sun but also in other stars. Many solar activity proxies exhibit a quasi-biennial (∼2 year) variation, which is superimposed upon the dominant 11 year cycle. A well-characterized stellar sample suggests at least two different relationships between rotation period and cycle period, with some stars exhibiting long and short cycles simultaneously. Within this sample, the solar cycle periods are typical of a more rapidly rotating star, implying that the Sun might be in a transitional state or that it has an unusual evolutionary history. In this work, we present new and archival observations of dual magnetic cycles in the young solar analog HD 30495, a ∼1 Gyr old G1.5 V star with a rotation period near 11 days. This star falls squarely on the relationships established by the broader stellar sample, with short-period variations at ∼1.7 years and a long cycle of ∼12 years. We measure three individual long-period cycles and find durations ranging from 9.6 to 15.5 years. We find the short-term variability to be intermittent, but present throughout the majority of the time series, though its occurrence and amplitude are uncorrelated with the longer cycle. These essentially solar-like variations occur in a Sun-like star with more rapid rotation, though surface differential rotation measurements leave open the possibility of a solar equivalence. Title: Improved WIMP-search reach of the CDMS II germanium data Authors: Agnese, R.; Anderson, A. J.; Asai, M.; Balakishiyeva, D.; Barker, D.; Basu Thakur, R.; Bauer, D. A.; Billard, J.; Borgland, A.; Bowles, M. A.; Brandt, D.; Brink, P. L.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Calkins, R.; Cerdeño, D. G.; Chagani, H.; Chen, Y.; Cooley, J.; Cornell, B.; Crewdson, C. H.; Cushman, P.; Daal, M.; Di Stefano, P. C. F.; Doughty, T.; Esteban, L.; Fallows, S.; Figueroa-Feliciano, E.; Godfrey, G. L.; Golwala, S. R.; Hall, J.; Harris, H. R.; Hertel, S. A.; Hofer, T.; Holmgren, D.; Hsu, L.; Huber, M. E.; Jardin, D.; Jastram, A.; Kamaev, O.; Kara, B.; Kelsey, M. H.; Kennedy, A.; Kiveni, M.; Koch, K.; Leder, A.; Loer, B.; Lopez Asamar, E.; Lukens, P.; Mahapatra, R.; Mandic, V.; McCarthy, K. A.; Mirabolfathi, N.; Moffatt, R. A.; Oser, S. M.; Page, K.; Page, W. A.; Partridge, R.; Pepin, M.; Phipps, A.; Prasad, K.; Pyle, M.; Qiu, H.; Rau, W.; Redl, P.; Reisetter, A.; Ricci, Y.; Rogers, H. E.; Saab, T.; Sadoulet, B.; Sander, J.; Schneck, K.; Schnee, R. W.; Scorza, S.; Serfass, B.; Shank, B.; Speller, D.; Toback, D.; Upadhyayula, S.; Villano, A. N.; Welliver, B.; Wilson, J. S.; Wright, D. H.; Yang, X.; Yellin, S.; Yen, J. J.; Young, B. A.; Zhang, J.; SuperCDMS Collaboration Bibcode: 2015PhRvD..92g2003A Altcode: 2015arXiv150405871A CDMS II data from the five-tower runs at the Soudan Underground Laboratory were reprocessed with an improved charge-pulse fitting algorithm. Two new analysis techniques to reject surface-event backgrounds were applied to the 612 kg days germanium-detector weakly interacting massive particle (WIMP)-search exposure. An extended analysis was also completed by decreasing the 10 keV analysis threshold to ∼5 keV , to increase sensitivity near a WIMP mass of 8 GeV /c2 . After unblinding, there were zero candidate events above a deposited energy of 10 keV and six events in the lower-threshold analysis. This yielded minimum WIMP-nucleon spin-independent scattering cross-section limits of 1.8 ×10-44 and 1.18 ×10-41 at 90% confidence for 60 and 8.6 GeV /c2 WIMPs, respectively. This improves the previous CDMS II result by a factor of 2.4 (2.7) for 60 (8.6 ) GeV /c2 WIMPs. Title: WIMP-Search Results from the Second CDMSlite Run Authors: SuperCDMS Collaboration; Agnese, R.; Anderson, A. J.; Aramaki, T.; Asai, M.; Baker, W.; Balakishiyeva, D.; Barker, D.; Basu Thakur, R.; Bauer, D. A.; Billard, J.; Borgland, A.; Bowles, M. A.; Brink, P. L.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Calkins, R.; Cerdeno, D. G.; Chagani, H.; Chen, Y.; Cooley, J.; Cornell, B.; Cushman, P.; Daal, M.; Di Stefano, P. C. F.; Doughty, T.; Esteban, L.; Fallows, S.; Figueroa-Feliciano, E.; Ghaith, M.; Godfrey, G. L.; Golwala, S. R.; Hall, J.; Harris, H. R.; Hofer, T.; Holmgren, D.; Hsu, L.; Huber, M. E.; Jardin, D.; Jastram, A.; Kamaev, O.; Kara, B.; Kelsey, M. H.; Kennedy, A.; Leder, A.; Loer, B.; Lopez Asamar, E.; Lukens, P.; Mahapatra, R.; Mandic, V.; Mast, N.; Mirabolfathi, N.; Moffatt, R. A.; Morales Mendoza, J. D.; Oser, S. M.; Page, K.; Page, W. A.; Partridge, R.; Pepin, M.; Phipps, A.; Prasad, K.; Pyle, M.; Qiu, H.; Rau, W.; Redl, P.; Reisetter, A.; Ricci, Y.; Roberts, A.; Rogers, H. E.; Saab, T.; Sadoulet, B.; Sander, J.; Schneck, K.; Schnee, R. W.; Scorza, S.; Serfass, B.; Shank, B.; Speller, D.; Toback, D.; Underwood, R.; Upadhyayula, S.; Villano, A. N.; Welliver, B.; Wilson, J. S.; Wright, D. H.; Yellin, S.; Yen, J. J.; Young, B. A.; Zhang, J. Bibcode: 2015arXiv150902448S Altcode: The CDMS low ionization threshold experiment (CDMSlite) uses cryogenic germanium detectors operated at a relatively high bias voltage to amplify the phonon signal in the search for weakly interacting massive particles (WIMPs). Results are presented from the second CDMSlite run with an exposure of 70 kg days, which reached an energy threshold for electron recoils as low as 56 eV. A fiducialization cut reduces backgrounds below those previously reported by CDMSlite. New parameter space for the WIMP-nucleon spin-independent cross section is excluded for WIMP masses between 1.6 and 5.5 GeV/$c^2$. Title: Sun-like Magnetic Cycles in the Fast-Rotating Young Solar Analog HD 30495 Authors: Egeland, Ricky; Metcalfe, Travis; Hall, Jeffrey C.; Henry, Gregory W. Bibcode: 2015IAUGA..2254437E Altcode: A growing body of evidence suggests that multiple dynamo mechanisms can drive magnetic variability on different timescales, not only in the Sun but also in other stars. Many solar activity proxies exhibit a quasi-biennial (~2 year) variation, which is superimposed upon the dominant 11 year cycle. A well-characterized stellar sample suggests at least two different relationships between rotation period and cycle period, with some stars exhibiting long and short cycles simultaneously. Within this sample, the solar cycle periods are typical of a more rapidly rotating star, implying that the Sun might be in a transitional state or that it has an unusual evolutionary history. In this work, we present new and archival observations of dual magnetic and photometric cycles in the young solar analog HD 30495, a ~500 Myr-old G1.5V star with a rotation period near 11 days. This star falls squarely on the relationships established by the broader stellar sample, with short-period variations at ~1.6 years and a long cycle of ~12 years. We measure three individual cycle episodes and find cycle durations ranging from 9.4-14.6 years. These essentially solar-like variations occur in a solar-like star with faster-than-solar rotation, though surface differential rotation measurements leave open the possibility of a solar equivalence. Title: A Tale of Two Regions: Site Protection Experience and Updated Regulations in Arizona and the Canary Islands Authors: Green, Richard F.; Diaz Castro, Javier; Allen, Lori; Alvarez del Castillo, Elizabeth; Corbally, Christopher J.; Davis, Donald; Falco, Emilio; Gabor, Paul; Hall, Jeffrey C.; Monrad, Christian Karl; Williams, G. Grant Bibcode: 2015IAUGA..2258199G Altcode: Some of the world's largest telescopes and largest concentrations of telescopes are on sites in Arizona and the Canary Islands. Active site protection efforts are underway in both regions; the common challenge is getting out ahead of the LED revolution in outdoor lighting. We review the work with local, regional, and national government bodies, with many successful updates of outdoor lighting codes. A successful statewide conference was held in Arizona to raise awareness of public officials about issues of light pollution for astronomy, safety, wildlife, and public health. We also highlight interactions with key entities near critical sites, including mines and prisons, leading to upgrades of their lighting to more astronomy-friendly form. We describe ongoing and planned sky monitoring efforts, noting their importance in quantifying the "impact on astronomy" increasingly requested by regulators. Title: Activity and Brightness Variations of Sun-Like Stars Authors: Hall, Jeffrey C. Bibcode: 2015IAUGA..2256949H Altcode: Long-term observations of variations in Sun-like stars now span a half century. The Mount Wilson Observatory (MWO) HK Project operated from 1966 to 2003, and the Lowell Observatory Solar-Stellar Spectrograph (SSS) project has operated since 1994; together these programs provide a record of chromospheric activity over multiple stellar cycles for more than 100 stars of V < ~7.5. Long-term photometric monitoring of Sun-like stars, including many of the MWO and SSS targets, began in the early 1980s and continues today at the Fairborn Observatory south of Tucson. I will review progress to date in combining and interpreting the spectrosopic and photometric data sets, including some new results from the most recent years of SSS and Fairborn data. I will also review where deficiencies remain in reconciling and combining the major data sets, and will discuss efforts presently underway to remedy this and provide a long-term record for the benefit of the community. Title: Dark Matter Search Results from the PICO-2L C3F8 Bubble Chamber Authors: Amole, C.; Ardid, M.; Asner, D. M.; Baxter, D.; Behnke, E.; Bhattacharjee, P.; Borsodi, H.; Bou-Cabo, M.; Brice, S. J.; Broemmelsiek, D.; Clark, K.; Collar, J. I.; Cooper, P. S.; Crisler, M.; Dahl, C. E.; Daley, S.; Das, M.; Debris, F.; Dhungana, N.; Farine, J.; Felis, I.; Filgas, R.; Fines-Neuschild, M.; Girard, F.; Giroux, G.; Hai, M.; Hall, J.; Harris, O.; Jackson, C. M.; Jin, M.; Krauss, C. B.; Lafrenière, M.; Laurin, M.; Lawson, I.; Levine, I.; Lippincott, W. H.; Mann, E.; Martin, J. P.; Maurya, D.; Mitra, P.; Neilson, R.; Noble, A. J.; Plante, A.; Podviianiuk, R. B.; Priya, S.; Robinson, A. E.; Ruschman, M.; Scallon, O.; Seth, S.; Sonnenschein, A.; Starinski, N.; Štekl, I.; Vázquez-Jáuregui, E.; Wells, J.; Wichoski, U.; Zacek, V.; Zhang, J.; PICO Collaboration Bibcode: 2015PhRvL.114w1302A Altcode: 2015arXiv150300008A New data are reported from the operation of a 2 liter C3F8 bubble chamber in the SNOLAB underground laboratory, with a total exposure of 211.5 kg days at four different energy thresholds below 10 keV. These data show that C3F8 provides excellent electron-recoil and alpha rejection capabilities at very low thresholds. The chamber exhibits an electron-recoil sensitivity of <3.5 ×1 0-10 and an alpha rejection factor of >98.2 %. These data also include the first observation of a dependence of acoustic signal on alpha energy. Twelve single nuclear recoil event candidates were observed during the run. The candidate events exhibit timing characteristics that are not consistent with the hypothesis of a uniform time distribution, and no evidence for a dark matter signal is claimed. These data provide the most sensitive direct detection constraints on WIMP-proton spin-dependent scattering to date, with significant sensitivity at low WIMP masses for spin-independent WIMP-nucleon scattering. Title: Dark matter effective field theory scattering in direct detection experiments Authors: Schneck, K.; Cabrera, B.; Cerdeño, D. G.; Mandic, V.; Rogers, H. E.; Agnese, R.; Anderson, A. J.; Asai, M.; Balakishiyeva, D.; Barker, D.; Basu Thakur, R.; Bauer, D. A.; Billard, J.; Borgland, A.; Brandt, D.; Brink, P. L.; Bunker, R.; Caldwell, D. O.; Calkins, R.; Chagani, H.; Chen, Y.; Cooley, J.; Cornell, B.; Crewdson, C. H.; Cushman, P.; Daal, M.; Di Stefano, P. C. F.; Doughty, T.; Esteban, L.; Fallows, S.; Figueroa-Feliciano, E.; Godfrey, G. L.; Golwala, S. R.; Hall, J.; Harris, H. R.; Hofer, T.; Holmgren, D.; Hsu, L.; Huber, M. E.; Jardin, D. M.; Jastram, A.; Kamaev, O.; Kara, B.; Kelsey, M. H.; Kennedy, A.; Leder, A.; Loer, B.; Lopez Asamar, E.; Lukens, P.; Mahapatra, R.; McCarthy, K. A.; Mirabolfathi, N.; Moffatt, R. A.; Morales Mendoza, J. D.; Oser, S. M.; Page, K.; Page, W. A.; Partridge, R.; Pepin, M.; Phipps, A.; Prasad, K.; Pyle, M.; Qiu, H.; Rau, W.; Redl, P.; Reisetter, A.; Ricci, Y.; Roberts, A.; Saab, T.; Sadoulet, B.; Sander, J.; Schnee, R. W.; Scorza, S.; Serfass, B.; Shank, B.; Speller, D.; Toback, D.; Upadhyayula, S.; Villano, A. N.; Welliver, B.; Wilson, J. S.; Wright, D. H.; Yang, X.; Yellin, S.; Yen, J. J.; Young, B. A.; Zhang, J.; SuperCDMS Collaboration Bibcode: 2015PhRvD..91i2004S Altcode: 2015arXiv150303379S We examine the consequences of the effective field theory (EFT) of dark matter-nucleon scattering for current and proposed direct detection experiments. Exclusion limits on EFT coupling constants computed using the optimum interval method are presented for SuperCDMS Soudan, CDMS II, and LUX, and the necessity of combining results from multiple experiments in order to determine dark matter parameters is discussed. We demonstrate that spectral differences between the standard dark matter model and a general EFT interaction can produce a bias when calculating exclusion limits and when developing signal models for likelihood and machine learning techniques. We also discuss the implications of the EFT for the next-generation (G2) direct detection experiments and point out regions of complementarity in the EFT parameter space. Title: Maximum likelihood analysis of low energy CDMS II germanium data Authors: Agnese, R.; Anderson, A. J.; Balakishiyeva, D.; Basu Thakur, R.; Bauer, D. A.; Billard, J.; Borgland, A.; Bowles, M. A.; Brandt, D.; Brink, P. L.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Cerdeno, D. G.; Chagani, H.; Chen, Y.; Cooley, J.; Cornell, B.; Crewdson, C. H.; Cushman, P.; Daal, M.; Di Stefano, P. C. F.; Doughty, T.; Esteban, L.; Fallows, S.; Figueroa-Feliciano, E.; Fritts, M.; Godfrey, G. L.; Golwala, S. R.; Graham, M.; Hall, J.; Harris, H. R.; Hertel, S. A.; Hofer, T.; Holmgren, D.; Hsu, L.; Huber, M. E.; Jastram, A.; Kamaev, O.; Kara, B.; Kelsey, M. H.; Kennedy, A.; Kiveni, M.; Koch, K.; Leder, A.; Loer, B.; Lopez Asamar, E.; Mahapatra, R.; Mandic, V.; Martinez, C.; McCarthy, K. A.; Mirabolfathi, N.; Moffatt, R. A.; Moore, D. C.; Nelson, R. H.; Oser, S. M.; Page, K.; Page, W. A.; Partridge, R.; Pepin, M.; Phipps, A.; Prasad, K.; Pyle, M.; Qiu, H.; Rau, W.; Redl, P.; Reisetter, A.; Ricci, Y.; Rogers, H. E.; Saab, T.; Sadoulet, B.; Sander, J.; Schneck, K.; Schnee, R. W.; Scorza, S.; Serfass, B.; Shank, B.; Speller, D.; Upadhyayula, S.; Villano, A. N.; Welliver, B.; Wright, D. H.; Yellin, S.; Yen, J. J.; Young, B. A.; Zhang, J.; SuperCDMS Collaboration Bibcode: 2015PhRvD..91e2021A Altcode: 2014arXiv1410.1003S We report on the results of a search for a Weakly Interacting Massive Particle (WIMP) signal in low-energy data of the Cryogenic Dark Matter Search experiment using a maximum likelihood analysis. A background model is constructed using geant4 to simulate the surface-event background from 210Pb decay-chain events, while using independent calibration data to model the gamma background. Fitting this background model to the data results in no statistically significant WIMP component. In addition, we perform fits using an analytic ad hoc background model proposed by Collar and Fields, who claimed to find a large excess of signal-like events in our data. We confirm the strong preference for a signal hypothesis in their analysis under these assumptions, but excesses are observed in both single- and multiple-scatter events, which implies the signal is not caused by WIMPs, but rather reflects the inadequacy of their background model. Title: Dark Sky Collaborators: Arizona (AZ) Observatories, Communities, and Businesses Authors: Del Castillo, Elizabeth Alvarez; Corbally, Christopher; Falco, Emilio E.; Green, Richard F.; Hall, Jeffrey C.; Williams, G. Grant Bibcode: 2015HiA....16..747D Altcode: With outdoor lighting ordinances in Arizona first in place around observatories in 1958 and 1972, then throughout the state since 1986, Arizonans have extensive experience working with communities and businesses to preserve our dark skies. Though communities are committed to the astronomy sector in our state, astronomers must collaborate with other stakeholders to implement solutions. Ongoing education and public outreach is necessary to enable ordinance updates as technology changes. Despite significant population increases, sky brightness measurements over the last 20 years show that ordinance updates are worth our efforts as we seek to maintain high quality skies around our observatories. Collaborations are being forged and actions taken to promote astronomy for the longer term in Arizona. Title: First Direct Limits on Lightly Ionizing Particles with Electric Charge Less than e /6 Authors: Agnese, R.; Anderson, A. J.; Balakishiyeva, D.; Basu Thakur, R.; Bauer, D. A.; Billard, J.; Borgland, A.; Bowles, M. A.; Brandt, D.; Brink, P. L.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Cerdeno, D. G.; Chagani, H.; Chen, Y.; Cooley, J.; Cornell, B.; Crewdson, C. H.; Cushman, P.; Daal, M.; Di Stefano, P. C. F.; Doughty, T.; Esteban, L.; Fallows, S.; Figueroa-Feliciano, E.; Godfrey, G. L.; Golwala, S. R.; Hall, J.; Harris, H. R.; Hertel, S. A.; Hofer, T.; Holmgren, D.; Hsu, L.; Huber, M. E.; Jastram, A.; Kamaev, O.; Kara, B.; Kelsey, M. H.; Kennedy, A.; Kiveni, M.; Koch, K.; Leder, A.; Loer, B.; Lopez Asamar, E.; Mahapatra, R.; Mandic, V.; Martinez, C.; McCarthy, K. A.; Mirabolfathi, N.; Moffatt, R. A.; Moore, D. C.; Nelson, H.; Nelson, R. H.; Ogburn, R. W.; Page, K.; Page, W. A.; Partridge, R.; Pepin, M.; Phipps, A.; Prasad, K.; Pyle, M.; Qiu, H.; Rau, W.; Redl, P.; Reisetter, A.; Ricci, Y.; Rogers, H. E.; Saab, T.; Sadoulet, B.; Sander, J.; Schneck, K.; Schnee, R. W.; Scorza, S.; Serfass, B.; Shank, B.; Speller, D.; Upadhyayula, S.; Villano, A. N.; Welliver, B.; Wright, D. H.; Yellin, S.; Yen, J. J.; Young, B. A.; Zhang, J.; CDMS Collaboration Bibcode: 2015PhRvL.114k1302A Altcode: 2014arXiv1409.3270A While the standard model of particle physics does not include free particles with fractional charge, experimental searches have not ruled out their existence. We report results from the Cryogenic Dark Matter Search (CDMS II) experiment that give the first direct-detection limits for cosmogenically produced relativistic particles with electric charge lower than e /6 . A search for tracks in the six stacked detectors of each of two of the CDMS II towers finds no candidates, thereby excluding new parameter space for particles with electric charges between e /6 and e /200 . Title: Bright Hot Jupiters: Phase Curves and Doppler Spectroscopy Authors: Crossfield, Ian; Birkby, Jayne; Brogi, Matteo; Showman, Adam; Krick, Jessica; Hansen, Brad; Hall, Jeffrey; Fortney, Jonathan; Harrington, Joe; Heng, Kevin; Lopez-Morales, Mercedes; Cubillos, Patricio; Snellen, Ignas; Cowan, Nick; Rodler, Florian; Benneke, Bjoern Bibcode: 2014sptz.prop11044C Altcode: Exoplanet phase curves provide a wealth of information about atmospheric dynamics, energetics, and chemistry. Phase curves have been observed for relatively few planets, yet the current small sample already hints at the inadequacy of current atmospheric models. Our ultimate goal of understanding the global circulation patterns and their relation to atmospheric chemistry requires a larger and more homogenous sample. Here, we propose to more than double the sample of hot Jupiters with high S/N phase observations by targeting seven bright systems. Combined with the powerful new technique of high-resolution infrared Doppler spectroscopy, our observations will enable an unprecedented comparative study to relate global circulation patterns to atmospheric chemistry, and ultimately to facilitate retrieval of global abundance and temperature maps of extrasolar planets. The planets in our sample represent the best objects to leverage both space-based phase curves and ground-based spectroscopy in a combined analysis. Spectroscopic observations break the inclination degeneracy that plagued earlier non-transiting phase variations, while phase curves provide crucial information about the planetary thermal continuum that is lost in the inherently relative spectroscopic analysis. Our program uses Spitzer's recently-validated snapshot-phase curve mode to obtain high-precision photometry on long timescales with low data volumes and high scheduling flexibility, and our new retrieval approach will become a critical capability in an era of measurements at higher S/N and spectral resolution with JWST and Extremely Large ground-based telescopes. Title: Erratum: First dark matter search results from a 4-kg CF3I bubble chamber operated in a deep underground site [Phys. Rev. D 86, 052001 (2012)] Authors: Behnke, E.; Behnke, J.; Brice, S. J.; Broemmelsiek, D.; Collar, J. I.; Conner, A.; Cooper, P. S.; Crisler, M.; Dahl, C. E.; Fustin, D.; Grace, E.; Hall, J.; Hu, M.; Levine, I.; Lippincott, W. H.; Moan, T.; Nania, T.; Ramberg, E.; Robinson, A. E.; Sonnenschein, A.; Szydagis, M.; Vázquez-Jáuregui, E.; Coupp Collaboration Bibcode: 2014PhRvD..90g9902B Altcode: No abstract at ADS Title: Flexible Cover Glass for Next Generation Solar Arrays Authors: Gray, D. A.; Hall, J.; Jones, G. M. Bibcode: 2014ESASP.719E..73G Altcode: The prospect of thin, flexible, high-efficiency solar cells has raised questions about how to integrate and protect them, especially on a flexible array substrate. Although these next-generation cells are still subject to development, it seems likely that some form of protection against radiation and atomic oxygen will be required. It is possible that chemically toughened coverglasses could fulfil this requirement; however a better understanding of glass strength and static fatigue properties is needed in order to evaluate this solution in all phases of operation. This paper aims to discuss the issues and present the results of experimental work to date. Title: Search for Low-Mass Weakly Interacting Massive Particles with SuperCDMS Authors: Agnese, R.; Anderson, A. J.; Asai, M.; Balakishiyeva, D.; Basu Thakur, R.; Bauer, D. A.; Beaty, J.; Billard, J.; Borgland, A.; Bowles, M. A.; Brandt, D.; Brink, P. L.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Cerdeno, D. G.; Chagani, H.; Chen, Y.; Cherry, M.; Cooley, J.; Cornell, B.; Crewdson, C. H.; Cushman, P.; Daal, M.; DeVaney, D.; Di Stefano, P. C. F.; Silva, E. Do Couto E.; Doughty, T.; Esteban, L.; Fallows, S.; Figueroa-Feliciano, E.; Godfrey, G. L.; Golwala, S. R.; Hall, J.; Hansen, S.; Harris, H. R.; Hertel, S. A.; Hines, B. A.; Hofer, T.; Holmgren, D.; Hsu, L.; Huber, M. E.; Jastram, A.; Kamaev, O.; Kara, B.; Kelsey, M. H.; Kenany, S.; Kennedy, A.; Kiveni, M.; Koch, K.; Leder, A.; Loer, B.; Lopez Asamar, E.; Mahapatra, R.; Mandic, V.; Martinez, C.; McCarthy, K. A.; Mirabolfathi, N.; Moffatt, R. A.; Nelson, R. H.; Novak, L.; Page, K.; Partridge, R.; Pepin, M.; Phipps, A.; Platt, M.; Prasad, K.; Pyle, M.; Qiu, H.; Rau, W.; Redl, P.; Reisetter, A.; Resch, R. W.; Ricci, Y.; Ruschman, M.; Saab, T.; Sadoulet, B.; Sander, J.; Schmitt, R. L.; Schneck, K.; Schnee, R. W.; Scorza, S.; Seitz, D. N.; Serfass, B.; Shank, B.; Speller, D.; Tomada, A.; Upadhyayula, S.; Villano, A. N.; Welliver, B.; Wright, D. H.; Yellin, S.; Yen, J. J.; Young, B. A.; Zhang, J.; SuperCDMS Collaboration Bibcode: 2014PhRvL.112x1302A Altcode: 2014arXiv1402.7137A We report a first search for weakly interacting massive particles (WIMPs) using the background rejection capabilities of SuperCDMS. An exposure of 577 kg days was analyzed for WIMPs with mass <30 GeV/c2, with the signal region blinded. Eleven events were observed after unblinding. We set an upper limit on the spin-independent WIMP-nucleon cross section of 1.2×10-42 cm2 at 8 GeV /c2. This result is in tension with WIMP interpretations of recent experiments and probes new parameter space for WIMP-nucleon scattering for WIMP masses <6 GeV /c2. Title: Recent Local and State Action in Arizona to Maintain Sky Quality Authors: Hall, Jeffrey C.; Shankland, P. D.; Green, R. F.; Jannuzi, B. Bibcode: 2014AAS...22341306H Altcode: The large number of observatories in Arizona has led to the development of a number of lighting control ordinances around the state, some quite strict. Several factors are now contributing to an increased need for active effort at the local, County, and State levels in maintaining the quality of these codes; these factors include an expansion of competing interests in the state, the increasing use of LED lighting, and the potential for major new investments through projects such as the Cherenkov Telescope Array (CTA) and enhancements to the Navy Precision Optical Interferometer. I will review recent strategies Arizona's observatories have used to effect maintenance of ordinances and preserve sky quality; cases include (1) a statewide effort in 2012 to curb a proliferation of electronic billboards and (2) engagement of a broad group of local, County, and State officials, as well as individuals from the private sector, in support of projects like CTA, including awareness of and support for dark-sky preservation. Title: Progress in Dark Sky Protection in Southern Arizona Authors: Green, Richard F.; Allen, L.; Alvarez Del Castillo, E. M.; Brocious, D. K.; Corbally, C. J.; Davis, D. R.; Falco, E. E.; Gabor, P.; Hall, J. C.; Jannuzi, B.; Larson, S. M.; Mighell, K. J.; Nance, C.; Shankland, P. D.; Walker, C. E.; Williams, G.; Zaritsky, D. F. Bibcode: 2014AAS...22341305G Altcode: Arizona has many observatories dedicated to scientific research and a rapidly growing population. Continuous interaction with governmental entities and education of the public are required to take advantage of the good intentions of lighting control ordinances in place around the state. We give several recent examples of active engagement of observatories: * Interaction of Mt. Graham International Observatory with the State prison and major copper mine. * Interaction of Smithsonian Astrophysical Observatory, acting on behalf of MMT Observatory and Steward Observatory, with the US Forest Service on the prospects of developing the Rosemont Copper Mine * Defense of the Outdoor Lighting and Sign Codes in Pima County and the City of Tucson * Coordinated observatory approach to statewide issues, including the establishment of radial zones of protection from LED billboards around observatory sites. Title: Search for Low-Mass Weakly Interacting Massive Particles Using Voltage-Assisted Calorimetric Ionization Detection in the SuperCDMS Experiment Authors: Agnese, R.; Anderson, A. J.; Asai, M.; Balakishiyeva, D.; Basu Thakur, R.; Bauer, D. A.; Billard, J.; Borgland, A.; Bowles, M. A.; Brandt, D.; Brink, P. L.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Cerdeno, D. G.; Chagani, H.; Cooley, J.; Cornell, B.; Crewdson, C. H.; Cushman, P.; Daal, M.; Di Stefano, P. C. F.; Doughty, T.; Esteban, L.; Fallows, S.; Figueroa-Feliciano, E.; Godfrey, G. L.; Golwala, S. R.; Hall, J.; Harris, H. R.; Hertel, S. A.; Hofer, T.; Holmgren, D.; Hsu, L.; Huber, M. E.; Jastram, A.; Kamaev, O.; Kara, B.; Kelsey, M. H.; Kennedy, A.; Kiveni, M.; Koch, K.; Loer, B.; Lopez Asamar, E.; Mahapatra, R.; Mandic, V.; Martinez, C.; McCarthy, K. A.; Mirabolfathi, N.; Moffatt, R. A.; Moore, D. C.; Nadeau, P.; Nelson, R. H.; Page, K.; Partridge, R.; Pepin, M.; Phipps, A.; Prasad, K.; Pyle, M.; Qiu, H.; Rau, W.; Redl, P.; Reisetter, A.; Ricci, Y.; Saab, T.; Sadoulet, B.; Sander, J.; Schneck, K.; Schnee, R. W.; Scorza, S.; Serfass, B.; Shank, B.; Speller, D.; Villano, A. N.; Welliver, B.; Wright, D. H.; Yellin, S.; Yen, J. J.; Young, B. A.; Zhang, J.; SuperCDMS Collaboration Bibcode: 2014PhRvL.112d1302A Altcode: 2013arXiv1309.3259A SuperCDMS is an experiment designed to directly detect weakly interacting massive particles (WIMPs), a favored candidate for dark matter ubiquitous in the Universe. In this Letter, we present WIMP-search results using a calorimetric technique we call CDMSlite, which relies on voltage-assisted Luke-Neganov amplification of the ionization energy deposited by particle interactions. The data were collected with a single 0.6 kg germanium detector running for ten live days at the Soudan Underground Laboratory. A low energy threshold of 170 eVee (electron equivalent) was obtained, which allows us to constrain new WIMP-nucleon spin-independent parameter space for WIMP masses below 6 GeV /c2. Title: The Navy Precision Optical Interferometer (npoi): AN Update Authors: Armstrong, J. T.; Hutter, D. J.; Baines, E. K.; Benson, J. A.; Bevilacqua, R. M.; Buschmann, T.; Clark, J. H.; Ghasempour, A.; Hall, J. C.; Hindsley, R. B.; Johnston, K. J.; Jorgensen, A. M.; Mozurkewich, D.; Muterspaugh, M. W.; Restaino, S. R.; Shankland, P. D.; Schmitt, H. R.; Tycner, C.; van Belle, G. T.; Zavala, R. T. Bibcode: 2013JAI.....240002A Altcode: The Navy Precision Optical Interferometer (NPOI) has two purposes: wide angle precise astrometry and high-resolution imaging, both at visible wavelengths. It operates with up to six 12-cm diameter apertures simultaneously, with baseline lengths (distances between array elements) from 16 m to 79 m, and disperses the combined light into 16 spectral channels. It has been operational since first fringes were found in 1994; six-beam operations began in 2001. The NPOI is undergoing upgrades in numerous areas: control system and data acquisition improvements, a second beam combiner, additional array stations for both longer and shorter baselines, and supplemental delay lines to improve sky coverage for the longer baselines. Future possibilities include the installation of four fixed 1.8 m telescopes as well as up to six moveable lightweight 1.4 m telescopes. Observing programs, including programs led by outside investigators, cover a broad range of stellar astrophysics as well as observations of geostationary satellites. Title: Silicon Detector Dark Matter Results from the Final Exposure of CDMS II Authors: Agnese, R.; Ahmed, Z.; Anderson, A. J.; Arrenberg, S.; Balakishiyeva, D.; Basu Thakur, R.; Bauer, D. A.; Billard, J.; Borgland, A.; Brandt, D.; Brink, P. L.; Bruch, T.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Cerdeno, D. G.; Chagani, H.; Cooley, J.; Cornell, B.; Crewdson, C. H.; Cushman, P.; Daal, M.; Dejongh, F.; do Couto e Silva, E.; Doughty, T.; Esteban, L.; Fallows, S.; Figueroa-Feliciano, E.; Filippini, J.; Fox, J.; Fritts, M.; Godfrey, G. L.; Golwala, S. R.; Hall, J.; Harris, R. H.; Hertel, S. A.; Hofer, T.; Holmgren, D.; Hsu, L.; Huber, M. E.; Jastram, A.; Kamaev, O.; Kara, B.; Kelsey, M. H.; Kennedy, A.; Kim, P.; Kiveni, M.; Koch, K.; Kos, M.; Leman, S. W.; Loer, B.; Lopez Asamar, E.; Mahapatra, R.; Mandic, V.; Martinez, C.; McCarthy, K. A.; Mirabolfathi, N.; Moffatt, R. A.; Moore, D. C.; Nadeau, P.; Nelson, R. H.; Page, K.; Partridge, R.; Pepin, M.; Phipps, A.; Prasad, K.; Pyle, M.; Qiu, H.; Rau, W.; Redl, P.; Reisetter, A.; Ricci, Y.; Saab, T.; Sadoulet, B.; Sander, J.; Schneck, K.; Schnee, R. W.; Scorza, S.; Serfass, B.; Shank, B.; Speller, D.; Sundqvist, K. M.; Villano, A. N.; Welliver, B.; Wright, D. H.; Yellin, S.; Yen, J. J.; Yoo, J.; Young, B. A.; Zhang, J. Bibcode: 2013PhRvL.111y1301A Altcode: We report results of a search for weakly interacting massive particles (WIMPS) with the silicon detectors of the CDMS II experiment. This blind analysis of 140.2 kg day of data taken between July 2007 and September 2008 revealed three WIMP-candidate events with a surface-event background estimate of 0.41-0.08+0.20(stat)-0.24+0.28(syst). Other known backgrounds from neutrons and Pb206 are limited to <0.13 and <0.08 events at the 90% confidence level, respectively. The exposure of this analysis is equivalent to 23.4 kg day for a recoil energy range of 7-100 keV for a WIMP of mass 10GeV/c2. The probability that the known backgrounds would produce three or more events in the signal region is 5.4%. A profile likelihood ratio test of the three events that includes the measured recoil energies gives a 0.19% probability for the known-background-only hypothesis when tested against the alternative WIMP+background hypothesis. The highest likelihood occurs for a WIMP mass of 8.6GeV/c2 and WIMP-nucleon cross section of 1.9×10-41cm2. Title: A Homogeneous Phase Curve Sample for Global Atmospheric Retrieval Authors: Crossfield, Ian; Cowan, Nicolas; Snellen, Ignas; Showman, Adam; Brogi, Matteo; Birkby, Jayne; Heng, Kevin; Harrington, Joseph; Fortney, Jonathan; Rodler, Florian; Hansen, Brad; Hall, Jeffrey; Lopez-Morales, Mercedes; Cubillos, Patricio; Benneke, Bjoern Bibcode: 2013sptz.prop10078C Altcode: Exoplanet phase curves provide a wealth of information about atmospheric dynamics, energetics, and chemistry. Phase curves have been observed for relatively few planets, yet the current small sample already hints at the inadequacy of current atmospheric models. Our ultimate goal of understanding the global circulation patterns and their relation to atmospheric chemistry requires a larger and more homogenous sample. Here, we propose to more than double the sample of hot Jupiters with high S/N phase observations by targeting five bright non-transiting systems. Combined with the powerful new technique of high-resolution infrared Doppler spectroscopy, our observations will enable an unprecedented comparative study to relate global circulation patterns and atmospheric chemistry, and ultimately facilitate retrieval of the first global abundance and temperature maps of extrasolar planets. The planets in our sample represent the best objects to leverage both space-based phase curves and ground-based spectroscopy in a combined analysis. Spectroscopic observations break the inclination degeneracy that plagued earlier non-transiting phase variations, while phase curves provide crucial information about the planetary thermal continuum that is lost in the inherently relative spectroscopic analysis. Our program uses Spitzer's recently-validated observing mode to obtain high-precision photometry on long timescales with low data volumes and high scheduling flexibility, and our new retrieval approach will become a critical capability in an era of measurements at higher S/N and spectral resolution with JWST and Extremely Large ground-based telescopes. Title: Snowmass CF1 Summary: WIMP Dark Matter Direct Detection Authors: Cushman, P.; Galbiati, C.; McKinsey, D. N.; Robertson, H.; Tait, T. M. P.; Bauer, D.; Borgland, A.; Cabrera, B.; Calaprice, F.; Cooley, J.; Empl, T.; Essig, R.; Figueroa-Feliciano, E.; Gaitskell, R.; Golwala, S.; Hall, J.; Hill, R.; Hime, A.; Hoppe, E.; Hsu, L.; Hungerford, E.; Jacobsen, R.; Kelsey, M.; Lang, R. F.; Lippincott, W. H.; Loer, B.; Luitz, S.; Mandic, V.; Mardon, J.; Maricic, J.; Maruyama, R.; Mahapatra, R.; Nelson, H.; Orrell, J.; Palladino, K.; Pantic, E.; Partridge, R.; Ryd, A.; Saab, T.; Sadoulet, B.; Schnee, R.; Shepherd, W.; Sonnenschein, A.; Sorensen, P.; Szydagis, M.; Volansky, T.; Witherell, M.; Wright, D.; Zurek, K. Bibcode: 2013arXiv1310.8327C Altcode: As part of the Snowmass process, the Cosmic Frontier WIMP Direct Detection subgroup (CF1) has drawn on input from the Cosmic Frontier and the broader Particle Physics community to produce this document. The charge to CF1 was (a) to summarize the current status and projected sensitivity of WIMP direct detection experiments worldwide, (b) motivate WIMP dark matter searches over a broad parameter space by examining a spectrum of WIMP models, (c) establish a community consensus on the type of experimental program required to explore that parameter space, and (d) identify the common infrastructure required to practically meet those goals. Title: Computational Challenges in Processing the Q1-Q16 Kepler Data Set Authors: Klaus, Todd C.; Henze, C.; Twicken, J. D.; Hall, J.; McCauliff, S. D.; Girouard, F.; Cote, M.; Morris, R. L.; Clarke, B.; Jenkins, J. M.; Caldwell, D.; Kepler Science Operations Center Bibcode: 2013DPS....4520907K Altcode: Since launch on March 6th, 2009, NASA’s Kepler Space Telescope has collected 48 months of data on over 195,000 targets. The raw data are rife with instrumental and astrophysical noise that must be removed in order to detect and model the transit-like signals present in the data. Calibrating the raw pixels, generating and correcting the flux light curves, and detecting and characterizing the signals require significant computational power. In addition, the algorithms that make up the Kepler Science Pipeline and their parameters are still undergoing changes (most of which increase the computational cost), creating the need to reprocess the entire data set on a regular basis. We discuss how we have ported all of the core elements of the pipeline to the Pleiades cluster at the NASA Advanced Supercomputing (NAS) Division, the needs driving the port, and the technical challenges we faced. In 2011 we ported the Transiting Planet Search (TPS) and Data Validation (DV) modules to Pleiades. These pipeline modules operate on the full data set and the computational complexity increases roughly by the square of the number of data points. At the time of the port it had become infeasible to run these modules on our local hardware, necessitating the move to Pleiades. In 2012 and 2013 we turned our attention to the front end of the pipeline; Pixel-level Calibration (CAL), Photometric Analysis (PA), and Pre-Search Data Conditioning (PDC). Porting these modules to Pleiades will allow us to reprocess the complete data set on a more frequent basis. The last time we reprocessed all data for the front end we only had 24 months of data. We estimate that the full 48-month data set would take over 200 days to complete on local hardware. When the port is complete we expect to reprocess this data set on Pleiades in about a month. The NASA Science Mission Directorate provided funding for the Kepler Mission. Title: Publisher's Note: Silicon detector results from the first five-tower run of CDMS II [Phys. Rev. D 88, 031104(R) (2013)] Authors: Agnese, R.; Ahmed, Z.; Anderson, A. J.; Arrenberg, S.; Balakishiyeva, D.; Basu Thakur, R.; Bauer, D. A.; Borgland, A.; Brandt, D.; Brink, P. L.; Bruch, T.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Cerdeno, D. G.; Chagani, H.; Cooley, J.; Cornell, B.; Crewdson, C. H.; Cushman, P.; Daal, M.; Dejongh, F.; Di Stefano, P. C. F.; do Couto e Silva, E.; Doughty, T.; Esteban, L.; Fallows, S.; Figueroa-Feliciano, E.; Filippini, J.; Fox, J.; Fritts, M.; Godfrey, G. L.; Golwala, S. R.; Hall, J.; Harris, R. H.; Hertel, S. A.; Hofer, T.; Holmgren, D.; Hsu, L.; Huber, M. E.; Jastram, A.; Kamaev, O.; Kara, B.; Kelsey, M. H.; Kennedy, A.; Kim, P.; Kiveni, M.; Koch, K.; Kos, M.; Leman, S. W.; Lopez-Asamar, E.; Mahapatra, R.; Mandic, V.; Martinez, C.; McCarthy, K. A.; Mirabolfathi, N.; Moffatt, R. A.; Moore, D. C.; Nadeau, P.; Nelson, R. H.; Page, K.; Partridge, R.; Pepin, M.; Phipps, A.; Prasad, K.; Pyle, M.; Qiu, H.; Rau, W.; Redl, P.; Reisetter, A.; Ricci, Y.; Saab, T.; Sadoulet, B.; Sander, J.; Schneck, K.; Schnee, R. W.; Scorza, S.; Serfass, B.; Shank, B.; Speller, D.; Sundqvist, K. M.; Villano, A. N.; Welliver, B.; Wright, D. H.; Yellin, S.; Yen, J. J.; Yoo, J.; Young, B. A.; Zhang, J. Bibcode: 2013PhRvD..88e9901A Altcode: No abstract at ADS Title: Silicon detector results from the first five-tower run of CDMS II Authors: Agnese, R.; Ahmed, Z.; Anderson, A. J.; Arrenberg, S.; Balakishiyeva, D.; Basu Thakur, R.; Bauer, D. A.; Borgland, A.; Brandt, D.; Brink, P. L.; Bruch, T.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Cerdeno, D. G.; Chagani, H.; Cooley, J.; Cornell, B.; Crewdson, C. H.; Cushman, P.; Daal, M.; Dejongh, F.; Di tefano, P. C. F.; do Couto e Silva, E.; Doughty, T.; Esteban, L.; Fallows, S.; Figueroa-Feliciano, E.; Filippini, J.; Fox, J.; Fritts, M.; Godfrey, G. L.; Golwala, S. R.; Hall, J.; Harris, R. H.; Hertel, S. A.; Hofer, T.; Holmgren, D.; Hsu, L.; Huber, M. E.; Jastram, A.; Kamaev, O.; Kara, B.; Kelsey, M. H.; Kennedy, A.; Kim, P.; Kiveni, M.; Koch, K.; Kos, M.; Leman, S. W.; Lopez-Asamar, E.; Mahapatra, R.; Mandic, V.; Martinez, C.; McCarthy, K. A.; Mirabolfathi, N.; Moffatt, R. A.; Moore, D. C.; Nadeau, P.; Nelson, R. H.; Page, K.; Partridge, R.; Pepin, M.; Phipps, A.; Prasad, K.; Pyle, M.; Qiu, H.; Rau, W.; Redl, P.; Reisetter, A.; Ricci, Y.; Saab, T.; Sadoulet, B.; Sander, J.; Schneck, K.; Schnee, R. W.; Scorza, S.; Serfass, B.; Shank, B.; Speller, D.; Sundqvist, K. M.; Villano, A. N.; Welliver, B.; Wright, D. H.; Yellin, S.; Yen, J. J.; Yoo, J.; Young, B. A.; Zhang, J. Bibcode: 2013PhRvD..88c1104A Altcode: 2013arXiv1304.3706C We report results of a search for weakly interacting massive particles (WIMPs) with the Si detectors of the CDMS II experiment. This report describes a blind analysis of the first data taken with CDMS II’s full complement of detectors in 2006-2007; results from this exposure using the Ge detectors have already been presented. We observed no candidate WIMP-scattering events in an exposure of 55.9 kg-days before analysis cuts, with an expected background of ∼1.1 events. The exposure of this analysis is equivalent to 10.3 kg-days over a recoil energy range of 7-100 keV for an ideal Si detector and a WIMP mass of 10GeV/c2. These data set an upper limit of 1.7×10-41cm2 on the WIMP-nucleon spin-independent cross section of a 10GeV/c2 WIMP. These data exclude parameter space for spin-independent WIMP-nucleon elastic scattering that is relevant to recent searches for low-mass WIMPs. Title: Direct measurement of the bubble-nucleation energy threshold in a CF3I bubble chamber Authors: Behnke, E.; Benjamin, T.; Brice, S. J.; Broemmelsiek, D.; Collar, J. I.; Cooper, P. S.; Crisler, M.; Dahl, C. E.; Fustin, D.; Hall, J.; Harnish, C.; Levine, I.; Lippincott, W. H.; Moan, T.; Nania, T.; Neilson, R.; Ramberg, E.; Robinson, A. E.; Ruschman, M.; Sonnenschein, A.; Vázquez-Jáuregui, E.; Rivera, R. A.; Uplegger, L. Bibcode: 2013PhRvD..88b1101B Altcode: 2013arXiv1304.6001C We have directly measured the energy threshold and efficiency for bubble nucleation from iodine recoils in a CF3I bubble chamber in the energy range of interest for a dark matter search. These interactions cannot be probed by standard neutron calibration methods, so we develop a new technique by observing the elastic scattering of 12GeV/c negative pions. The pions are tracked with a silicon pixel telescope and the reconstructed scattering angle provides a measure of the nuclear recoil kinetic energy. The bubble chamber was operated with a nominal threshold of (13.6±0.6)keV. Interpretation of the results depends on the response to fluorine and carbon recoils, but in general we find agreement with the predictions of the classical bubble-nucleation theory. This measurement confirms the applicability of CF3I as a target for spin-independent dark matter interactions and represents a novel technique for calibration of superheated fluid detectors. Title: 2013 KN6 Authors: Scotti, J. V.; Stevens, B. L.; Boattini, A.; Christensen, E. J.; Gibbs, A. R.; Grauer, A. D.; Hill, R. E.; Johnson, J. A.; Kowalski, R. A.; Larson, S. M.; McNaught, R. H.; Shelly, F. C.; Wiggins, P.; McGaha, J. E.; Diaz, N. D.; Aymami, J. M.; Camarasa, J.; Bosch, J. M.; Aixela, G.; Bosque, R.; Rodriguez, D.; Diepvens, A.; Jahn, J.; Zolnowski, M.; Kusiak, M.; Kurtze, L.; Hidas, A.; Pritchett, N. E.; Mills, M.; Urbanik, M.; Guido, E.; Howes, N.; Hall, J.; Holmes, R.; Foglia, S.; Buzzi, L.; Devore, H.; Kostin, A.; Linder, T.; Lister, T.; Vorobjov, T.; Chapman, A.; Jacques, C.; Pimentel, E.; Losse, F.; Carreno, A.; Piqueras, J.; Briggs, D.; Viano, E.; Sato, H.; Shaheen, W.; Viscome, G.; Colazo, C.; Melia, R.; Aznar, A. Bibcode: 2013MPEC....L...09S Altcode: No abstract at ADS Title: SuperCDMS status from Soudan and plans for SNOLab Authors: Sander, J.; Ahmed, Z.; Anderson, A. J.; Arrenberg, S.; Balakishiyeva, D.; Thakur, R. B.; Bauer, D. A.; Brandt, D.; Brink, P. L.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Cerdeno, D. G.; Chagani, H.; Cooley, J.; Cornell, B.; Crewdson, C. H.; Cushman, P.; Daal, M.; Di Stefano, P. C. F.; Silva, E. Do Couto E.; Doughty, T.; Esteban, L.; Fallows, S.; Figueroa-Feliciano, E.; Fox, J.; Fritts, M.; Godfrey, G. L.; Golwala, S. R.; Hall, J.; Hasi, J.; Hertel, S. A.; Hofer, T.; Holmgren, D.; Hsu, L.; Huber, M. E.; Jastram, A.; Kamaev, O.; Kara, B.; Kelsey, M. H.; Kim, P.; Kiveni, M.; Koch, K.; Kos, M.; Leman, S. W.; Liu, S.; Loer, B.; Mahapatra, R.; Mandic, V.; Martinez, C.; Mccarthy, K. A.; Mirabolfathi, N.; Moffat, R.; Moore, D. C.; Nadeau, P.; Nelson, R.; Page, K.; Partridge, R.; Pepin, M.; Phipps, A.; Prasad, K.; Pyle, M.; Qiu, H.; Qiu, X.; Radpour, R.; Rau, W.; Reisetter, A.; Resch, R. W.; Ricci, Y.; Saab, T.; Sadoulet, B.; Schnee, R. W.; Scorza, S.; Serfass, B.; Shank, B.; Shneck, K.; Speller, D.; Sundqvist, K. M.; Villano, A. N.; Welliver, B.; Yellin, S.; Yen, J.; Yoo, J.; Young, B. A.; Zhang, J. Bibcode: 2013AIPC.1534..129S Altcode: Matter, as we know it, makes up less than 5% of the Universe. Various astrophysical observations have confirmed that one quarter of the Universe and most of the matter content in the Universe is made up of Dark Matter. The nature of Dark Matter is yet to be discovered and is one of the biggest questions in Physics. Particle Physics combined with astrophysical measurements of the abundance gives rise to a Dark Matter candidate called Weakly Interacting Massive Particle (WIMP). The low density of WIMPs in the galaxies and the extremely weak nature of the interaction with ordinary matter make detection of the WIMP an extraordinarily challenging task, with abundant fakes from various radioactive and cosmogenic backgrounds with much stronger electromagnetic interaction. The extremely weak nature of the WIMP interaction dictates detectors that have extremely low naturally occurring radioactive background, a large active volume (mass) of sensitive detector material to maximize statistics, a highly efficient detector based rejection mechanism for the dominant electromagnetic background and sophisticated analysis techniques to reject any residual background. This paper describes the status of the SuperCDMS experiment. Title: The Pulsar Search Collaboratory: Discovery and Timing of Five New Pulsars Authors: Rosen, R.; Swiggum, J.; McLaughlin, M. A.; Lorimer, D. R.; Yun, M.; Heatherly, S. A.; Boyles, J.; Lynch, R.; Kondratiev, V. I.; Scoles, S.; Ransom, S. M.; Moniot, M. L.; Cottrill, A.; Weaver, M.; Snider, A.; Thompson, C.; Raycraft, M.; Dudenhoefer, J.; Allphin, L.; Thorley, J.; Meadows, B.; Marchiny, G.; Liska, A.; O'Dwyer, A. M.; Butler, B.; Bloxton, S.; Mabry, H.; Abate, H.; Boothe, J.; Pritt, S.; Alberth, J.; Green, A.; Crowley, R. J.; Agee, A.; Nagley, S.; Sargent, N.; Hinson, E.; Smith, K.; McNeely, R.; Quigley, H.; Pennington, A.; Chen, S.; Maynard, T.; Loope, L.; Bielski, N.; McGough, J. R.; Gural, J. C.; Colvin, S.; Tso, S.; Ewen, Z.; Zhang, M.; Ciccarella, N.; Bukowski, B.; Novotny, C. B.; Gore, J.; Sarver, K.; Johnson, S.; Cunningham, H.; Collins, D.; Gardner, D.; Monteleone, A.; Hall, J.; Schweinhagen, R.; Ayers, J.; Jay, S.; Uosseph, B.; Dunkum, D.; Pal, J.; Dydiw, S.; Sterling, M.; Phan, E. Bibcode: 2013ApJ...768...85R Altcode: 2012arXiv1209.4108R We present the discovery and timing solutions of five new pulsars by students involved in the Pulsar Search Collaboratory, a NSF-funded joint program between the National Radio Astronomy Observatory and West Virginia University designed to excite and engage high-school students in Science, Technology, Engineering, and Mathematics (STEM) and related fields. We encourage students to pursue STEM fields by apprenticing them within a professional scientific community doing cutting edge research, specifically by teaching them to search for pulsars. The students are analyzing 300 hr of drift-scan survey data taken with the Green Bank Telescope at 350 MHz. These data cover 2876 deg2 of the sky. Over the course of five years, more than 700 students have inspected diagnostic plots through a web-based graphical interface designed for this project. The five pulsars discovered in the data have spin periods ranging from 3.1 ms to 4.8 s. Among the new discoveries are PSR J1926-1314, a long period, nulling pulsar; PSR J1821+0155, an isolated, partially recycled 33 ms pulsar; and PSR J1400-1438, a millisecond pulsar in a 9.5 day orbit whose companion is likely a white dwarf star. Title: Silicon Detector Dark Matter Results from the Final Exposure of CDMS II Authors: CDMS Collaboration; Agnese, R.; Ahmed, Z.; Anderson, A. J.; Arrenberg, S.; Balakishiyeva, D.; Basu Thakur, R.; Bauer, D. A.; Billard, J.; Borgland, A.; Brandt, D.; Brink, P. L.; Bruch, T.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Cerdeno, D. G.; Chagani, H.; Cooley, J.; Cornell, B.; Crewdson, C. H.; Cushman, P.; Daal, M.; Dejongh, F.; Silva, E. Do Couto E; Doughty, T.; Esteban, L.; Fallows, S.; Figueroa-Feliciano, E.; Filippini, J.; Fox, J.; Fritts, M.; Godfrey, G. L.; Golwala, S. R.; Hall, J.; Harris, R. H.; Hertel, S. A.; Hofer, T.; Holmgren, D.; Hsu, L.; Huber, M. E.; Jastram, A.; Kamaev, O.; Kara, B.; Kelsey, M. H.; Kennedy, A.; Kim, P.; Kiveni, M.; Koch, K.; Kos, M.; Leman, S. W.; Loer, B.; Lopez Asamar, E.; Mahapatra, R.; Mandic, V.; Martinez, C.; McCarthy, K. A.; Mirabolfathi, N.; Moffatt, R. A.; Moore, D. C.; Nadeau, P.; Nelson, R. H.; Page, K.; Partridge, R.; Pepin, M.; Phipps, A.; Prasad, K.; Pyle, M.; Qiu, H.; Rau, W.; Redl, P.; Reisetter, A.; Ricci, Y.; Saab, T.; Sadoulet, B.; Sander, J.; Schneck, K.; Schnee, R. W.; Scorza, S.; Serfass, B.; Shank, B.; Speller, D.; Sundqvist, K. M.; Villano, A. N.; Welliver, B.; Wright, D. H.; Yellin, S.; Yen, J. J.; Yoo, J.; Young, B. A.; Zhang, J. Bibcode: 2013arXiv1304.4279C Altcode: We report results of a search for Weakly Interacting Massive Particles (WIMPS) with the silicon detectors of the CDMS II experiment. This blind analysis of 140.2 kg-days of data taken between July 2007 and September 2008 revealed three WIMP-candidate events with a surface-event background estimate of 0.41^{+0.20}_{-0.08}(stat.)^{+0.28}_{-0.24}(syst.). Other known backgrounds from neutrons and 206Pb are limited to < 0.13 and <0.08 events at the 90% confidence level, respectively. The exposure of this analysis is equivalent to 23.4 kg-days for a recoil energy range of 7-100 keV for a WIMP of mass 10 GeV/c2. The probability that the known backgrounds would produce three or more events in the signal region is 5.4%. A profile likelihood ratio test of the three events that includes the measured recoil energies gives a 0.19% probability for the known-background-only hypothesis when tested against the alternative WIMP+background hypothesis. The highest likelihood occurs for a WIMP mass of 8.6 GeV/c2 and WIMP-nucleon cross section of 1.9e-41 cm2. Title: Decadal Variations of Sun-Like Stars Authors: Lockwood, G. W.; Henry, G. W.; Hall, J. C.; Radick, R. R. Bibcode: 2013ASPC..472..203L Altcode: Observations of more than 300 Sun-like field stars carried out at Fairborn Observatory since 1993 now include 168 observed for 10 years or longer. This project, a successor to previous work at Lowell Observatory and Cloudcroft Observatory, beginning in 1955 and continuing for nearly half a century, demonstrates finally that variability at the Sun's low level of total irradiance variation can be detected in stars. By also including Ca II H&K observations from the Mount Wilson and Lowell observatories, we have discovered how the patterns of photometric variability are related to chromospheric activity. We discuss the limitations of detectability imposed by comparison star variability and as an example of a star close to the detection limit we show the evidence for cyclic variability in the solar twin 18 Sco. Title: Magnetic Activity Cycles in the Exoplanet Host Star epsilon Eridani Authors: Metcalfe, T. S.; Buccino, A. P.; Brown, B. P.; Mathur, S.; Soderblom, D. R.; Henry, T. J.; Mauas, P. J. D.; Petrucci, R.; Hall, J. C.; Basu, S. Bibcode: 2013ApJ...763L..26M Altcode: 2012arXiv1212.4425M The active K2 dwarf epsilon Eri has been extensively characterized both as a young solar analog and more recently as an exoplanet host star. As one of the nearest and brightest stars in the sky, it provides an unparalleled opportunity to constrain stellar dynamo theory beyond the Sun. We confirm and document the 3-year magnetic activity cycle in epsilon Eri originally reported by Hatzes and coworkers, and we examine the archival data from previous observations spanning 45 years. The data show coexisting 3-year and 13-year periods leading into a broad activity minimum that resembles a Maunder minimum-like state, followed by the resurgence of a coherent 3-year cycle. The nearly continuous activity record suggests the simultaneous operation of two stellar dynamos with cycle periods of 2.95 ± 0.03 years and 12.7 ± 0.3 years, which, by analogy with the solar case, suggests a revised identification of the dynamo mechanisms that are responsible for the so-called "active" and "inactive" sequences as proposed by Böhm-Vitense. Finally, based on the observed properties of epsilon Eri, we argue that the rotational history of the Sun is what makes it an outlier in the context of magnetic cycles observed in other stars (as also suggested by its Li depletion), and that a Jovian-mass companion cannot be the universal explanation for the solar peculiarities. Title: As Big and As Good As It Gets: The Large Monolithic Imager for Lowell Observatory's 4.3-m Discovery Channel Telescope Authors: Massey, Philip; Dunham, E. W.; Bida, T. A.; Collins, P.; Hall, J. C.; Hunter, D. A.; Lauman, S.; Levine, S.; Neugent, K.; Nye, R.; Oliver, R.; Schleicher, D.; Zoonematkermani, S. Bibcode: 2013AAS...22134502M Altcode: The Large Monolithic Imager (LMI), a camera built at Lowell Observatory, is currently undergoing commissioning on Lowell's new 4.3-m Discovery Channel Telescope (DCT). At the heart of the LMI is the largest charge-coupled device (CCD) that can be built using current fabrication techniques, and the first of its kind to be made by e2v. The active area of the chip is 92.2mmx92.4mm, and has 6144 by 6160 15-micron pixels. Our choice of a single chip over a mosaic of smaller ones was inspired by the success of USNO in deploying a similarly ginormous device made by Semiconductor Technology Associates, Inc. There are some significant advantages that a (very!) large single CCD has over a mosaic of smaller ones. With a mosaic, one has to dither to fill in the gaps between the chips for complete areal coverage. This is not only costly in overhead, but it also poses a limitation in faint surface brightness studies, as the sky brightness is constantly changing during the dithering process. In addition, differences in the wavelength dependence of the DQE can lead to differences in the color terms from chip to chip in mosaics, requiring one to deal with each chip as a separate instrument (see the Local Group Galaxy photometry of Massey et al. 2006, AJ, 131, 2478). The LMI avoids these problems. The Discovery Channel Telescope is being built by Lowell Observatory in partnership with Discovery Communications. First light took place in May 2012. Institutional DCT partners include Boston University (in perpetuity), the University of Maryland, and the University of Toledo. More about the DCT can be found in the adjacent poster by Hall et al. The LMI has been made possible thanks to a National Science Foundation grant (AST-1005313). We are currently doing on-sky evaluation of the camera, as commissioning of the DCT progresses, determining color terms, photometric zero-points, astrometric characteristics, etc. We will present these results, along with technical details and many pretty pictures (!), in our poster. Title: Characterization of Potential U.S. Sites for the Cherenkov Telescope Array Authors: Ong, R. A.; Aune, T.; Hall, J. Bibcode: 2013ICRC...33.2848O Altcode: 2013arXiv1307.4719O The Cherenkov Telescope Array (CTA) is a major ground-based observatory proposed for gammaray astronomy. CTA is envisioned to consist of two large arrays of atmospheric Cherenkov telescopes for the study of sources of high-energy gamma rays in the energy range of a few tens of GeV to beyond 100 TeV. One array would be located in the southern hemisphere and one in the northern hemisphere. After a detailed search, we have identified two potential sites in the USA for the northern array. Both sites are located in northern Arizona. Here we describe the two sites and the deployment of instrumentation to characterize them. The characteristics of the sites, in terms of their atmospheric and climatic properties, are described. We show recent data from the automated monitoring equipment at the sites and compare these data to a commercial simulation. Details regarding the facilities and infrastructure required for the sites are also presented. Title: A Search for Exozodis with Kepler Authors: Stark, Christopher C.; Boss, A. P.; Weinberger, A. J.; Jackson, B.; Endl, M.; Cochran, W. D.; Caldwell, C.; Agol, E.; Ford, E. B.; Hall, J.; Ibrahim, K.; Li, J. Bibcode: 2013AAS...22110406S Altcode: Planets embedded within exozodiacal dust disks may form large scale clumpy dust structures by trapping dust into resonant orbits. When viewed edge-on, these clumpy dust structures periodically pass in front of their host star, creating orbit-long light curve variations potentially detectable with Kepler. Here I present the first search for these resonant structures in the inner regions of planetary systems by analyzing the light curves of planet candidate host stars identified by the Kepler mission. Our detection routine produced one promising candidate disk structure associated with a hot Jupiter planet candidate. However, radial velocity measurements show this planet candidate to be an eclipsing binary with an unusual periodic signal. We use our null result to place an upper limit on the frequency of high contrast resonant dust clumps, a useful metric for future missions that aim to image extrasolar planets in the inner regions of their planetary systems. Title: First Light from the 4.3-meter Discovery Channel Telescope At Lowell Observatory Authors: Hall, Jeffrey C.; Levine, S. Bibcode: 2013AAS...22134501H Altcode: Seven years after groundbreaking on July 12, 2005, the 4.3-meter Discovery Channel Telescope (DCT) is now complete and into commissioning. We obtained first light images in mid 2012 with a 4K x 4K CCD and have recently obtained our first images with the DCT's main camera, the 6K x 6K Large Monolithic Imager (LMI, see adjacent poster by Massey). We held a celebratory gala on July 21, 2012, in Flagstaff. The DCT's delivered image quality is regularly subarcsecond with near-uniform image quality across the FOV from zenith to >2 airmasses, although we have not fully commissioned the active optics system. We attribute this to the outstanding quality of the mirror figures, performed by the University of Arizona's College of Optical Sciences (for M1) and L3 Brashear (for M2). The instrument cube at the RC focus can accommodate four instruments plus the LMI. Designed and built at Lowell Observatory, the cube also contains the DCT's autoguider and wavefront sensor. First light instruments include the 4000 DeVeny spectrograph (the former KPNO White Spectrograph), a low-resolution, high-throughput IR spectrograph, and a higher-resolution IR spectrograph/imager being built by Goddard Space Flight Center in collaboration with the University of Maryland. We are seeking funding for long-slit and fiber-fed echelle spectrographs for higher resolution optical spectroscopy. The DCT can also be configured to host Nasmyth and prime focus instruments. Discovery Communications and its founder John Hendricks contributed $16M to the $53M cost of the telescope, in return for naming rights and first rights to public, educational use of images in their programming. Analysis of data and publication by astronomers in professional journals follows the same procedure as for any other major telescope facility. Discovery's first DCT feature, "Scanning the Skies," aired on September 9, 2012. Future outreach plans include initiating webcasts to classrooms via the Discovery Education networks, reaching 30-40M schoolchildren across the USA. The DCT partner consortium includes Boston University (in perpetuity), the University of Maryland, and the University of Toledo, all of whom have ongoing, long term access to the facility. Title: Comet Observations [H17 Angel Peaks Observatory] Authors: Hall, J. Bibcode: 2012MPC..80338..13H Altcode: No abstract at ADS Title: Comet C/2012 t5 (bressi) Authors: Knoefel, A.; Buzzi, L.; Bressi, T. H.; Nishiyama, K.; Sakamoto, T.; Masi, G.; Nocentini, F.; Masi, U.; Blythe, M.; Spitz, G.; Brungard, R.; Paige, J.; Festler, P.; McVey, T.; Valdivia, A.; Gall, C.; Dupouy, P.; de Vanssay, J. B.; Bryssinck, E.; Diepvens, A.; Miller, P.; Roche, P.; Tripp, A.; Miles, R.; Holmes, R.; Foglia, S.; Buz, L.; Vorobjov, T.; Johnson, J. A.; Boattini, A.; Christensen, E. J.; Gibbs, A. R.; Grauer, A. D.; Hill, R. E.; Kowalski, R. A.; Larson, S. M.; McNaught, R. H.; Ryan, W. H.; Sato, H.; Ligustri, R.; Guido, E.; Sostero, G.; Howes, N.; Hall, J.; Devore, H.; Hug, G.; Ruiz, P.; Koschny, D.; Busch, M.; Williams, G. V. Bibcode: 2012MPEC....U...38K Altcode: No abstract at ADS Title: Minor Planet Observations [H17 Angel Peaks Observatory] Authors: Hall, J. Bibcode: 2012MPC..80879...1H Altcode: No abstract at ADS Title: First dark matter search results from a 4-kg CF3I bubble chamber operated in a deep underground site Authors: Behnke, E.; Behnke, J.; Brice, S. J.; Broemmelsiek, D.; Collar, J. I.; Conner, A.; Cooper, P. S.; Crisler, M.; Dahl, C. E.; Fustin, D.; Grace, E.; Hall, J.; Hu, M.; Levine, I.; Lippincott, W. H.; Moan, T.; Nania, T.; Ramberg, E.; Robinson, A. E.; Sonnenschein, A.; Szydagis, M.; Vázquez-Jáuregui, E. Bibcode: 2012PhRvD..86e2001B Altcode: 2012arXiv1204.3094B New data are reported from the operation of a 4.0-kg CF3I bubble chamber in the 6800-foot-deep SNOLAB underground laboratory. The effectiveness of ultrasound analysis in discriminating alpha-decay background events from single nuclear recoils has been confirmed, with a lower bound of >99.3% rejection of alpha-decay events. Twenty single nuclear recoil event candidates and three multiple bubble events were observed during a total exposure of 553 kg-days distributed over three different bubble nucleation thresholds. The effective exposure for single bubble recoil-like events was 437.4 kg-days. A neutron background internal to the apparatus, of known origin, is estimated to account for five single nuclear recoil events and is consistent with the observed rate of multiple bubble events. The remaining excess of single bubble events exhibits characteristics indicating the presence of an additional background. These data provide new direct detection constraints on WIMP-proton spin-dependent scattering for WIMP masses >20GeV/c2 and demonstrate significant sensitivity for spin-independent interactions. Title: Comment on ``First Results of the Phase II SIMPLE Dark Matter Search'' Authors: Dahl, C. E.; Hall, J.; Lippincott, W. H. Bibcode: 2012PhRvL.108y9001D Altcode: 2011arXiv1111.6192D Comment on M. Felizardo et al., Phys. Rev. Lett. 105, 211301 (2010).PRLTAO0031-9007 The authors of the Letter offer a Reply.10.1103/PhysRevLett.105.211301 Title: Low-Mass WIMP Sensitivity and Statistical Discrimination of Electron and Nuclear Recoils by Varying Luke-Neganov Phonon Gain in Semiconductor Detectors Authors: Pyle, M.; Bauer, D. A.; Cabrera, B.; Hall, J.; Schnee, R. W.; Basu Thakur, R.; Yellin, S. Bibcode: 2012JLTP..167.1081P Altcode: 2012arXiv1201.3685P; 2012JLTP..tmp...81P; 2012JLTP..tmp..272P Amplifying the phonon signal in a semiconductor dark matter detector can be accomplished by operating at high voltage bias and converting the electrostatic potential energy into Luke-Neganov phonons. This amplification method has been validated at up to | E|=40 V/cm without producing leakage in CDMS II Ge detectors, allowing sensitivity to a benchmark WIMP with mass M χ =8 GeV/c2 and σ=1.8×10-42 cm2 (with significant sensitivity for M χ >2 GeV/c2) assuming flat electronic recoil backgrounds near threshold. Furthermore, for the first time we show that differences in Luke-Neganov gain for nuclear and electronic recoils can be used to discriminate statistically between low-energy background and a hypothetical WIMP signal by operating at two distinct voltage biases. Specifically, 99% of events have p-value <10-8 for a simulated 20 kg-day experiment with a benchmark WIMP signal with M χ =8 GeV/c2 and σ=3.3×10-41 cm2. Title: Mars Balloon Science Authors: Wolf, A.; Beegle, L.; Raymond, C.; Plaut, J.; Pollard, B.; Gim, Y.; Wu, X.; Hall, J. Bibcode: 2012LPICo1679.4294W Altcode: Balloons are uniquely suitable platforms for some observations important for Mars science and future human exploration. They are technologically within reach, and are small enough to be packaged as secondary payloads. Title: Minor Planet Observations [H17 Angel Peaks Observatory] Authors: Hall, J. Bibcode: 2012MPC..79335...1H Altcode: No abstract at ADS Title: Solar Twins and Stellar Maunder Minima Authors: Hall, Jeffrey C. Bibcode: 2012AAS...22050001H Altcode: In 1966, Olin C. Wilson undertook an answer to the question “Does the chromospheric activity of main-sequence stars vary with time, and if so, how?”, initiating the so-called HK Project at Mount Wilson Observatory, which resulted in a magnificent 43-year data set and which has spawned a number of complementary synoptic programs in both hemispheres. Subsequent developments, in particular the realization that activity controls angular momentum evolution in the stars and Sun, that solar activity modulates irradiance, and that there was a pronounced response of terrestrial climate to the Maunder Minimum, spurred efforts to identify solar twins, stars that Giusa Cayrel de Strobel required to possess “fundamental physical parameters very similar, if not identical to those of the Sun.” Non-cycling states appear to occur in the Mount Wilson stars and in other synoptic data with about the same frequency that the Sun’s grand minima occur in the long-term proxy record, suggesting that stellar analogs of the Maunder Minimum may be used to guide understanding of the Sun’s state in the late seventeenth century and, as appears possible given the extended Cycle 23/24 minimum, in the near future. However, the magnitude limits of the existing surveys have kept the sample of solar twins small and long-term monitoring programs have only recently begun to accumulate good time-domain data beyond the canonical HK-index. Addressing these and other issues toward understanding prolonged stellar minima is therefore a key area of inquiry in solar-stellar connection work for the next decade. I will summarize the state of the field and the most promising lines of work for the immediate future. I and my colleagues Wes Lockwood and Brian Skiff sincerely appreciate the National Science Foundation’s long-time support of stellar cycles work at Lowell Observatory. Title: Search for annual modulation in low-energy CDMS-II data Authors: CDMS Collaboration; Ahmed, Z.; Akerib, D. S.; Anderson, A. J.; Arrenberg, S.; Bailey, C. N.; Balakishiyeva, D.; Baudis, L.; Bauer, D. A.; Brink, P. L.; Bruch, T.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Cooley, J.; Cushman, P.; Daal, M.; DeJongh, F.; Di Stefano, P. C. F.; Dragowsky, M. R.; Fallows, S.; Figueroa-Feliciano, E.; Filippini, J.; Fox, J.; Fritts, M.; Golwala, S. R.; Hall, J.; Hertel, S. A.; Hofer, T.; Holmgren, D.; Hsu, L.; Huber, M. E.; Kamaev, O.; Kiveni, M.; Kos, M.; Leman, S. W.; Liu, S.; Mahapatra, R.; Mandic, V.; McCarthy, K. A.; Mirabolfathi, N.; Moore, D. C.; Nelson, H.; Ogburn, R. W.; Phipps, A.; Prasad, K.; Pyle, M.; Qiu, X.; Rau, W.; Reisetter, A.; Ricci, Y.; Saab, T.; Sadoulet, B.; Sander, J.; Schnee, R. W.; Seitz, D.; Serfass, B.; Speller, D.; Sundqvist, K. M.; Tarka, M.; Thakur, R. B.; Villano, A. N.; Welliver, B.; Yellin, S.; Yoo, J.; Young, B. A.; Zhang, J. Bibcode: 2012arXiv1203.1309C Altcode: We report limits on annual modulation of the low-energy event rate from the Cryogenic Dark Matter Search (CDMS II) experiment at the Soudan Underground Laboratory. Such a modulation could be produced by interactions from Weakly Interacting Massive Particles (WIMPs) with masses ~10 GeV/c^2. We find no evidence for annual modulation in the event rate of veto-anticoincident single-detector interactions consistent with nuclear recoils, and constrain the magnitude of any modulation to <0.06 event [keVnr kg day]^-1 in the 5-11.9 keVnr energy range at the 99% confidence level. These results disfavor an explanation for the reported modulation in the 1.2-3.2 keVee energy range in CoGeNT in terms of nuclear recoils resulting from elastic scattering of WIMPs at >98% confidence. For events consistent with electron recoils, no significant modulation is observed for either single- or multiple-detector interactions in the 3.0-7.4 keVee range. Title: Minor Planet Observations [H17 Angel Peaks Observatory] Authors: Hall, J. Bibcode: 2012MPC..77794...1H Altcode: No abstract at ADS Title: Lowell Observatory's Discovery Channel Telescope: Status, Key Science, and Opportunities Authors: Hall, Jeffrey C.; Levine, S. E. Bibcode: 2012AAS...21942224H Altcode: On July 12, 2005 Lowell Observatory broke ground at the construction site of the 4.3-meter Discovery Channel Telescope (DCT) near Happy Jack, AZ, 40 miles southeast of Flagstaff and at an elevation of 7,800'. The facility is now nearly complete, with testing of the primary mirror and active optics well underway and testing at RC focus imminent. First light is expected by May 2012.

Lowell and its partners, Boston University and the University of Maryland, will use the DCT for a variety of projects including studies of star formation in dwarf galaxies, cometary nuclei and KBOs, activity variations of Sun-like stars, and ToO follow-up observations of GRBs. Discovery Communications will use results of projects carried out by Lowell and its partners in broadcast and online media, reaching 99 million households in the USA and over 1.5 billion subscribers worldwide. The first major feature on the making of the telescope is expected to air on Discovery in June 2012.

In this poster we describe the general capabilities of the telescope, first light instrument suite, and key science projects. We also seek an additional partner to join us, BU, and UMD and invite interested parties or institutions to visit this poster and the adjacent one, presented by DCT Commissioning Scientist Stephen Levine, for more information. Title: The Lowell Observatory Predoctoral Scholar Program Authors: Hall, Jeffrey C.; Prato, L. A. Bibcode: 2012AAS...21923604H Altcode: Lowell Observatory is pleased to solicit applications for our Predoctoral Scholar Fellowship Program. Now beginning its fifth year, this program provides unique research opportunities to graduate students in good standing and currently enrolled at Ph.D. granting institutions. Lowell staff research spans a wide range of topics from astronomical instrumentation to icy bodies in our solar system, exoplanet science, and stellar populations and dwarf irregular galaxies.

The Observatory's new 4.3-meter Discovery Channel Telescope is on track for first light by mid-2012, making this a particularly exciting time in our history. Student research is expected to lead to a thesis dissertation appropriate for graduation at the doctoral level at the student's home institution.

Currently, three students are enrolled and three have successfully completed their thesis work at Lowell and moved on to postdocs and astronomy jobs elsewhere. The Observatory provides competitive compensation and full benefits to student scholars. For more information, see http://www2.lowell.edu/rsch/predoc.php and links therein. Applications for Fall 2012 are due by May 1, 2012. Title: Lowell Observatory's Discovery Channel Telescope: Telescope and Systems Specifications and Commissioning Status Authors: Levine, Stephen; Hall, J. C. Bibcode: 2012AAS...21942225L Altcode: Lowell Observatory's 4.3-meter Discovery Channel Telescope is in the process of being commissioned now. The telescope is located 40 miles southeast of Flagstaff,AZ at an elevation of 7,800 feet. On sky testing of the major subsystems began in early fall 2011, with commissioning work leading up to first light in late spring of 2012. We present a review of the design specifications of the telescope and its major subsystems. This is followed by a discussion of the commissioning time-line, and current status and performance of the telescope, and optics (including the active optics support system for the primary mirror). Title: Results of the First Observations with the Hamburg Robotic Telescope Authors: Mittag, M.; Hempelmann, A.; González-Pérez, J. N.; Schmitt, J. H. M. M.; Hall, J. C. Bibcode: 2011ASPC..448.1187M Altcode: 2011csss...16.1187M The results of the first scientific observations with the Hamburg Robotic Telescope (HRT) are presented. These observations were performed between October 2008 and August 2009. The goals of this program were a test of the observational performance of the telescope and the creation of a transformation equation from the HRT S-index to the Mount Wilson S-index. The mean of the deviations between the transformed HRT S-Indices and the corresponding Mount Wilson S-Indices is ≍4%. These deviations can be -- at least partially -- explained by stellar variability and the non-simultaneity of the observations. Furthermore, the first monitoring of several stars was performed. Title: Minor Planet Observations [H17 Angel Peaks Observatory] Authors: Hall, J. Bibcode: 2011MPC..77396...1H Altcode: No abstract at ADS Title: Minor Planet Observations [H17 Angel Peaks Observatory] Authors: Hall, J. Bibcode: 2011MPC..77005...1H Altcode: No abstract at ADS Title: A near-infrared spectrograph for the Discovery Channel Telescope Authors: Roe, H. G.; Dunham, E. W.; Bida, T. A.; Hall, J. C.; Degroff, W. Bibcode: 2011epsc.conf.1823R Altcode: 2011DPS....43.1823R Lowell Observatory is constructing the Discovery Channel Telescope (DCT) at Happy Jack, Arizona, approximately an hour from Lowell's main campus in Flagstaff, Arizona. The DCT is a 4.3-m optical/ infrared telescope. Construction of the telescope is complete and First Light of the DCT is planned for 2012Q2. In its initial configuration instruments will be co-mounted on a rotatable/selectable cube at the Cassegrain focus. Motorized deployable fold mirrors enable rapid switching amongst instruments. In the future the Nasmyth foci will be available for larger instruments as well. The first generation of instruments on DCT include: the Large Monolithic Imager (LMI), the Near-Infrared High-Throughput Spectrograph (NIHTS, pronounced "nights"), and the DeVeny optical spectrograph. The LMI contains a single large 6.1x6.1 K detector with a 12.5 arcmin2 FOV. NIHTS is a low resolution efficient near-infrared spectrograph and is the subject of this presentation. The DeVeny is Lowell's existing optical spectrograph with resolutions available between 500 and 4000. NIHTS is a low-resolution high-throughput infrared spectrograph covering 0.9-2.4 μm in a single fixed spectral setting at a resolution of »100. For simplicity and replicability NIHTS contains no moving parts. The science detector is a 10242 HAWAII-1 array. The fixed slit plate features an 80" long slit with several different slit widths (2,3,4 and 12 pixels) available along its length. The widest slit width is designed to allow accurate flux calibration, while the 3 and 4-pixel slits are closely matched to typical seeing at the DCT site (0.86" mean). Different resolutions will be rapidly selectable by dithering the telescope, and a typical observation is anticipated to involve a sequence of dithers both at the desired resolution and at SED resolution for calibration purposes. Offset guiding and wavefront sensing to control the active optics of the primary mirror are provided by the facility via deployable probes in the instrument cube. Target acquisition and slit-guiding is possible in the optical with the LMI or in the near-infrared with an In- GaAs slit-viewing camera that is part of NIHTS. Because the fold mirror to NIHTS is a dichroic, simultaneous optical imaging with LMI and near-infrared spectroscopy with NIHTS is enabled. NASA funded the construction of NIHTS as part of a larger project, the Kuiper Spectral Survey (KSS), and will be available to all users of the DCT. Title: Recent Advancements in Titan Balloon Techniques Authors: Reh, K.; Hall, J.; Vargas, A.; Colonius, T.; Dieudonne, W.; Coustenis, A.; Lunine, J.; Deramecourt, A. Bibcode: 2011epsc.conf..519R Altcode: 2011DPS....43..519R Suggestions for the use of balloons to explore Saturn's icy moon Titan have been proposed for more than 40 years. Many alternative mission concepts [1], [2], [4], [5] have been developed since that time, catalyzed by scientific discoveries resulting from the Voyager 1 flyby in 1980 and the Cassini- Huygens mission that arrived in 2004. The results from Cassini-Huygens, in particular, revealed Titan to be a complex and fascinating world with diverse topographical features and a methane-based hydrological cycle. The Huygens probe [3] demonstrated excellent visibility below a 10 km altitude with its high resolution images and measured low wind speeds at the surface (< 1-2 m/s). The motivation to return to Titan has intensified in the wake of these results and the increasing priority of related scientific questions. Because of the uniquely dense, high molecular weight atmosphere, very small diurnal temperature variations and low gravity, it is widely recognized that a buoyant vehicle could provide an unparalleled means of in situ exploration on a global scale. This poster provides a summary of recent advancements in Titan balloon techniques that someday will enable a return to Titan on a grand scale. Title: Comet Observations [H17 Angel Peaks Observatory] Authors: Hall, J. Bibcode: 2011MPC..76274..22H Altcode: No abstract at ADS Title: Recent Advancements in Titan Balloon Techniques Authors: Reh, K.; Hall, J.; Vargas, A.; Colonius, T.; Dieudonne, W.; Coustenis, A.; Lunine, J.; Deramecourt, A. Bibcode: 2011epsc.conf..522R Altcode: 2011DPS....43..522R Suggestions for the use of balloons to explore Saturn's icy moon Titan have been proposed for more than 40 years. Many alternative mission concepts [1], [2], [4], [5] have been developed since that time, catalyzed by scientific discoveries resulting from the Voyager 1 flyby in 1980 and the Cassini- Huygens mission that arrived in 2004. The results from Cassini-Huygens, in particular, revealed Titan to be a complex and fascinating world with diverse topographical features and a methane-based hydrological cycle. The Huygens probe [3] demonstrated excellent visibility below a 10 km altitude with its high resolution images and measured low wind speeds at the surface (< 1-2 m/s). The motivation to return to Titan has intensified in the wake of these results and the increasing priority of related scientific questions. Because of the uniquely dense, high molecular weight atmosphere, very small diurnal temperature variations and low gravity, it is widely recognized that a buoyant vehicle could provide an unparalleled means of in situ exploration on a global scale. This oral presentation provides a summary of recent advancements in Titan balloon techniques that someday will enable a return to Titan on a grand scale. Title: Minor Planet Observations [H17 Angel Peaks Observatory] Authors: Hall, J. Bibcode: 2011MPC..76561...1H Altcode: No abstract at ADS Title: Comet C/2011 s2 (kowalski) Authors: Skvarc, J.; Knoefel, A.; Haver, R.; Gorelli, R.; Buzzi, L.; Sarneczky, K.; Jung, M.; Bill, H.; Pettarin, E.; Kowalski, R. A.; Ahern, J. D.; Beshore, E. C.; Boattini, A.; Garradd, G. J.; Gibbs, A. R.; Tricarico, P.; Grauer, A. D.; Hill, R. E.; Larson, S. M.; McNaught, R. H.; Blythe, M.; Spitz, G.; Brungard, R.; Paige, J.; Festler, P.; McVey, T.; Valdivia, A.; Gall, C.; Emmerich, M.; Melchert, S.; Jaeger, M.; Prosperi, E.; Vollmann, W.; Klein, M.; Ryan, W. H.; Ryan, E. V.; Guido, E.; Sostero, G.; Howes, N.; Sato, H.; Baroni, S.; Concari, P.; Foglia, S.; Galli, G.; Tombelli, M.; Hall, J.; Holmes, R.; Vorobjov, T.; Hug, G.; Birtwhistle, P.; Williams, G. V. Bibcode: 2011MPEC....T...12S Altcode: No abstract at ADS Title: Combined limits on WIMPs from the CDMS and EDELWEISS experiments Authors: Ahmed, Z.; Akerib, D. S.; Armengaud, E.; Arrenberg, S.; Augier, C.; Bailey, C. N.; Balakishiyeva, D.; Baudis, L.; Bauer, D. A.; Benoît, A.; Bergé, L.; Blümer, J.; Brink, P. L.; Broniatowski, A.; Bruch, T.; Brudanin, V.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Censier, B.; Chapellier, M.; Chardin, G.; Charlieux, F.; Cooley, J.; Coulter, P.; Cox, G. A.; Cushman, P.; Daal, M.; Defay, X.; de Jesus, M.; Dejongh, F.; di Stefano, P. C. F.; Dolgorouki, Y.; Domange, J.; Dumoulin, L.; Dragowsky, M. R.; Eitel, K.; Fallows, S.; Figueroa-Feliciano, E.; Filippini, J.; Filosofov, D.; Fourches, N.; Fox, J.; Fritts, M.; Gascon, J.; Gerbier, G.; Gironnet, J.; Golwala, S. R.; Gros, M.; Hall, J.; Hennings-Yeomans, R.; Henry, S.; Hertel, S. A.; Hervé, S.; Holmgren, D.; Hsu, L.; Huber, M. E.; Juillard, A.; Kamaev, O.; Kiveni, M.; Kluck, H.; Kos, M.; Kozlov, V.; Kraus, H.; Kudryavtsev, V. A.; Leman, S. W.; Liu, S.; Loaiza, P.; Mahapatra, R.; Mandic, V.; Marnieros, S.; Martinez, C.; McCarthy, K. A.; Mirabolfathi, N.; Moore, D.; Nadeau, P.; Navick, X. -F.; Nelson, H.; Nones, C.; Ogburn, R. W.; Olivieri, E.; Pari, P.; Pattavina, L.; Paul, B.; Phipps, A.; Pyle, M.; Qiu, X.; Rau, W.; Reisetter, A.; Ricci, Y.; Robinson, M.; Rozov, S.; Saab, T.; Sadoulet, B.; Sander, J.; Sanglard, V.; Schmidt, B.; Schnee, R. W.; Scorza, S.; Seitz, D. N.; Semikh, S.; Serfass, B.; Sundqvist, K. M.; Tarka, M.; Torrento-Coello, A. S.; Vagneron, L.; Verdier, M. -A.; Walker, R. J.; Wikus, P.; Yakushev, E.; Yellin, S.; Yoo, J.; Young, B. A.; Zhang, J. Bibcode: 2011PhRvD..84a1102A Altcode: 2011arXiv1105.3377C The CDMS and EDELWEISS collaborations have combined the results of their direct searches for dark matter using cryogenic germanium detectors. The total data set represents 614kg·days equivalent exposure. A straightforward method of combination was chosen for its simplicity before data were exchanged between experiments. The results are interpreted in terms of limits on spin-independent weakly interacting, massive particle (WIMP)-nucleon cross section. For a WIMP mass of 90GeV/c2, where this analysis is most sensitive, a cross section of 3.3×10-44cm2 is excluded at 90% C.L. At higher WIMP masses, the combination improves the individual limits, by a factor 1.6 above 700GeV/c2. Alternative methods of combining the data provide stronger constraints for some ranges of WIMP masses and weaker constraints for others. Title: Observations and Orbits of Comets Authors: Tesi, L.; Bacci, P.; Fagioli, G.; Bacci, R.; Casali, M.; Coffano, A.; Marinello, W.; Micheli, M.; Pizzetti, G.; Cernis, K.; Zdanavicius, J.; Maskoliunas, M.; Haver, R.; Foglia, S.; Galli, G.; Buzzi, L.; Naves, R.; Campas, M.; Hasubick, W.; Donati, S.; McAndrew, S. G.; Sanchez C., A.; Donato, L.; Gonano, V.; Travagini, M.; Bill, H.; Baransky, A.; Buriev, A.; Ponomarenko, V.; Scotti, J. V.; Kowalski, R. A.; Ahern, J. D.; Beshore, E. C.; Boattini, A.; Garradd, G. J.; Gibbs, A. R.; Tricarico, P.; Grauer, A. D.; Hill, R. E.; Larson, S. M.; McNaught, R. H.; Blythe, M.; Spitz, G.; Brungard, R.; Paige, J.; Festler, P.; McVey, T.; Valdivia, A.; Brewington, H.; Dembicky, J.; Harvanek, M.; Ketzeback, B.; Long, D.; Pan, K.; Malanushenko, O.; McMillan, R.; Snedden, S.; Watters, S.; Sarneczky, K.; Durig, D. T.; Uriostegui, J. R.; Danusantoso, J. F.; Kharel, S.; Duenas, D. E.; Rice, A. C.; Vasquez, J. A.; Murphree, C. L.; Koury, E. S.; Castellano, J.; Ferrando, R.; Vidal, J. R.; Baldris, F.; Kocher, P.; Jaeger, M.; Prosperi, E.; Vollmann, W.; Rinner, C.; Kugel, F.; Nicolas, J.; Bel, J.; Borghini, W.; Bryssinck, E.; Sachot, G.; Soulier, J. F.; Diepvens, A.; Dangl, G.; Hills, K.; Takahashi, T.; Novichonok, A.; Baroni, S.; Concari, P.; Tombelli, M.; Chestnov, D.; Sato, H.; Herald, D.; Lister, T.; Guido, E.; Howes, N.; Sostero, G.; McCormick, J.; Primak, N.; Schultz, A.; Thiel, J.; Goggia, T.; Glinos, T.; Plaksa, S.; Elenin, L.; Hall-Angel Peaks Observatory, J.; Hall, J.; Holmes, R.; Vorobjov, T.; Linder, T.; Mills, M.; Hug, G.; Sherrod, P. C.; Bell, C.; Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.; Magain, P.; Limon, F.; Gonzalez, J.; Pena Ciriza, F.; Del Maes, A.; Hernandez, J. F.; Garcia, F.; Fletcher, J.; Climent, T.; Williams, G. V. Bibcode: 2011MPEC....N...13T Altcode: No abstract at ADS Title: Comet Observations [H17 Angel Peaks Observatory] Authors: Hall, J. Bibcode: 2011MPC..75359..10H Altcode: No abstract at ADS Title: Minor Planet Observations [H17 Angel Peaks Observatory] Authors: Hall, J. Bibcode: 2011MPC..75509...1H Altcode: No abstract at ADS Title: 2011 ME Authors: Blythe, M.; Spitz, G.; Brungard, R.; Paige, J.; Festler, P.; McVey, T.; Valdivia, A.; McGaha, J. E.; Hall-Angel Peaks Observatory, J.; Hall, J.; Hug, G.; Birtwhistle, P.; Tomatic, A. U. Bibcode: 2011MPEC....M...24B Altcode: No abstract at ADS Title: Minor Planet Observations [H17 Angel Peaks Observatory] Authors: Hall, J. Bibcode: 2011MPC..75287...1H Altcode: No abstract at ADS Title: Search for inelastic dark matter with the CDMS II experiment Authors: Ahmed, Z.; Akerib, D. S.; Arrenberg, S.; Bailey, C. N.; Balakishiyeva, D.; Baudis, L.; Bauer, D. A.; Brink, P. L.; Bruch, T.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Cooley, J.; Do Couto E Silva, E.; Cushman, P.; Daal, M.; Dejongh, F.; di Stefano, P.; Dragowsky, M. R.; Duong, L.; Fallows, S.; Figueroa-Feliciano, E.; Filippini, J.; Fox, J.; Fritts, M.; Golwala, S. R.; Hall, J.; Hennings-Yeomans, R.; Hertel, S. A.; Holmgren, D.; Hsu, L.; Huber, M. E.; Kamaev, O.; Kiveni, M.; Kos, M.; Leman, S. W.; Liu, S.; Mahapatra, R.; Mandic, V.; McCarthy, K. A.; Mirabolfathi, N.; Moore, D.; Nelson, H.; Ogburn, R. W.; Phipps, A.; Pyle, M.; Qiu, X.; Ramberg, E.; Rau, W.; Razeti, M.; Reisetter, A.; Resch, R.; Saab, T.; Sadoulet, B.; Sander, J.; Schnee, R. W.; Seitz, D. N.; Serfass, B.; Sundqvist, K. M.; Tarka, M.; Wikus, P.; Yellin, S.; Yoo, J.; Young, B. A.; Zhang, J. Bibcode: 2011PhRvD..83k2002A Altcode: 2010arXiv1012.5078C Results are presented from a reanalysis of the entire five-tower data set acquired with the Cryogenic Dark Matter Search (CDMS II) experiment at the Soudan Underground Laboratory, with an exposure of 969 kg-days. The analysis window was extended to a recoil energy of 150 keV, and an improved surface-event background-rejection cut was defined to increase the sensitivity of the experiment to the inelastic dark matter (iDM) model. Three dark matter candidates were found between 25 keV and 150 keV. The probability to observe three or more background events in this energy range is 11%. Because of the occurrence of these events, the constraints on the iDM parameter space are slightly less stringent than those from our previous analysis, which used an energy window of 10-100 keV. Title: Observations and Orbits of Comets Authors: Tesi, L.; Bacci, P.; Fagioli, G.; Gajdos, S.; Buzzi, L.; Naves, R.; Campas, M.; Kadota, K.; Klein, M.; Jung, M.; Feger, F.; Bill, H.; Blythe, M.; Spitz, G.; Brungard, R.; Paige, J.; Festler, P.; McVey, T.; Valdivia, A.; Brewington, H.; Dembicky, J.; Harvanek, M.; Ketzeback, B.; Long, D.; Pan, K.; Malanushenko, O.; McMillan, R.; Snedden, S.; Watters, S.; Sarneczky, K.; Durig, D. T.; Uriostegui, J. R.; Tran, J. T.; Nichols, E. M.; Strickland, T. D.; Torres Perez, J. A.; Murp, C. L.; Essix, G. V.; Williams, K. A.; Morris, T. A.; Rice, A. C.; Va, J. A.; Duenas, D. E.; Kharel, S.; Grishaw, A. C.; Emerson, S. E.; Guhlin, A. R.; Edman, J. R.; Johnson, E. C.; Danusantoso, J. F.; Castellano, J.; Vidal, J. R.; Baldris, F.; Salto, J. L.; Salto, A.; Jaeger, M.; Prosperi, E.; Vollmann, W.; Rinner, C.; Kugel, F.; Nicolas, J.; Noel, T.; Hills, K.; Takahashi, T.; Bryssinck, E.; Plaksa, S.; McNaught, R. H.; Ahern, J. D.; Beshore, E. C.; Boattini, A.; Garradd, G. J.; Gibbs, A. R.; Grauer, A. D.; Hill, R. E.; Kowalski, R. A.; Larson, S. M.; Lister, T.; Fulton, B. J.; Dymock, R.; Sato, H.; Ligustri, R.; Chestnov, D.; Novichonok, A.; Elenin, L.; Hall, J.; Sherrod, P. C.; Bell, C.; Limon, F.; Gonzalez, J.; Busch, M.; Drefke, A.; Geffert, P.; Koschny, D.; Kracht, R.; Kresken, R.; Hernandez, J. F.; Garcia, F.; Climent, T. Bibcode: 2011MPEC....M...31T Altcode: No abstract at ADS Title: Minor Planet Observations [H17 Angel Peaks Observatory] Authors: Hall, J. Bibcode: 2011MPC..75003...1H Altcode: No abstract at ADS Title: Results from a Low-Energy Analysis of the CDMS II Germanium Data Authors: Ahmed, Z.; Akerib, D. S.; Arrenberg, S.; Bailey, C. N.; Balakishiyeva, D.; Baudis, L.; Bauer, D. A.; Brink, P. L.; Bruch, T.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Cooley, J.; Do Couto E Silva, E.; Cushman, P.; Daal, M.; Dejongh, F.; di Stefano, P.; Dragowsky, M. R.; Duong, L.; Fallows, S.; Figueroa-Feliciano, E.; Filippini, J.; Fox, J.; Fritts, M.; Golwala, S. R.; Hall, J.; Hennings-Yeomans, R.; Hertel, S. A.; Holmgren, D.; Hsu, L.; Huber, M. E.; Kamaev, O.; Kiveni, M.; Kos, M.; Leman, S. W.; Liu, S.; Mahapatra, R.; Mandic, V.; McCarthy, K. A.; Mirabolfathi, N.; Moore, D.; Nelson, H.; Ogburn, R. W.; Phipps, A.; Pyle, M.; Qiu, X.; Ramberg, E.; Rau, W.; Reisetter, A.; Resch, R.; Saab, T.; Sadoulet, B.; Sander, J.; Schnee, R. W.; Seitz, D. N.; Serfass, B.; Sundqvist, K. M.; Tarka, M.; Wikus, P.; Yellin, S.; Yoo, J.; Young, B. A.; Zhang, J. Bibcode: 2011PhRvL.106m1302A Altcode: 2010arXiv1011.2482C We report results from a reanalysis of data from the Cryogenic Dark Matter Search (CDMS II) experiment at the Soudan Underground Laboratory. Data taken between October 2006 and September 2008 using eight germanium detectors are reanalyzed with a lowered, 2 keV recoil-energy threshold, to give increased sensitivity to interactions from weakly interacting massive particles (WIMPs) with masses below ∼10GeV/c2. This analysis provides stronger constraints than previous CDMS II results for WIMP masses below 9GeV/c2 and excludes parameter space associated with possible low-mass WIMP signals from the DAMA/LIBRA and CoGeNT experiments. Title: Minor Planet Observations [H17 Angel Peaks Observatory] Authors: Hall, J. Bibcode: 2011MPC..74630...1H Altcode: No abstract at ADS Title: Minor Planet Observations [H17 Angel Peaks Observatory] Authors: Hall, J. Bibcode: 2011MPC..74230...1H Altcode: No abstract at ADS Title: Minor Planet Observations [H17 Angel Peaks Observatory] Authors: Hall, J. Bibcode: 2011MPC..73908...1H Altcode: No abstract at ADS Title: Improved Limits on Spin-Dependent WIMP-Proton Interactions from a Two Liter CF3I Bubble Chamber Authors: Behnke, E.; Behnke, J.; Brice, S. J.; Broemmelsiek, D.; Collar, J. I.; Cooper, P. S.; Crisler, M.; Dahl, C. E.; Fustin, D.; Hall, J.; Hinnefeld, J. H.; Hu, M.; Levine, I.; Ramberg, E.; Shepherd, T.; Sonnenschein, A.; Szydagis, M. Bibcode: 2011PhRvL.106b1303B Altcode: 2010arXiv1008.3518B Data from the operation of a bubble chamber filled with 3.5 kg of CF3I in a shallow underground site are reported. An analysis of ultrasound signals accompanying bubble nucleations confirms that alpha decays generate a significantly louder acoustic emission than single nuclear recoils, leading to an efficient background discrimination. Three dark matter candidate events were observed during an effective exposure of 28.1kgday, consistent with a neutron background. This observation provides strong direct detection constraints on weakly interacting massive particle (WIMP)-proton spin-dependent scattering for WIMP masses >20GeV/c2. Title: Minor Planet Observations [H17 Angel Peaks Observatory] Authors: Hall, J. Bibcode: 2011MPC..73453...2H Altcode: No abstract at ADS Title: Lessons from Solar Twins Authors: Hall, Jeffrey Bibcode: 2010S&T...120a..22H Altcode: No abstract at ADS Title: The Discovery Channel Telescope: early integration Authors: Smith, Byron; Chylek, Tomas; Degroff, Bill; Finley, David; Hall, Jeffrey; Lotz, Paul J.; McCreight, Brad; Venetiou, Alexander Bibcode: 2010SPIE.7733E..0AS Altcode: 2010SPIE.7733E...8S The Discovery Channel Telescope (DCT) is a 4.3-meter astronomical research telescope being built in northern Arizona as a partnership between Discovery Communications and Lowell Observatory. The telescope will be able to support substantial instrument payloads at Cassegrain, Nasmyth, and prime foci, and high observing cadences. The first-light configuration will be as an f/6.1 Ritchey-Chrétien at Cassegrain with a 30 arc-minute field-of-view. Major facility work is complete, and the telescope is currently in the integration phase with first-light anticipated in 2011. We present an overview of the design and progress to date, and include plans for final integration, commissioning, and early science. Title: Computational Modeling and Experiments of Natural Convection for a Titan Montgolfiere Authors: Samanta, Arnab; Appelö, Daniel; Colonius, Tim; Nott, Julian; Hall, Jeffrey Bibcode: 2010AIAAJ..48.1007S Altcode: No abstract at ADS Title: Structure and rifting evolution of the northern Newfoundland Basin from Erable multichannel seismic reflection profiles across the southeastern margin of Flemish Cap Authors: Welford, J. K.; Smith, J. A.; Hall, J.; Deemer, S.; Srivastava, S. P.; Sibuet, J. -C. Bibcode: 2010GeoJI.180..976W Altcode: We present the results from processing and interpreting five lines from the 1992 Erable multichannel seismic reflection experiment extending from the southeastern margin of Flemish Cap into the northern Newfoundland Basin. These profiles reveal significant along strike variations in the rifting styles experienced by Flemish Cap. In the southwest, a 100-km-wide transition zone is identified between thinned continental crust and thin oceanic crust. Similar to the conjugate Galicia Bank and Iberian margins, this transition zone contains a section of deep basement adjacent to a series of shallower ridges and is interpreted as exhumed serpentinized mantle. Along strike towards the northeast, this transition zone pinches out completely within 100 km and is replaced by thin oceanic crust directly adjacent to thinned continental crust. By interpreting nearby seismic profiles and profiles on the conjugate margins using the same classification criteria, we construct regional maps of the distribution of crustal domains on both sides of the North Atlantic. These maps reveal significant variations in rifting style on the conjugate margins and along strike of each margin and also highlight the role of ancient transfer zones in compartmentalizing these rifting variations into four distinct regions. We propose that the limited localization of shallow topographically high serpentinized peridotite ridges on the Newfoundland-Iberia and Flemish Cap-Galicia Bank conjugate margins, was directly related to an increase in the rate of extension following the separation of Flemish Cap and Galicia Bank which exhumed deeper, less serpentinized mantle. Title: Dark Matter Search Results from the CDMS II Experiment Authors: CDMS II Collaboration; Ahmed, Z.; Akerib, D. S.; Arrenberg, S.; Bailey, C. N.; Balakishiyeva, D.; Baudis, L.; Bauer, D. A.; Brink, P. L.; Bruch, T.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Cooley, J.; Cushman, P.; Daal, M.; DeJongh, F.; Dragowsky, M. R.; Duong, L.; Fallows, S.; Figueroa-Feliciano, E.; Filippini, J.; Fritts, M.; Golwala, S. R.; Grant, D. R.; Hall, J.; Hennings-Yeomans, R.; Hertel, S. A.; Holmgren, D.; Hsu, L.; Huber, M. E.; Kamaev, O.; Kiveni, M.; Kos, M.; Leman, S. W.; Mahapatra, R.; Mandic, V.; McCarthy, K. A.; Mirabolfathi, N.; Moore, D.; Nelson, H.; Ogburn, R. W.; Phipps, A.; Pyle, M.; Qiu, X.; Ramberg, E.; Rau, W.; Reisetter, A.; Saab, T.; Sadoulet, B.; Sander, J.; Schnee, R. W.; Seitz, D. N.; Serfass, B.; Sundqvist, K. M.; Tarka, M.; Wikus, P.; Yellin, S.; Yoo, J.; Young, B. A.; Zhang, J. Bibcode: 2010Sci...327.1619C Altcode: 2009arXiv0912.3592T Astrophysical observations indicate that dark matter constitutes most of the mass in our universe, but its nature remains unknown. Over the past decade, the Cryogenic Dark Matter Search (CDMS II) experiment has provided world-leading sensitivity for the direct detection of weakly interacting massive particle (WIMP) dark matter. The final exposure of our low-temperature germanium particle detectors at the Soudan Underground Laboratory yielded two candidate events, with an expected background of 0.9 ± 0.2 events. This is not statistically significant evidence for a WIMP signal. The combined CDMS II data place the strongest constraints on the WIMP-nucleon spin-independent scattering cross section for a wide range of WIMP masses and exclude new parameter space in inelastic dark matter models. Title: Analysis of the low-energy electron-recoil spectrum of the CDMS experiment Authors: Ahmed, Z.; Akerib, D. S.; Arrenberg, S.; Bailey, C. N.; Balakishiyeva, D.; Baudis, L.; Bauer, D. A.; Beaty, J.; Brink, P. L.; Bruch, T.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Cooley, J.; Cushman, P.; Dejongh, F.; Dragowsky, M. R.; Duong, L.; Figueroa-Feliciano, E.; Filippini, J.; Fritts, M.; Golwala, S. R.; Grant, D. R.; Hall, J.; Hennings-Yeomans, R.; Hertel, S.; Holmgren, D.; Hsu, L.; Huber, M. E.; Kamaev, O.; Kiveni, M.; Kos, M.; Leman, S. W.; Mahapatra, R.; Mandic, V.; Moore, D.; McCarthy, K. A.; Mirabolfathi, N.; Nelson, H.; Ogburn, R. W.; Pyle, M.; Qiu, X.; Ramberg, E.; Rau, W.; Reisetter, A.; Saab, T.; Sadoulet, B.; Sander, J.; Schnee, R. W.; Seitz, D. N.; Serfass, B.; Sundqvist, K. M.; Wang, G.; Wikus, P.; Yellin, S.; Yoo, J.; Young, B. A. Bibcode: 2010PhRvD..81d2002A Altcode: 2009arXiv0907.1438A We report on the analysis of the low-energy electron-recoil spectrum from the CDMS II experiment using data with an exposure of 443.2 kg-days. The analysis provides details on the observed counting rate and possible background sources in the energy range of 2-8.5 keV. We find no significant excess of a peaked contribution to the total counting rate above the background model, and compare this observation to the recent DAMA results. In the framework of a conversion of a dark matter particle into electromagnetic energy, our 90% confidence level upper limit of 0.246events/kg/day at 3.15 keV is lower than the total rate above background observed by DAMA. In absence of any specific particle physics model to provide the scaling in cross section between NaI and Ge, we assume a Z2 scaling. With this assumption the observed rate in DAMA remains higher than the upper limit in CDMS. Under the conservative assumption that the modulation amplitude is 6% of the total rate we obtain upper limits on the modulation amplitude a factor of ∼2 lower than observed by DAMA, constraining some possible interpretations of this modulation. Title: The Night Time Sun: X-Ray Observations of the Solar Twin 18 Scorpii Authors: Coughlin, Jared; Guinan, E. F.; Engle, S. G.; DeWarf, L.; Hall, J. C.; DePasquale, J.; Thompson, R. R. Bibcode: 2010AAS...21542417C Altcode: 2010BAAS...42..333C Since the study by Porto de Mello & da Silva(1997,ApJ,482) the nearby 5.5-mag G2V star 18 Scorpii has been considered one of the best solar twins, being a near-perfect match to our Sun in all physical characteristics(Teff, R, log(g), MV, metallicity, luminosity, and chromospheric CaII H&K emissions). Also, 18 Sco has a rotation period of PRot=22.7±0.5 days(Petit et al. 2008), which is very close to that of the Sun. In addition, ongoing CaII H&K observations carried out at Lowell Observatory indicate a possible 7-11yr. activity cycle. However, until our X-ray observations with XMM-Newton in Aug 2005, 18 Sco had never been observed in this spectral region. The analysis of these measurements yield an X-ray luminosity and coronal plasma temperature of LX=8±1.5ergs/s and TCorona 1.5-2 MK. These data were taken near mid-cycle and match very closely with those of the Sun(LX 6-30ergs/s TCorona 2 MK). In addition to these measures, interferometric angular diameter measures with the Palomar Testbed Interferometer yield a stellar diameter of 0.975±0.162 R/RSun. Fitting the star's observed properties to current evolution models indicates a mass of M=0.98±0.05 MSun and an age of 4-5 Gyr. This age estimate (4.4±0.4 Gyr) is in excellent agreement with an age inferred from age-rotation-activity relations from the Sun in Time project. These observations demonstrate that 18 Sco is a bonafide solar twin out through the X-ray portion of the spectrum. Such a distinction makes is a very important star to use as a proxy "Night Time” Sun for standardization purposes, an excellent candidate for asteroseismic studies, and as a target for searches for life-bearing terrestrial planets.

This research is supported by grants from NASA/FUSE, NSF/RUI and by the Villanova University Research for Undergraduates Award Program, which we gratefully acknowledge. Title: 51 Pegasi - a planet-bearing Maunder minimum candidate Authors: Poppenhäger, K.; Robrade, J.; Schmitt, J. H. M. M.; Hall, J. C. Bibcode: 2009A&A...508.1417P Altcode: 2009arXiv0911.4862P We observed 51 Peg, the first detected planet-bearing star, in a 55 ks XMM-Newton pointing and in 5 ks pointings each with Chandra HRC-I and ACIS-S. The star has a very low count rate in the XMM observation, but is clearly visible in the Chandra images due to the detectors' different sensitivity at low X-ray energies. This allows a temperature estimate for 51 Peg's corona of T⪉ 1 MK; the detected ACIS-S photons can be plausibly explained by emission lines of a very cool plasma near 200 eV. The constantly low X-ray surface flux and the flat-activity profile seen in optical Ca II data suggest that 51 Peg is a Maunder minimum star; an activity enhancement due to a Hot Jupiter, as proposed by recent studies, seems to be absent. The star's X-ray fluxes in different instruments are consistent with the exception of the HRC Imager, which might have a larger effective area below 200 eV than given in the calibration. Title: The Cryogenic Dark Matter Search (CDMS) experiment: Results, status and perspective Authors: Mirabolfathi, N.; Ahmed, Z.; Akerib, D. S.; Arrenberg, S.; Bailey, C. N.; Balakishiyeva, D.; Baudis, L.; Bauer, D. A.; Beaty, J.; Brink, P. L.; Bruch, T.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Clark, K.; Cooley, J.; Cushman, P.; Dejongh, F.; Dragowski, M. R.; Duong, L.; Figueroa-Feliciano, E.; Filippini, J.; Fritts, M.; Golwala, S. R.; Grant, D. R.; Hall, J.; Hennins-Yeomans, R.; Hertel, S.; Homgren, D.; Hsu, L.; Huber, M. E.; Kamaev, O.; Kiveni, M.; Kos, M.; Leman, S. W.; Mahapatra, R.; Mandic, V.; Moore, D.; McCarthy, K. A.; Nelson, H.; Ogburn, R. W.; Pyle, M.; Qiu, X.; Ramberg, E.; Rau, W.; Reisetter, A.; Saab, T.; Sadoulet, B.; Sanders, J.; Schnee, R. W.; Seitz, D. N.; Serfass, B.; Sundqvist, K. M.; Wang, G.; Yellin, S.; Yoo, J.; Young, B. A. Bibcode: 2009AIPC.1185..623M Altcode: The Cryogenic Dark Matter Search experiment (CDMS) is using Phonon+Ionization detectors to search for Dark Matter in the form of Weakly Interactive Massive Particles (WIMPs). We report on new results from the operation of CDMS five ``towers'' at Soudan underground laboratory. With new and more massive detectors, SuperCDMS project has been started since March 2009. We report on the current status of SuperCDMS and its perspective. Title: The Cryogenic Dark Matter Search (CDMS) : Present Status and Future Authors: Brink, P. L.; Ahmed, Z.; Akerib, D. S.; Bailey, C. N.; Balakishiyeva, D.; Bauer, D. A.; Beaty, J.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Cooley, J.; Do Couto E Silva, E.; Cushman, P.; Dejongh, F.; Dragowsky, M. R.; Duong, L.; Figueroa-Feliciano, E.; Filippini, J.; Fritts, M.; Golwala, S. R.; Grant, D. R.; Hall, J.; Hennings-Yeomans, R.; Hertel, S.; Hojem, A.; Holmgren, D.; Hsu, L.; Huber, M. E.; Kamaev, O.; Kos, M.; Kiveni, M.; Leman, S. W.; Mahapatra, R.; Mandic, V.; McCarthy, K. A.; Moore, D.; Mirabolfathi, N.; Nelson, H.; Novak, L.; Ogburn, R. W.; Pyle, M.; Qiu, X.; Ramberg, E.; Rau, W.; Reisetter, A.; Saab, T.; Sadoulet, B.; Sander, J.; Schmitt, R.; Schnee, R. W.; Seitz, D. N.; Serfass, B.; Sundqvist, K. M.; Tomada, A.; Wang, G.; Wikus, P.; Yellin, S.; Yoo, J.; Young, B. A. Bibcode: 2009AIPC.1182..260B Altcode: The CDMS collaboration utilizes Ge detectors for their Weakly Interacting Massive Particle (WIMP) search at the Soudan mine, Minnesota. The final data run of CDMS II is complete and a detector upgrade for SuperCDMS has commenced. A SuperTower of five 1-inch thick Ge crystals has been installed and undergoing commissioning. Its surface-event rejection capability should allow SuperCDMS to continue to run background free for the next proposed phases: 15 kg Ge deployment at Soudan, and up to 150 kg Ge deployment at SNOLAB. Recent detector advances to allow a 1 tonne Ge experiment are also discussed. Title: Search for Axions with the CDMS Experiment Authors: Ahmed, Z.; Akerib, D. S.; Arrenberg, S.; Bailey, C. N.; Balakishiyeva, D.; Baudis, L.; Bauer, D. A.; Beaty, J.; Brink, P. L.; Bruch, T.; Bunker, R.; Cabrera, B.; Caldwell, D. O.; Cooley, J.; Cushman, P.; Dejongh, F.; Dragowsky, M. R.; Duong, L.; Figueroa-Feliciano, E.; Filippini, J.; Fritts, M.; Golwala, S. R.; Grant, D. R.; Hall, J.; Hennings-Yeomans, R.; Hertel, S.; Holmgren, D.; Hsu, L.; Huber, M. E.; Kamaev, O.; Kiveni, M.; Kos, M.; Leman, S. W.; Mahapatra, R.; Mandic, V.; Moore, D.; McCarthy, K. A.; Mirabolfathi, N.; Nelson, H.; Ogburn, R. W.; Pyle, M.; Qiu, X.; Ramberg, E.; Rau, W.; Reisetter, A.; Saab, T.; Sadoulet, B.; Sander, J.; Schnee, R. W.; Seitz, D. N.; Serfass, B.; Sundqvist, K. M.; Tarka, M.; Wang, G.; Yellin, S.; Yoo, J.; Young, B. A. Bibcode: 2009PhRvL.103n1802A Altcode: 2009arXiv0902.4693C We report on the first axion search results from the Cryogenic Dark Matter Search (CDMS) experiment at the Soudan Underground Laboratory. An energy threshold of 2 keV for electron-recoil events allows a search for possible solar axion conversion into photons or local galactic axion conversion into electrons in the germanium crystal detectors. The solar axion search sets an upper limit on the Primakov coupling gaγγ of 2.4×10-9GeV-1 at the 95% confidence level for an axion mass less than 0.1keV/c2. This limit benefits from the first precise measurement of the absolute crystal plane orientations in this type of experiment. The galactic axion search analysis sets a world-leading experimental upper limit on the axioelectric coupling gaēe of 1.4×10-12 at the 90% confidence level for an axion mass of 2.5keV/c2. Title: The Activity and Variability of the Sun and Sun-Like Stars. II. Contemporaneous Photometry and Spectroscopy of Bright Solar Analogs Authors: Hall, Jeffrey C.; Henry, Gregory W.; Lockwood, G. Wesley; Skiff, Brian A.; Saar, Steven H. Bibcode: 2009AJ....138..312H Altcode: We present 14 years of contemporaneous photometric and spectroscopic observations of 28 solar analog stars, taken with the Tennessee State University Automatic Photometric Telescopes at Fairborn Observatory and the Solar-Stellar Spectrograph at Lowell Observatory. These are the best observed and most nearly Sun-like of the targets in our magnitude-limited (V <= 7.5) sample. The correlations between luminosity and activity reveal the expected inverse activity-brightness correlations for active stars. Strong direct correlations between activity and brightness are not prevalent for the less active solar age stars, but are precision limited. The Sun does not appear to have unusually low photometric variability when compared with the most Sun-like inactive solar analogs. We present evidence that the activity index R'HK is not a good discriminant of Maunder Minimum candidate stars. On the basis of a star that appears to have transitioned from a low-variability state to a cycling state, we investigate the regime in which stars might switch from faculae-dominated to spot-dominated variations. Title: A Venus Flagship Mission: Report of the Venus Science and Technology Definition Team Authors: Bullock, M. A.; Senske, D. A.; Balint, T. S.; Benz, A.; Campbell, B. A.; Chassefiere, E.; Colaprete, A.; Cutts, J. A.; Glaze, L.; Gorevan, S.; Grinspoon, D. H.; Hall, J.; Hashimoto, G. L.; Head, J. W.; Hunter, G.; Johnson, N.; Kerzhanovich, V. V.; Kiefer, W. S.; Kolawa, E. A.; Kremic, T.; Kwok, J.; Limaye, S. S.; Mackwell, S. J.; Marov, M. Y.; Ocampo, A.; Schubert, G.; Stofan, E. R.; Svedhem, H.; Titov, D. V.; Treiman, A. H. Bibcode: 2009LPI....40.2410B Altcode: The Venus STDT has defined the goals, objectives, mission architecture, science investigations and payload for a Flagship-class mission to Venus. The mission puts advanced exploration capabilities in orbit, in the atmosphere, and on the surface. Title: The Cryogenic Dark Matter Search (CDMS) experiment: Results and prospects Authors: Brink, P. L.; Ahmed, Z.; Akerib, D. S.; Bailey, C. N.; Bauer, D. A.; Beaty, J.; Bunker, R.; Burke, S.; Cabrera, B.; Caldwell, D. O.; Cooley, J.; Cushman, P.; DeJongh, F.; Dragowsky, M. R.; Duong, L.; Figueroa-Feliciano, E.; Filippini, J.; Fritts, M.; Golwala, S. R.; Grant, D. R.; Hall, J.; Hennings-Yeomans, R.; Hertel, S.; Holmgren, D.; Huber, M. E.; Mahapatra, R.; Mandic, V.; McCarthy, K. A.; Mirabolfathi, N.; Nelson, H.; Novak, L.; Ogburn, R. W.; Pyle, M.; Qiu, X.; Ramberg, E.; Rau, W.; Reisetter, A.; Saab, T.; Sadoulet, B.; Sander, J.; Schmitt, R.; Schnee, R. W.; Seitz, D. N.; Serfass, B.; Sirois, A.; Sundqvist, K. M.; Tomada, A.; Wang, G.; Yellin, S.; Yoo, J.; Young, B. A. Bibcode: 2009JPhCS.150a2006B Altcode: Weakly Interacting Massive Particles (WIMPs) are a strong candidate for the Cold Dark Matter of the Universe. CDMS-II is a direct-search WIMP search experiment, operating at 50 mK and housed at the Soudan mine, Minnesota. The 250 gram Ge detectors utilize athermal phonon sensors where tungsten transition edge sensors are operated in negative electrothermal feedback. The search at Soudan is ongoing with an expected final reach of CDMS-II by the end of 2008 of a WIMP-nucleon cross-section sensitivity of 2.1 x10-44 cm2, at a WIMP mass of 60 GeV/c2. To proceed further, we have proposed the SuperCDMS program. Title: The Stars as a Sun: Secular Variations of Cycling and Non-Cycling Stars Authors: Hall, Jeffrey C.; Giampapa, Mark S.; Henry, Gregory W.; Lean, Judith L.; Saar, Steven H.; Soderblom, David R. Bibcode: 2009astro2010S.111H Altcode: No abstract at ADS Title: Progress and Key Projects of the Discovery Channel Telescope at Lowell Observatory Authors: Hall, Jeffrey C.; Smith, B.; Chylek, T.; DeGroff, B.; Lotz, P.; Venetiou, A. J.; Westcott, K.; Bida, T.; Dunham, E. W.; Zoonematkermani, S.; Collins, P.; Millis, R. L. Bibcode: 2009AAS...21347412H Altcode: 2009BAAS...41R.429H The Discovery Channel Telescope (DCT) is a 4.2-m instrument under construction 35 miles southeast of Flagstaff, Arizona. All first light components of the telescope are actively being worked, with commissioning scheduled for early 2011. Planned first generation instruments include an imager, IR spectrograph, and optical spectrograph at the RC focus. The design also provides for observations at prime and Nasmyth foci. Research and results from the telescope will be widely disseminated through Lowell Observatory's partnership with Discovery Communications. I will describe the design and construction status of the telescope, as well as the key projects identified for the initial science operations. Title: Search for Weakly Interacting Massive Particles with the First Five-Tower Data from the Cryogenic Dark Matter Search at the Soudan Underground Laboratory Authors: Ahmed, Z.; Akerib, D. S.; Arrenberg, S.; Attisha, M. J.; Bailey, C. N.; Baudis, L.; Bauer, D. A.; Beaty, J.; Brink, P. L.; Bruch, T.; Bunker, R.; Burke, S.; Cabrera, B.; Caldwell, D. O.; Cooley, J.; Cushman, P.; Dejongh, F.; Dragowsky, M. R.; Duong, L.; Emes, J.; Figueroa-Feliciano, E.; Filippini, J.; Fritts, M.; Gaitskell, R. J.; Golwala, S. R.; Grant, D. R.; Hall, J.; Hennings-Yeomans, R.; Hertel, S.; Holmgren, D.; Huber, M. E.; Mahapatra, R.; Mandic, V.; McCarthy, K. A.; Mirabolfathi, N.; Nelson, H.; Novak, L.; Ogburn, R. W.; Pyle, M.; Qiu, X.; Ramberg, E.; Rau, W.; Reisetter, A.; Saab, T.; Sadoulet, B.; Sander, J.; Schmitt, R.; Schnee, R. W.; Seitz, D. N.; Serfass, B.; Sirois, A.; Sundqvist, K. M.; Tarka, M.; Tomada, A.; Wang, G.; Yellin, S.; Yoo, J.; Young, B. A. Bibcode: 2009PhRvL.102a1301A Altcode: 2008arXiv0802.3530C We report results from the Cryogenic Dark Matter Search at the Soudan Underground Laboratory (CDMS II) featuring the full complement of 30 detectors. A blind analysis of data taken between October 2006 and July 2007 sets an upper limit on the weakly interacting massive particle (WIMP) nucleon spin-independent cross section of 6.6×10-44cm2 (4.6×10-44cm2 when combined with previous CDMS II data) at the 90% confidence level for a WIMP mass of 60GeV/c2. This achieves the best sensitivity for dark matter WIMPs with masses above 44GeV/c2, and significantly restricts the parameter space for some favored supersymmetric models. Title: Section on Prospects for Dark Matter Detection of the White Paper on the Status and Future of Ground-Based TeV Gamma-Ray Astronomy Authors: Buckley, J.; Baltz, E. A.; Bertone, G.; Byrum, K.; Fegan, S.; Ferrer, F.; Gondolo, P.; Hall, J.; Hooper, D.; Horan, D.; Koushiappas, S.; Krawczynski, H.; LeBohec, S.; Profumo, S.; Silk, J.; Tait, T.; Vassiliev, V.; Wagner, R.; Wakely, S.; Wood, M.; Zaharijas, G. Bibcode: 2008arXiv0812.0795B Altcode: This is a report on the findings of the dark matter science working group for the white paper on the status and future of TeV gamma-ray astronomy. The white paper was commissioned by the American Physical Society, and the full white paper can be found on astro-ph (arXiv:0810.0444). This detailed section discusses the prospects for dark matter detection with future gamma-ray experiments, and the complementarity of gamma-ray measurements with other indirect, direct or accelerator-based searches. We conclude that any comprehensive search for dark matter should include gamma-ray observations, both to identify the dark matter particle (through the charac- teristics of the gamma-ray spectrum) and to measure the distribution of dark matter in galactic halos. Title: A Venus Flagship Mission: Exploring a World of Contrasts Authors: Senske, D.; Bullock, M.; Balint, T.; Benz, A.; Campbell, B.; Chassefiere, E.; Colaprete, A.; Cutts, J.; Glaze, L.; Gorevan, S.; Grinspoon, D.; Hall, J.; Hasimoto, G.; Head, J.; Hunter, G.; Johnson, N.; Kiefer, W.; Kolawa, E.; Kremic, T.; Kwok, J.; Limaye, S.; Mackwell, S.; Marov, M.; Peterson, C.; Schubert, G.; Spilker, T.; Stofan, E.; Svedhem, H.; Titov, D.; Treiman, A. Bibcode: 2008AGUFM.P22A..08S Altcode: Results from past missions and the current Venus Express Mission show that Venus is a world of contrasts, providing clear science drivers for renewed exploration of this planet. In early 2008, NASA's Science Mission Directorate formed a Science and Technology Definition Team (STDT) to formulate science goals and objectives, mission architecture and a technology roadmap for a flagship class mission to Venus. This 3- to 4 billon mission, to launch in the post 2020 timeframe, should revolutionize our understanding of how climate works on terrestrial planets, including the close relationship between volcanism, tectonism, the interior, and the atmosphere. It would also more clearly elucidate the geologic history of Venus, including the existence and persistence of an ancient ocean. Achieving these objectives will provide a basis to understand the habitability of extra solar terrestrial planets. To address a broad range of science questions this mission will be composed of flight elements that include an orbiter that is highlighted by an interferometric SAR to provide surface topographic and image information at scales one to two orders of magnitude greater than that achieved by any previous spacecraft to Venus. Two balloons with a projected lifetime of weeks will probe the structure and dynamics of the atmosphere at an altitude of 50 to 70-km. In addition, two descent probes will collect data synergistic to that from the balloon and analyze the geochemistry of surface rocks over a period of hours. The technology road map focuses on key areas of science instruments and enabling engineering to provide greater in situ longevity in the hostile Venus environment. Title: Stellar Chromospheric Activity Authors: Hall, Jeffrey C. Bibcode: 2008LRSP....5....2H Altcode: The Sun, stars similar to it, and many rather dissimilar to it, have chromospheres, regions classically viewed as lying above the brilliant photosphere and characterized by a positive temperature gradient and a marked departure from radiative equilibrium. Stellar chromospheres exhibit a wide range of phenomena collectively called activity, stemming largely from the time evolution of their magnetic fields and the mass flux and transfer of radiation through the complex magnetic topology and the increasingly optically thin plasma of the outer stellar atmosphere. In this review, I will (1) outline the development of our understanding of chromospheric structure from 1960 to the present, (2) discuss the major observational programs and theoretical lines of inquiry, (3) review the origin and nature of both solar and stellar chromospheric activity and its relationship to, and effect on, stellar parameters including total energy output, and (4) summarize the outstanding problems today. Title: The X-ray cycle in the solar-type star HD 81809. XMM-Newton observations and implications for the coronal structure Authors: Favata, F.; Micela, G.; Orlando, S.; Schmitt, J. H. M. M.; Sciortino, S.; Hall, J. Bibcode: 2008A&A...490.1121F Altcode: 2008arXiv0806.2279F Context: The 11-yr cycle is the best known manifestation of the Sun's activity. While chromospheric cycles have been studied in a number of solar-like stars, very little is known about how these are reflected in the cyclical behavior of the coronal X-ray emission in stars other than the Sun.
Aims: Our long-term XMM-Newton program of long-term monitoring of a solar-like star with a well-studied chromospheric cycle, HD 81809, aims to study whether an X-ray cycle is present, along with studying its characteristics and its relation to the chromospheric cycle.
Methods: Regular observations of HD 81809 were performed with XMM-Newton, spaced by 6 months from 2001 to 2007. We studied the variations in the resulting coronal luminosity and temperature, and compared them with the chromospheric Ca ii variations. We also modeled the observations in terms of a mixture of active regions, using a methodology originally developed to study the solar corona.
Results: Our observations show a well-defined cycle with an amplitude exceeding 1 dex and an average luminosity approximately one order of magnitude higher than in the Sun. The behavior of the corona of HD 81809 can be modeled well in terms of varying coverage of solar-like active regions, with a larger coverage than for the Sun, showing it to be compatible with a simple extension of the solar case. Title: NASA's Venus Science and Technology Definition Team: A Flagship Mission to Venus Authors: Bullock, Mark Alan; Senske, D. A.; Balint, T. S.; Campbell, B. A.; Chassefiere, E.; Colaprete, A.; Cutts, J. A.; Glaze, L.; Gorevan, S.; Grinspoon, D. H.; Hall, J.; Hartford, W.; Hashimoto, G. L.; Head, J. W.; Hunter, G.; Johnson, N.; Kiefer, W. S.; Kolawa, E. A.; Kremic, T.; Kwok, J.; Limaye, S. S.; Mackwell, S. J.; Marov, M. Y.; Ocampo, A.; Schubert, G.; Stofan, E. R.; Svedhem, H.; Titov, D. V.; Treiman, A. H. Bibcode: 2008DPS....40.3208B Altcode: 2008BAAS...40R.452B The Venus Science and Technology Definition Team (STDT) was formed by NASA to look at science objectives, mission architecture, science investigations, and instrument payload for a Flagship-class mission to Venus. This $3-4B mission, to launch in the 2020-2025 timeframe, should revolutionize our understanding of how climate works on terrestrial planets, including the close relationship between volcanism, tectonism, the interior, and the atmosphere. It would also be capable of resolving the geologic history of Venus, including the existence and persistence of an ancient ocean. Achieving all these objectives will be necessary to understand the habitability of extrasolar terrestrial planets that should be detected in the next few years. The Venus STDT is comprised of scientists and engineers from the United States, the Russian Federation, France, Germany, the Netherlands, and Japan. The team began work in January 2008, gave an interim report at NASA headquarters in May, and will deliver a final report in December 2008. The Venus STDT will also produce a technology roadmap to identify crucial investments to meet the unique challenges of in situ Venus exploration.

We will discuss the mission architecture and payload that have been designed to address the science objectives, and the methods we used. Most of the science objectives in the latest VEXAG white paper can be addressed by a Venus Flagship mission, and equally importantly, NASA can fly a large mission to another Earth-sized planet with the explicit intention of better understanding our own. Title: A Search for Dark Matter Annihilation with the Whipple 10 m Telescope Authors: Wood, M.; Blaylock, G.; Bradbury, S. M.; Buckley, J. H.; Byrum, K. L.; Chow, Y. C. K.; Cui, W.; de la Calle Perez, I.; Falcone, A. D.; Fegan, S. J.; Finley, J. P.; Grube, J.; Hall, J.; Hanna, D.; Holder, J.; Horan, D.; Humensky, T. B.; Kieda, D. B.; Kildea, J.; Konopelko, A.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Nagai, T.; Ong, R. A.; Perkins, J. S.; Pohl, M.; Quinn, J.; Rose, H. J.; Sembroski, G. H.; Vassiliev, V. V.; Wagner, R. G.; Wakely, S. P.; Weekes, T. C.; Weinstein, A. Bibcode: 2008ApJ...678..594W Altcode: 2008arXiv0801.1708W We present observations of the dwarf galaxies Draco and Ursa Minor, the Local Group galaxies M32 and M33, and the globular cluster M15 conducted with the Whipple 10 m gamma-ray telescope to search for the gamma-ray signature of self-annihilating weakly interacting massive particles (WIMPs), which may constitute astrophysical dark matter (DM). We review the motivations for selecting these sources based on their unique astrophysical environments and report the results of the data analysis that produced upper limits on the excess rate of gamma rays for each source. We consider models for the DM distribution in each source based on the available observational constraints and discuss possible scenarios for the enhancement of the gamma-ray luminosity. Limits on the thermally averaged product of the total self-annihilation cross section and velocity of the WIMP, langleσυrangle , are derived using conservative estimates for the magnitude of the astrophysical contribution to the gamma-ray flux. Although these limits do not constrain predictions from the currently favored theoretical models of supersymmetry (SUSY), future observations with VERITAS will probe a larger region of the WIMP parameter phase space, langleσυrangle , and WIMP particle mass (mχ). Title: First observation of planet-induced X-ray emission: The system HD 179949 Authors: Saar, S. H.; Cuntz, M.; Kashyap, V. L.; Hall, J. C. Bibcode: 2008IAUS..249...79S Altcode: 2007IAUS..249...79S; 2007arXiv0712.3270S We present the first observation of planet-induced stellar X-ray activity, identified for the HD 179949 system, using Chandra / ACIS-S. The HD 179949 system consists of a close-in giant planet orbiting an F9 V star. Previous ground-based observations already showed enhancements in Ca II K in phase with the planetary orbit. We find an 30% increase in the X-ray flux over quiescent levels coincident with the phase of the Ca II enhancements. There is also a trend for the emission to be hotter at increased fluxes, confirmed by modeling, showing the enhancement at 1 keV compared to 0.4 keV for the background star. Title: First results from VERITAS Authors: Hanna, D.; Acciari, V. A.; Amini, R.; Badran, H. M.; Blaylock, G.; Bradbury, S. M.; Buckley, J. H.; Bugaev, V.; Butt, Y.; Byrum, K. L.; Celik, O.; Cesarini, A.; Ciupik, L.; Chow, Y. C. K.; Cogan, P.; Colin, P.; Cui, W.; Daniel, M. K.; Dowdall, C.; Dowkontt, P.; Duke, C.; Ergin, T.; Falcone, A. D.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortin, P.; Fortson, L. F.; Gall, D.; Gibbs, K.; Gillanders, G.; Glidewell, O. J.; Grube, J.; Guenette, R.; Gyuk, G.; Hall, J.; Hays, E.; Holder, J.; Horan, D.; Hughes, S. B.; Hui, C. M.; Humensky, T. B.; Imran, A.; Kaaret, P.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Konopelko, A.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Lebohec, S.; Lee, K.; Manseri, H.; McCann, A.; McCutcheon, M.; Millis, J.; Moriarty, P.; Mukherjee, R.; Nagai, T.; Niemiec, J.; Ogden, P. A.; Ong, R. A.; Pandel, D.; Perkins, J. S.; Pizlo, F.; Pohl, M.; Quinn, J.; Ragan, K.; Reynolds, P. T.; Roache, E.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Smith, A. W.; Steele, D.; Swordy, S. P.; Syson, A.; Toner, J. A.; Valcarcel, L.; Vassiliev, V. V.; Wagner, R.; Wakely, S. P.; Ward, J. E.; Weekes, T. C.; Weinstein, A.; White, R. J.; Williams, D. A.; Wissel, S. A.; Wood, M.; Zitzer, B. Bibcode: 2008NIMPA.588...26H Altcode: VERITAS is an array of four, 12-m-diameter, Cherenkov telescopes, designed to explore the very-high-energy gamma-ray sky in the energy band between 100 GeV and 50 TeV. Its construction and commissioning have occurred over the past two years and the array has been taking scientific data with three or more telescopes since November 2006. We present results from observations made with VERITAS during the past observing season, including new results on the distant blazar 1ES1218+304, the active galaxy M87 and the high-mass X-ray binary system LS I +61 303. We also describe the plans in place for the coming observing seasons. Title: VERITAS: Status and Latest Results Authors: Maier, G.; Acciari, V. A.; Amini, R.; Blaylock, G.; Bradbury, S. M.; Buckley, J. H.; Bugaev, V.; Butt, Y.; Byrum, K. L.; Celik, O.; Cesarini, A.; Ciupik, L.; Chow, Y. C. K.; Cogan, P.; Colin, P.; Cui, W.; Daniel, M. K.; Dowdall, C.; Dowkontt, P.; Duke, C.; Ergin, T.; Falcone, A. D.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fotin, P.; Fortson, L. F.; Gall, D.; Gibbs, K.; Gillanders, G.; Grube, J.; Guenette, R.; Gyuk, G.; Hall, J.; Hanna, D.; Hays, E.; Holder, J.; Horan, D.; Hughes, S. B.; Hui, C. M.; Humensky, T. B.; Imran, A.; Kaaret, P.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Konopelko, A.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Lee, K.; Manseri, H.; McCann, A.; McCutcheron, M.; Millis, J.; Moriarty, P.; Mukherjee, R.; Nagai T.; Niemiec, J.; Ogden, P. A.; Ong, R. A.; Pandel, D.; Perkins, J. S.; Pizlo, F.; Pohl, M.; Quinn, J.; Ragan, K.; Reynolds, P. T.; Roache, E.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Smith, A. W.; Steele, D.; Swordy, S. P.; Syson, A.; Toner, J. A.; Valcarcel, L.; Vassiliev, V. V.; Wagner, R.; Wakely, S. P.; Ward, J. E.; Weeks, T. C.; Weinstein, A.; White, R. J.; Williams, D. A.; Wissel, S. A.; Wood, M.; Zitzer, B. Bibcode: 2008ICRC....3.1457M Altcode: 2008ICRC...30c1457M; 2007arXiv0709.3654M VERITAS is an atmospheric Cherenkov telescope array designed to study astrophysical sources of very high energy gamma radiation. Located in southern Arizona, USA, the array consists of four 12-m diameter imaging Cherenkov telescopes. All four telescopes have been deployed at the basecamp of the Whipple Observatory and they became fully operational in early 2007. This paper describes the operational status of VERITAS, outlines the initial performance parameters of the instrument, and presents the latest results that have been obtained. Title: The Whipple Observatory 10 m gamma-ray telescope, 1997 2006 Authors: Kildea, J.; Atkins, R. W.; Badran, H. M.; Blaylock, G.; Bond, I. H.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D. A.; Celik, O.; Chow, Y. C. K.; Cui, W.; Cogan, P.; Daniel, M. K.; de la Calle Perez, I.; Dowdall, C.; Duke, C.; Falcone, A. D.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gall, D.; Gillanders, G. H.; Grube, J.; Gutierrez, K. J.; Hall, J.; Hall, T. A.; Holder, J.; Horan, D.; Hughes, S. B.; Jordan, M.; Jung, I.; Kenny, G. E.; Kertzman, M.; Knapp, J.; Konopelko, A.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Lloyd-Evans, J.; Millis, J.; Moriarty, P.; Nagai, T.; Ogden, P. A.; Ong, R. A.; Perkins, J. S.; Petry, D.; Pizlo, F.; Pohl, M.; Quinn, J.; Quinn, M.; Rebillot, P. F.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Smith, A. W.; Syson, A.; Toner, J. A.; Valcarcel, L.; Vassiliev, V. V.; Wakely, S. P.; Weekes, T. C.; White, R. J. Bibcode: 2007APh....28..182K Altcode: Details are presented of the Whipple Observatory's 10 m atmospheric Cherenkov telescope and camera, as it evolved during the period 1997 until 2006. The design of the telescope and camera's optical and electronic systems is discussed together with a detailed description of the four-stage GRANITE (Gamma-RAy New Imaging TElescope) upgrade program, undertaken during the same time period. The objective of the upgrade was to improve the telescope's sensitivity for the detection of very-high-energy gamma-rays. Results from the program are provided and are briefly discussed in the context of the design of VERITAS. Title: Development of bubble chambers with enhanced stability and sensitivity to low-energy nuclear recoils Authors: Bolte, W. J.; Collar, J. I.; Crisler, M.; Hall, J.; Holmgren, D.; Nakazawa, D.; Odom, B.; O'Sullivan, K.; Plunkett, R.; Ramberg, E.; Raskin, A.; Sonnenschein, A.; Vieira, J. D. Bibcode: 2007NIMPA.577..569B Altcode: 2005astro.ph..3398B The viability of using Bubble Chambers as dark matter particle detectors is considered. Techniques leading to the enhanced chamber stability needed for this new application are described in detail. Prototype trials show that sensitivity to the low-energy nuclear recoils induced by Weakly Interacting Massive Particles (WIMP) is possible in conditions of extreme insensitivity to minimum ionizing backgrounds. An understanding of detector response is demonstrated using existing theoretical models. We briefly comment on the prospects for detection of supersymmetric dark matter with large CF3I chambers. Title: The Sun-like Activity of the Solar Twin 18 Scorpii Authors: Hall, Jeffrey C.; Henry, Gregory W.; Lockwood, G. Wesley Bibcode: 2007AJ....133.2206H Altcode: 2007astro.ph..3450H We present the results of 10 yr of complementary spectroscopic and photometric observations of the solar twin 18 Scorpii. We show that over the course of its ~7 yr chromospheric activity cycle, 18 Sco's brightness varies in the same manner as the Sun's and with a likely total brightness variation of 0.09%, similar to the 0.1% decadal variation in the total solar irradiance. Title: Observations of the Unidentified TeV γ-Ray Source TeV J2032+4130 with the Whipple Observatory 10 m Telescope Authors: Konopelko, A.; Atkins, R. W.; Blaylock, G.; Buckley, J. H.; Butt, Y.; Carter-Lewis, D. A.; Celik, O.; Cogan, P.; Chow, Y. C. K.; Cui, W.; Dowdall, C.; Ergin, T.; Falcone, A. D.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortin, P.; Gillanders, G. H.; Gutierrez, K. J.; Hall, J.; Hanna, D.; Horan, D.; Hughes, S. B.; Humensky, T. B.; Imran, A.; Jung, I.; Kaaret, P.; Kenny, G. E.; Kertzman, M.; Kieda, D. B.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Moriarty, P.; Mukherjee, R.; Nagai, T.; Ong, R. A.; Perkins, J. S.; Pohl, M.; Ragan, K.; Reynolds, P. T.; Rose, H. J.; Sembroski, G. H.; Schrödter, M.; Smith, A. W.; Steele, D.; Syson, A.; Swordy, S. P.; Toner, J. A.; Valcarcel, L.; Vassiliev, V. V.; Wagner, R. G.; Wakely, S. P.; Weekes, T. C.; White, R. J.; Williams, D. A.; Zitzer, B.; VERITAS Collaboration Bibcode: 2007ApJ...658.1062K Altcode: 2006astro.ph.11730K We report on observations of the sky region around the unidentified TeV γ-ray source (TeV J2032+4130) carried out with the Whipple Observatory 10 m atmospheric Cerenkov telescope for a total of 65.5 hr between 2003 and 2005. The standard two-dimensional analysis developed by the Whipple collaboration for a stand-alone telescope reveals an excess in the field of view at a pretrial significance level of 6.1 σ. The measured position of this excess is α=20h32m27s, δ=41deg39'17'' (J2000.0). The estimated integral flux for this γ-ray source is about 8% of the Crab Nebula flux. The data are consistent with a pointlike source. Here we present a detailed description of the standard two-dimensional analysis technique used for the analysis of data taken with the Whipple Observatory 10 m telescope and the results for the TeV J2032+4130 campaign. We include a short discussion of the physical mechanisms that may be responsible for the observed γ-ray emission, based on possible association with known astrophysical objects, in particular, Cygnus OB2. Title: The Activity and Variability of the Sun and Sun-like Stars. I. Synoptic Ca II H and K Observations Authors: Hall, Jeffrey C.; Lockwood, G. W.; Skiff, Brian A. Bibcode: 2007AJ....133..862H Altcode: Synoptic measurements of activity in Sun-like stars have been performed continuously since 1966, and the largest set comes from the Mount Wilson HK project, in the form of the well-known S index. We have been monitoring the activity and variability of the Sun and a large sample of Sun-like stars, in terms of S and absolute flux, since 1994 with the Solar-Stellar Spectrograph (SSS) at Lowell Observatory. Directly inspired by the similar long-term program at Mount Wilson Observatory, the SSS incorporates both an HK spectrograph and an echelle for visible and far-red observations. This is the first of three papers presenting the results of some 20,000 observations of the Sun and Sun-like stars with the SSS. In this paper we describe our program, review the calibration of solar and stellar fluxes to S and the chromospheric emission fraction R'HK, compare our derived stellar activity measures to those from other programs, and discuss the broad characteristics of the activity and variability in our target set, with particular attention to good solar analogs and noncycling stars. In subsequent papers we will discuss the echelle data and present detailed examinations of stars of particular interest. Title: Very High Energy Observations of Gamma-Ray Burst Locations with the Whipple Telescope Authors: Horan, D.; Atkins, R. W.; Badran, H. M.; Blaylock, G.; Bradbury, S. M.; Buckley, J. H.; Byrum, K. L.; Celik, O.; Chow, Y. C. K.; Cogan, P.; Cui, W.; Daniel, M. K.; de la Calle Perez, I.; Dowdall, C.; Falcone, A. D.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortin, P.; Fortson, L. F.; Gillanders, G. H.; Grube, J.; Gutierrez, K. J.; Hall, J.; Hanna, D.; Holder, J.; Hughes, S. B.; Humensky, T. B.; Kenny, G. E.; Kertzman, M.; Kieda, D. B.; Kildea, J.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Maier, G.; Moriarty, P.; Nagai, T.; Ong, R. A.; Perkins, J. S.; Petry, D.; Quinn, J.; Quinn, M.; Ragan, K.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Steele, D.; Swordy, S. P.; Toner, J. A.; Valcarcel, L.; Vassiliev, V. V.; Wagner, R. G.; Wakely, S. P.; Weekes, T. C.; White, R. J.; Williams, D. A. Bibcode: 2007ApJ...655..396H Altcode: 2007astro.ph..1281H Gamma-ray burst (GRB) observations at very high energies (VHE; E>100 GeV) can impose tight constraints on some GRB emission models. Many GRB afterglow models predict a VHE component similar to that seen in blazars and plerions, in which the GRB spectral energy distribution has a double-peaked shape extending into the VHE regime. VHE emission coincident with delayed X-ray flare emission has also been predicted. GRB follow-up observations have had high priority in the observing program at the Whipple 10 m gamma-ray telescope, and GRBs will continue to be high-priority targets as the next-generation observatory, VERITAS, comes online. Upper limits on the VHE emission at late times (>~4 hr) from seven GRBs observed with the Whipple Telescope are reported here. Title: Time Series Observations of UX Ursae Majoris Authors: Alexander, W. R.; Hall, J.; Nelson, T.; Miller, D. Bibcode: 2006JAVSO..34..276A Altcode: No abstract at ADS Title: Coronal activity cycles in 61 Cygni Authors: Hempelmann, A.; Robrade, J.; Schmitt, J. H. M. M.; Favata, F.; Baliunas, S. L.; Hall, J. C. Bibcode: 2006A&A...460..261H Altcode: Context: .While the existence of stellar analogues of the 11 years solar activity cycle is proven for dozens of stars from optical observations of chromospheric activity, the observation of clearly cyclical coronal activity is still in its infancy.
Aims: .In this paper, long-term X-ray monitoring of the binary 61 Cygni is used to investigate possible coronal activity cycles in moderately active stars.
Methods: .We are monitoring both stellar components, a K5V (A) and a K7V (B) star, of 61 Cyg with XMM-Newton. The first four years of these observations are combined with ROSAT HRI observations of an earlier monitoring campaign. The X-ray light curves are compared with the long-term monitoring of chromospheric activity, as measured by the Mt.Wilson CaII H+K S-index.
Results: .Besides the observation of variability on short time scales, long-term variations of the X-ray activity are clearly present. For 61 Cyg A we find a coronal cycle which clearly reflects the well-known and distinct chromospheric activity cycle. The changes of coronal properties during the cycle resemble the solar behaviour. The coronal activity of 61 Cyg B also follows the chromospheric variability, although a pronounced sinusoidal chromospheric cycle of large amplitude is not noticeable. This is also reflected in the XMM-Newton observations with a rather complex long-term variability during that time.
Conclusions: .61 Cyg A is the first star where a persistent coronal activity cycle has been observed. Title: Time Series Observations of UX Ursae Majoris. Authors: Alexander, W. R.; Hall, J.; Nelson, T.; Miller, D. Bibcode: 2006JAVSO..34R.276A Altcode: No abstract at ADS Title: A Survey of Chromospheric Activity in the Solar-Type Stars in the Open Cluster M67 Authors: Giampapa, Mark S.; Hall, Jeffrey C.; Radick, Richard R.; Baliunas, Sallie L. Bibcode: 2006ApJ...651..444G Altcode: 2006astro.ph..7313G We present the results of a spectroscopic survey of the Ca II H and K core strengths in a sample of 60 solar-type stars that are members of the solar-age and solar-metallicity open cluster M67. We adopt the HK index, defined as the summed H+K core strengths in 1 Å bandpasses centered on the H and K lines, respectively, as a measure of the chromospheric activity that is present. We compare the distribution of mean HK index values for the M67 solar-type stars with the variation of this index as measured for the Sun during the contemporary solar cycle. We find that the stellar distribution in our HK index is broader than that for the solar cycle. Approximately 17% of the M67 Sun-like stars exhibit average HK indices that are less than solar minimum. About 7%-12% are characterized by relatively high activity in excess of solar maximum values, while 72%-80% of the solar analogs exhibit Ca II H+K strengths within the range of the modern solar cycle. The ranges given reflect uncertainties in the most representative value of the maximum in the HK index to adopt for the solar cycle variations observed during the period AD 1976-2004. Thus, ~20%-30% of our homogeneous sample of Sun-like stars have mean chromospheric H+K strengths that are outside the range of the contemporary solar cycle. Any cycle-like variability that is present in the M67 solar-type stars appears to be characterized by periods greater than ~6 yr. Finally, we estimate a mean chromospheric age for M67 in the range of 3.8-4.3 Gyr.

The results presented herein are based on data obtained at the WIYN telescope and at the McMath-Pierce Solar Telescope. The WIYN Observatory is a joint facility of the University of Wisconsin-Madison, Indiana University, Yale University, and the National Optical Astronomy Observatory. The McMath-Pierce Solar Telescope Facility is operated by the National Solar Observatory for the National Science Foundation. This paper is WIYN Open Cluster Study XXVIII in the series. Title: Deployment of the VERITAS observatory Authors: LeBohec, S.; Atkins, R. W.; Badran, H. M.; Blaylock, G.; Bond, I. H.; Boyle, P. J.; Bradbury, Sm; Buckley, J. H.; Carter-Lewis, Da; Celik, O.; Chow, Y. C. K.; Cogan, P.; P, W. Cu; Daniel, M. K.; de la Calle Perez, I.; Dowdall; Dowkontt, P.; Duke, C.; Ergin, T.; Falcone, A. D.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortin, P.; Fortson, L.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hanna, D.; Hays, E.; Holder, J.; Horana, D.; Hughes, S. B.; Humensky, T. B.; Kaaret, P.; Kenny, G. E.; Kertzmann, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Linton, E.; Lloyd-Evans, J.; Maier, G.; Manseri, H.; Milovanovic, A.; Moriarty, P.; Mukherjee, R.; Nagai, T. N.; Ogden, P. A.; Olevitch, M.; Ong, R. A.; Perkins, J. S.; Petry, D.; Pizlo, F.; Pohl, M.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Reynolds, P. T.; Rebillot, P.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Steele, D.; Swordy, S. P.; Syson, A.; Valcarcel, L.; Vassiliev, V. V.; Wagner, R. G.; Wakely, S. P.; Walker, G.; Weekes, T. C.; White, R. J.; Williams, D. A.; Zweerink, J. Bibcode: 2006JPhCS..47..232L Altcode: The Very Energetic Radiation Imaging Telescope Array System (VERITAS) being constructed in Southern Arizona consists of an array of four Atmospheric Cherenkov 12m Telescopes designed to observe astrophysical gamma rays in the energy range from 100 GeV to tens of TeV. A first telescope has been in operation on a temporary site since the end of 2004 and meets all specifications. The second is being installed on the same site, 85m from the first, in order to test stereoscopic capabilities. The full system of four telescopes is expected to be installed on the definitive site by the end of 2006. Title: VERITAS: status c.2005 Authors: Weekes, T. C.; Atkins, R. W.; Badran, H. M.; Blaylock, G.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Bryum, K. L.; Carter-Lewis, D. A.; Celik, O.; Chow, Y. C. K.; Cogan, P.; Cui, W.; Daniel, M. K.; de La Calle Perez, I.; Dowdall, C.; Dowkontt, P.; Duke, C.; Ergin, T.; Falcone, A. D.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortin, P.; Fortson, L.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Guitterez, K. J.; Hall, J.; Hall, T. A.; Hanna, D.; Hays, E.; Hillas, A. M.; Holder, J.; Horan, D.; Hughes, S. B.; Humensky, T. B.; Kaaret, P.; Kenny, G. E.; Kertzmann, M.; Kiedai, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Lebohec, S.; Linton, E.; Lloyd-Evans, J.; Maier, G.; Manseri, H.; Milovanovic, A.; Moriarty, P.; Mukherjee, R.; Nagai, T. N.; Ogden, P. A.; Olevitch, M.; Ong, R. A.; Perkins, J. S.; Petry, D.; Pizlo, F.; Pohl, M.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Reynolds, P. T.; Rebillot, P.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Steele, D.; Swordy, S. P.; Syson, A.; Toner, J.; Valcarcel, L.; Vassiliev, V. V.; Wagner, R. G.; Wakely, S. P.; Walker, G.; White, R. J.; Williams, D. A.; VERITAS Collaboration Bibcode: 2006AIPC..842.1001W Altcode: VERITAS (Very Energetic Radiation Imaging Telescope Array System), is one of a new generation of TeV gamma-ray observatories. The current status of its construction is described here. The first two telescopes and cameras have been completed and meet the design specifications; the full array of four telescopes could be operational by the end of 2006. Title: The first VERITAS telescope Authors: Holder, J.; Atkins, R. W.; Badran, H. M.; Blaylock, G.; Bradbury, S. M.; Buckley, J. H.; Byrum, K. L.; Carter-Lewis, D. A.; Celik, O.; Chow, Y. C. K.; Cogan, P.; Cui, W.; Daniel, M. K.; de la Calle Perez, I.; Dowdall, C.; Dowkontt, P.; Duke, C.; Falcone, A. D.; Fegan, S. J.; Finley, J. P.; Fortin, P.; Fortson, L. F.; Gibbs, K.; Gillanders, G.; Glidewell, O. J.; Grube, J.; Gutierrez, K. J.; Gyuk, G.; Hall, J.; Hanna, D.; Hays, E.; Horan, D.; Hughes, S. B.; Humensky, T. B.; Imran, A.; Jung, I.; Kaaret, P.; Kenny, G. E.; Kieda, D.; Kildea, J.; Knapp, J.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.; Little, E. K.; Maier, G.; Manseri, H.; Milovanovic, A.; Moriarty, P.; Mukherjee, R.; Ogden, P. A.; Ong, R. A.; Petry, D.; Perkins, J. S.; Pizlo, F.; Pohl, M.; Quinn, J.; Ragan, K.; Reynolds, P. T.; Roache, E. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Sleege, G.; Steele, D.; Swordy, S. P.; Syson, A.; Toner, J. A.; Valcarcel, L.; Vassiliev, V. V.; Wakely, S. P.; Weekes, T. C.; White, R. J.; Williams, D. A.; Wagner, R. Bibcode: 2006APh....25..391H Altcode: 2006astro.ph..4119H The first atmospheric Cherenkov telescope of VERITAS (the Very Energetic Radiation Imaging Telescope Array System) has been in operation since February 2005. We present here a technical description of the instrument and a summary of its performance. The calibration methods are described, along with the results of Monte Carlo simulations of the telescope and comparisons between real and simulated data. The analysis of TeV γ-ray observations of the Crab Nebula, including the reconstructed energy spectrum, is shown to give results consistent with earlier measurements. The telescope is operating as expected and has met or exceeded all design specifications. Title: TeV Gamma-Ray Observations of the Perseus and Abell 2029 Galaxy Clusters Authors: Perkins, J. S.; Badran, H. M.; Blaylock, G.; Bradbury, S. M.; Cogan, P.; Chow, Y. C. K.; Cui, W.; Daniel, M. K.; Falcone, A. D.; Fegan, S. J.; Finley, J. P.; Fortin, P.; Fortson, L. F.; Gillanders, G. H.; Gutierrez, K. J.; Grube, J.; Hall, J.; Hanna, D.; Holder, J.; Horan, D.; Hughes, S. B.; Humensky, T. B.; Kenny, G. E.; Kertzman, M.; Kieda, D. B.; Kildea, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Maier, G.; Moriarty, P.; Ong, R. A.; Pohl, M.; Ragan, K.; Rebillot, P. F.; Sembroski, G. H.; Steele, D.; Swordy, S. P.; Valcarcel, L.; Vassiliev, V. V.; Wakely, S. P.; Weekes, T. C.; Williams, D. A.; VERITAS Collaboration Bibcode: 2006ApJ...644..148P Altcode: 2006astro.ph..2258P Galaxy clusters might be sources of TeV gamma rays emitted by high-energy protons and electrons accelerated by large-scale structure formation shocks, galactic winds, or active galactic nuclei. Furthermore, gamma rays may be produced in dark matter particle annihilation processes at the cluster cores. We report on observations of the galaxy clusters Perseus and A2029 using the 10 m Whipple Cerenkov telescope during the 2003-2004 and 2004-2005 observing seasons. We apply a two-dimensional analysis technique to scrutinize the clusters for TeV emission. In this paper we first determine flux upper limits on TeV gamma-ray emission from point sources within the clusters. Second, we derive upper limits on the extended cluster emission. We subsequently compare the flux upper limits with EGRET upper limits at 100 MeV and theoretical models. Assuming that the gamma-ray surface brightness profile mimics that of the thermal X-ray emission and that the spectrum of cluster cosmic rays extends all the way from thermal energies to multi-TeV energies with a differential spectral index of -2.1, our results imply that the cosmic-ray proton energy density is less than 7.9% of the thermal energy density for the Perseus Cluster. Title: Science Autonomy on a Titan Airborne Platform Authors: Lorenz, R. D.; Zimmerman, W.; Lunine, J. I.; Reh, K.; Elliott, J.; Spilker, T.; Hall, J.; Jones, J.; Team, T. Bibcode: 2006AGUSMIN43E..07L Altcode: A prominent concept for future Titan exploration is an airship or altitude-controlled balloon which could drift or be driven slowly across Titan's varied, Earth-like landscape. Science goals that such a mission could address include high- resolution imaging for geomorphology and meteorology, subsurface sounding by radar, and in-situ sampling of surface material for analysis of organic composition. On-board science autonomy has an important role to play in such a mission. One factor is the 1.25hr one-way light time which drives latency in ground control intervention during critical events like surface sampling. A second issue is that while formidable data returns are possible via a robust combination of direct to earth (DTE - a few kbps, possibly continuously) and orbiter relay (intermittent windows of some tens of minutes permitting Gbits per day), the instruments on the platform are able to generate far larger data volumes. On-board autonomy will therefore add science value by generating more compact data products and prioritizing data for downlink. Autonomous science product generation might include selective highlighting of in-situ sampling data, generation of mosaic maps, digital elevation models and trajectory reconstruction from image data (rather than telemetering all individual images), landscape classification (dunes, river networks, etc.), and two-dimensional subsurface profiles generated by stacking individual sounder echoes. This presentation will summarize present thinking on a future Titan airborne mission and the role of autonomy. Title: A new search for primordial black hole evaporations using the Whipple gamma-ray telescope Authors: Linton, E. T.; Atkins, R. W.; Badran, H. M.; Blaylock, G.; Boyle, P. J.; Buckley, J. H.; Byrum, K. L.; Carter-Lewis, D. A.; Celik, O.; Chow, Y. C. K.; Cogan, P.; Daniel, M. K.; Dowdall, C.; Falcone, A. D.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortin, P.; Guiterrez, K. J.; Hall, J.; Hanna, D.; Holder, J.; Horan, D.; Hughes, S. B.; Humensky, T. B.; Jung, I.; Kenny, G. E.; Kertzman, M.; Kieda, D. B.; Kildea, J.; Knapp, J.; Krawczynski, H.; Lang, M. J.; LeBohec, S.; Maier, G.; Moriarty, P.; Ong, R. A.; Perkins, J. S.; Pizlo, F.; Pohl, M.; Quinn, J.; Ragan, K.; Rebillot, P. F.; Reynolds, P. T.; Sembroski, G. H.; Steele, D.; Swordy, S. P.; Valcarcel, L.; Wakely, S. P.; Weekes, T. C.; White, R. J. Bibcode: 2006JCAP...01..013L Altcode: Stephen Hawking's prediction that black holes should radiate like black bodies has several important consequences, including the possibility of the detection of small (~1015 g) black holes created in the very early universe. The detection of such primordial black holes (PBHs) would be an important discovery, not only confirming Hawking's theory, but also providing valuable insights into the history of the early universe. A search through 5.5 years of archival data from the Whipple Atmospheric Cerenkov Telescope is made for TeV gamma-ray bursts on 1, 3, and 5 s timescales. On the basis of a null result from this direct search for PBH evaporations, an upper limit of 1.08 × 106 pc-3 yr-1 (99% CL) is set on the PBH evaporation rate in the local region of the galaxy, assuming the Standard Model of particle physics. This is more than a factor of two better than the previous limit at this energy range and includes longer timescales than have previously been explored. Comparison of this result with previous limits on the fraction of the critical density comprised by PBHs, Ωpbh, depends strongly on assumptions made about PBH clustering; in models predicting strong PBH clustering, the limit in this work could be as many as ten orders of magnitude more stringently than those set by diffuse MeV gamma-ray observations. Title: Experimental results for Titan aerobot thermo-mechanical subsystem development Authors: Hall, J.; Jones, J.; Kerzhanovich, V.; Lachenmeier, T.; Mahr, P.; Pauken, M.; Plett, G.; Smith, L.; van Luvender, M.; Yavrouian, A. Bibcode: 2006cosp...36..280H Altcode: 2006cosp.meet..280H This paper describes experimental results from a development program focused in maturing Titan aerobot technology in the areas of mechanical and thermal subsystems Results from four key activities are described first a cryogenic balloon materials development program involving coupon and cylinder tests and culminating in the fabrication and subsequent testing of an inflated 4 6 m long prototype blimp at 93 K second a combined lab experiment and numerical simulation effort to assess potential problems resulting from radioisotope thermal generator waste heat generation near an inflated blimp third an aerial deployment and inflation development program consisting of laboratory and helicopter drop tests on a near full scale 11 m long prototype blimp and fourth a proof of concept experiment demonstrating the viability of using a mechanically steerable high gain antenna on a floating blimp to perform direct to Earth telecommunications from Titan The paper provides details on all of these successful activities and discusses their impact on the overall effort to produce mature systems technology for future Titan aerobot missions Title: Prototype design and testing of a Venus long duration, high altitude balloon Authors: Hall, J.; Fairbrother, D.; Frederickson, T.; Kerzhanovich, V.; Said, M.; Sandy, C.; Willey, C.; Yavrouian, A. Bibcode: 2006cosp...36..281H Altcode: 2006cosp.meet..281H This paper describes the design fabrication and testing of a full scale prototype balloon intended for long duration flight in the upper atmosphere of Venus The balloon is 5 5 meters in diameter and is designed to carry a 45 kg payload at an altitude of 55 km The balloon material is a 180 g m 2 multi-component laminate comprised of the following layers bonded together from outside to inside aluminized Teflon film aluminized Mylar film Vectran fabric and a polyurethane coating This construction provides the required balloon functional characteristics of low gas permeability sulfuric acid resistance and high strength for superpressure operation The design burst superpressure is 35 000 Pa which is predicted to be twice the worst case value expected during flight at the highest solar irradiance in the mission profile The prototype is constructed from 16 gores with bi-taped seams employing a sulfuric acid resistant adhesive on the outside Material coupon tests were performed to evaluate the optical and mechanical characteristics of the laminate These were followed by full prototype tests for inflation leakage and sulfuric acid tolerance The results confirmed the suitability of this balloon design for use at Venus in a long duration mission The various data are presented and the implications for mission design and operation are discussed Title: Electron energy spectra, fluxes, and day-night asymmetries of 8B solar neutrinos from measurements with NaCl dissolved in the heavy-water detector at the Sudbury Neutrino Observatory Authors: Aharmim, B.; Ahmed, S. N.; Anthony, A. E.; Beier, E. W.; Bellerive, A.; Bergevin, M.; Biller, S. D.; Boger, J.; Boulay, M. G.; Bowler, M. G.; Bullard, T. V.; Chan, Y. D.; Chen, M.; Chen, X.; Cleveland, B. T.; Cox, G. A.; Currat, C. A.; Dai, X.; Dalnoki-Veress, F.; Deng, H.; Doe, P. J.; Dosanjh, R. S.; Doucas, G.; Duba, C. A.; Duncan, F. A.; Dunford, M.; Dunmore, J. A.; Earle, E. D.; Elliott, S. R.; Evans, H. C.; Ewan, G. T.; Farine, J.; Fergani, H.; Fleurot, F.; Formaggio, J. A.; Frame, K.; Frati, W.; Fulsom, B. G.; Gagnon, N.; Graham, K.; Grant, D. R.; Hahn, R. L.; Hall, J. C.; Hallin, A. L.; Hallman, E. D.; Handler, W. B.; Hargrove, C. K.; Harvey, P. J.; Hazama, R.; Heeger, K. M.; Heelan, L.; Heintzelman, W. J.; Heise, J.; Helmer, R. L.; Hemingway, R. J.; Hime, A.; Howard, C.; Howe, M. A.; Huang, M.; Jagam, P.; Jelley, N. A.; Klein, J. R.; Kormos, L. L.; Kos, M. S.; Krüger, A.; Kraus, C.; Krauss, C. B.; Krumins, A. V.; Kutter, T.; Kyba, C. C.; Labranche, H.; Lange, R.; Law, J.; Lawson, I. T.; Lesko, K. T.; Leslie, J. R.; Levine, I.; Loach, J. C.; Luoma, S.; MacLellan, R.; Majerus, S.; Mak, H. B.; Maneira, J.; Marino, A. D.; McCauley, N.; McDonald, A. B.; McGee, S.; McGregor, G.; Mifflin, C.; Miknaitis, K. K.; Moffat, B. A.; Nally, C. W.; Neubauer, M. S.; Nickel, B. G.; Noble, A. J.; Norman, E. B.; Oblath, N. S.; Okada, C. E.; Ollerhead, R. W.; Orrell, J. L.; Oser, S. M.; Ouellet, C.; Peeters, S. J.; Poon, A. W.; Rielage, K.; Robertson, B. C.; Robertson, R. G.; Rollin, E.; Rosendahl, S. S.; Rusu, V. L.; Schwendener, M. H.; Seibert, S. R.; Simard, O.; Simpson, J. J.; Sims, C. J.; Sinclair, D.; Skensved, P.; Smith, M. W.; Starinsky, N.; Stokstad, R. G.; Stonehill, L. C.; Tafirout, R.; Takeuchi, Y.; Tešić, G.; Thomson, M.; Thorman, M.; Tsui, T.; van Berg, R.; Water, R. G.; Virtue, C. J.; Wall, B. L.; Waller, D.; Waltham, C. E.; Tseung, H. Wan; Wark, D. L.; Wendland, J.; West, N.; Wilkerson, J. F.; Wilson, J. R.; Wittich, P.; Wouters, J. M.; Wright, A.; Yeh, M.; Zuber, K. Bibcode: 2005PhRvC..72e5502A Altcode: 2005nucl.ex...2021S Results are reported from the complete salt phase of the Sudbury Neutrino Observatory experiment in which NaCl was dissolved in the 2H2O (“D2O”) target. The addition of salt enhanced the signal from neutron capture as compared to the pure D2O detector. By making a statistical separation of charged-current events from other types based on event-isotropy criteria, the effective electron recoil energy spectrum has been extracted. In units of 106cm-2s-1, the total flux of active-flavor neutrinos from 8B decay in the Sun is found to be 4.94+0.21-0.21(stat)+0.38-0.34(syst) and the integral flux of electron neutrinos for an undistorted 8B spectrum is 1.68+0.06-0.06(stat)+0.08-0.09(syst); the signal from (νx,e) elastic scattering is equivalent to an electron-neutrino flux of 2.35+0.22-0.22(stat)+0.15-0.15(syst). These results are consistent with those expected for neutrino oscillations with the so-called large mixing angle parameters and also with an undistorted spectrum. A search for matter-enhancement effects in the Earth through a possible day-night asymmetry in the charged-current integral rate is consistent with no asymmetry. Including results from other experiments, the best-fit values for two-neutrino mixing parameters are Δm2=(8.0+0.6-0.4)×10-5 eV2 and θ=33.9+2.4-2.2 degrees. Title: A Multiwavelength View of the TeV Blazar Markarian 421: Correlated Variability, Flaring, and Spectral Evolution Authors: Błażejowski, M.; Blaylock, G.; Bond, I. H.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D. A.; Celik, O.; Cogan, P.; Cui, W.; Daniel, M.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L.; Gammell, S.; Gibbs, K.; Gillanders, G. G.; Grube, J.; Gutierrez, K.; Hall, J.; Hanna, D.; Holder, J.; Horan, D.; Humensky, B.; Kenny, G.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Maier, G.; Mendoza, D.; Milovanovic, A.; Moriarty, P.; Nagai, T. N.; Ong, R. A.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Reynolds, P. T.; Rebillot, P.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Valcarel, L.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; White, R.; Zweerink, J.; VERITAS Collaboration; Mochejska, B.; Smith, B.; Aller, M.; Aller, H.; Teräsranta, H.; Boltwood, P.; Sadun, A.; Stanek, K.; Adams, E.; Foster, J.; Hartman, J.; Lai, K.; Böttcher, M.; Reimer, A.; Jung, I. Bibcode: 2005ApJ...630..130B Altcode: 2005astro.ph..5325B We report results from an intensive multiwavelength monitoring campaign on the TeV blazar Mrk 421 over the period of 2003-2004. The source was observed simultaneously at TeV energies with the Whipple 10 m telescope and at X-ray energies with the Rossi X-Ray Timing Explorer (RXTE) during each clear night within the Whipple observing windows. Supporting observations were also frequently carried out at optical and radio wavelengths to provide simultaneous or contemporaneous coverages. The large amount of simultaneous data has allowed us to examine the variability of Mrk 421 in detail, including cross-band correlation and broadband spectral variability, over a wide range of flux. The variabilities are generally correlated between the X-ray and gamma-ray bands, although the correlation appears to be fairly loose. The light curves show the presence of flares with varying amplitudes on a wide range of timescales at both X-ray and TeV energies. Of particular interest is the presence of TeV flares that have no coincident counterparts at longer wavelengths, because the phenomenon seems difficult to understand in the context of the proposed emission models for TeV blazars. We have also found that the TeV flux reached its peak days before the X-ray flux did during a giant flare (or outburst) in 2004 (with the peak flux reaching ~135 mcrab in X-rays, as seen by the RXTE ASM, and ~3 crab in gamma rays). Such a difference in the development of the flare presents a further challenge to both the leptonic and hadronic emission models. Mrk 421 varied much less at optical and radio wavelengths. Surprisingly, the normalized variability amplitude in the optical seems to be comparable to that in the radio, perhaps suggesting the presence of different populations of emitting electrons in the jet. The spectral energy distribution of Mrk 421 is seen to vary with flux, with the two characteristic peaks moving toward higher energies at higher fluxes. We have failed to fit the measured spectral energy distributions (SEDs) with a one-zone synchrotron self-Compton model; introducing additional zones greatly improves the fits. We have derived constraints on the physical properties of the X-ray/gamma-ray flaring regions from the observed variability (and SED) of the source. The implications of the results are discussed. Title: Autonomous Flight Control for a Titan Exploration Aerobot Authors: Elfes, A.; Montgomery, J.; Hall, J.; Joshi, S.; Hall, J.; Payne, J.; Bergh, C. Bibcode: 2005ESASP.603E..91E Altcode: 2005aira.confE..91E No abstract at ADS Title: Development of bubble chambers with sensitivity to WIMPs Authors: Bond, L.; Collar, J. I.; Ely, J.; Flake, M.; Hall, J.; Jordan, D.; Nakazawa, D.; Raskin, A.; Sonnenschein, A.; Sullivan, K. O. Bibcode: 2005NewAR..49..271B Altcode: Bubble nucleation in moderately superheated liquids can be triggered by nuclear recoils from WIMPs. This phenomenon is the basis for superheated droplet detectors. The droplet technique is currently limited by insensitivity to spin-independent interactions, due to lack of heavy elements in the usual target liquids, and sensitivity to contamination of the gel by alpha emitters. As an alternative, we have developed a new type of homogeneous bubble chamber, which can contain heavy liquids, including CF 3Br, CF 3I, and C 3F 8. Detectors of this type may be scalable to large size at modest cost and could have very low backgrounds. We discuss results obtained with a 12 ml prototype and plans for a 1 liter chamber. Title: Indirect Observations of the Dark Matter at TeV Gamma-Ray Energies Authors: Hall, J. Bibcode: 2005AAS...206.2105H Altcode: 2005BAAS...37..462H Non-baryonic dark matter (DM) could emit gamma rays if the DM consists of weakly interacting massive particles (WIMPs). Particle theories for WIMPs suggest that they could annihilate producing gamma rays as a final product. The Galactic Center dynamics observed in the IR seems to be driven by three million solar masses within 90 AU of the dynamical center of the Milky Way. TeV gamma rays were detected in the same direction. We discuss the possibility that the TeV radiation from the GC results from annihilating WIMPs using a neutralino as our particle model. We use the IR observations to constrain the dark matter density profile. Other DM dominated systems such as dwarf galaxies are also promising for indirect detection of the DM. We discuss an ongoing program to observe DM dominated systems at TeV energies. Title: A Survey of Unidentified EGRET Sources at Very High Energies Authors: Fegan, S. J.; Badran, H. M.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D. A.; Catanese, M.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J. A.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Le Bohec, S.; Lessard, R. W.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; McEnery, J.; Moriarty, P.; Mukherjee, R.; Muller, D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2005ApJ...624..638F Altcode: The Whipple Observatory 10 m γ-ray telescope has been used to survey the error boxes of EGRET unidentified sources in an attempt to find counterparts at energies of 350 GeV and above. Twenty-one unidentified sources detected by EGRET (more than 10% of the total number) have been included in this survey. In no case is a statistically significant signal found in the EGRET error box, which implies that, at least for this sample, the γ-ray spectra of these sources steepen between 100 MeV and 350 GeV. For each EGRET source location, we list candidate associations and derive upper limits on the integral γ-ray flux above 350 GeV. Title: Spectrum of Very High Energy Gamma-Rays from the blazar 1ES 1959+650 during Flaring Activity in 2002 Authors: Daniel, M. K.; Badran, H. M.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D. A.; Catanese, M.; Celik, O.; Cogan, P.; Cui, W.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J. A.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Humensky, T. B.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Le Bohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Müller, D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2005ApJ...621..181D Altcode: 2005astro.ph..3085D The blazar 1ES 1959+650 was observed in a flaring state with the Whipple 10 m Imaging Atmospheric Cerenkov Telescope in 2002 May. A spectral analysis has been carried out on the data from that time period, and the resulting very high energy gamma-ray spectrum (E>=316 GeV) can be well fitted by a power law of differential spectral index α=2.78+/-0.12stat+/-0.21sys. On 2002 June 4, the source flared dramatically in the gamma-ray range without any coincident increase in the X-ray emission, providing the first unambiguous example of an ``orphan'' gamma-ray flare from a blazar. The gamma-ray spectrum for these data can also be described by a simple power-law fit with α=2.82+/-0.15stat+/-0.30sys. There is no compelling evidence for spectral variability or for any cutoff to the spectrum. Title: The very high energy gamma ray spectra of IES 1959+650 and Mrk 421 as measured with the Whipple 10 m telescope Authors: Daniel, M. K.; Badran, H. M.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Byrum, K.; Carter-Lewis, D. A.; Celik, O.; Cogan, P.; Cui, W.; de La Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Guiterrez, K. J.; Hall, J.; Hanna, D.; Holder, J.; Horan, D.; Hughes, S.; Humensky, T. B.; Jung, I.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Le Bohec, S.; Linton, E.; Lloyd-Evans, J.; Mendoza, D.; Merriman, A.; Milovanovic, A.; Moriarty, P.; Nagai, T.; Ong, R. A.; Pallassini, R.; Perkins, J.; Petry, D.; Pohl, M.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Valcarcel, L.; Vassiliev, V. V.; Wagner, R.; Wakely, S. P.; Walker, G.; Weekes, T. C.; White, R. J.; Zweerink, J.; VERITAS Collaboration Bibcode: 2005AIPC..745..462D Altcode: No abstract at ADS Title: Recent Observations of IC443 with the Whipple 10m Telescope Authors: VERITAS Collaboration; Badran, H. M.; Blaylock, G.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Byrum, K.; Carter-Lewis, D. A.; Celik, O.; Cogan, P.; Cui, W.; de La Calle Perez, I.; Daniel, M. K.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Guiterrez, K. J.; Hall, J.; Hanna, D.; Horan, D.; Hughes, S.; Humensky, T. B.; Jung, I.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Le Bohec, S.; Linton, E.; Lloyd-Evans, J.; Mendoza, D.; Merriman, A.; Milovanovic, A.; Moriarty, P.; Nagai, T.; Ong, R. A.; Pallassini, R.; Perkins, J.; Petry, D.; Pohl, M.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Valcarcel, L.; Vassiliev, V. V.; Wagner, R.; Wakely, S. P.; Walker, G.; Weekes, T. C.; White, R. J.; Zweerink, J. Bibcode: 2005AIPC..745..275V Altcode: We present here the results of recent observations made with the Whipple 10m imaging Cherenkov telescope of the region of the supernova remnant IC443. No evidence for gamma-ray emission was found, and we obtain an upper limit above 500 GeV (99.9% confidence) of 0.6 × 10-7 ph m-2 s-1 (0.11 Crab) at the location of the recently identified X-ray plerion nebula and 0.8 × 10-7 ph m-2 s-1 (0.14 Crab) at the site of the OH maser at the densest part of the molecular cloud. Title: Very High Energy Observations of Gamma Ray Bursts with the Whipple/VERITAS Telescopes Authors: Horan, D.; Badran, H. M.; Blaylock, G.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Byrum, K.; Carter-Lewis, D. A.; Celik, O.; Cogan, P.; Cui, W.; Daniel, M. K.; de La Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Guiterrez, K. J.; Hall, J.; Hanna, D.; Holder, J.; Hughes, S.; Humensky, T. B.; Jung, I.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Le Bohec, S.; Linton, E.; Lloyd-Evans, J.; Mendoza, D.; Merriman, A.; Milovanovic, A.; Moriarty, P.; Nagai, T.; Ong, R. A.; Pallassini, R.; Perkins, J.; Petry, D.; Pohl, M.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Valcarcel, L.; Vassiliev, V. V.; Wagner, R.; Wakely, S. P.; Walker, G.; Weekes, T. C.; White, R. J.; Zweerink, J. Bibcode: 2005AIPC..745..591H Altcode: Gamma-ray Burst (GRB) observations at Very High Energies (VHE, E > 100 GeV) can impose tight constraints on some GRB emission models. Many GRB after-glow models predict a VHE component similar to that seen in blazars and supernova remnants, in which the GRB spectral energy distribution has a double-peaked shape extending into the VHE regime. Consistent with this afterglow scenario, EGRET detected delayed high energy emission from all five bright BATSE GRBs that occurred within its field of view. GRB observations have had high priority in the observing program at the Whipple 10m Telescope and will continue to be high priority targets when the next generation observatory VERITAS comes online. Upper limits on the VHE emission from ten GRBs observed with the Whipple Telescope are reported here. Title: The VERITAS Prototype and the Upcoming VERITAS Array Authors: Falcone, Abe D.; Badran, H. M.; Blaylock, G.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Byrum, K.; Carter-Lewis, D. A.; Celik, O.; Cogan, P.; Cui, W.; Daniel, M.; de La Calle Perez, I.; Dowkontt, P.; Duke, C.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Guiterrez, K. J.; Hall, J.; Hanna, D.; Holder, J.; Horan, D.; Hughes, S.; Humensky, T. B.; Jung, I.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Le Bohec, S.; Linton, E.; Lloyd-Evans, J.; Mendoza, D.; Merriman, A.; Milovanovic, A.; Moriarty, P.; Nagai, T.; Olevitch, M.; Ong, R. A.; Pallassini, R.; Perkins, J.; Petry, D.; Pizlo, F.; Pohl, M.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Valcarcel, L.; Vassiliev, V. V.; Wagner, R.; Wakely, S. P.; Walker, G.; Weekes, T. C.; White, R. J.; Zweerink, J.; VERITAS Collaboration Bibcode: 2005AIPC..745..633F Altcode: No abstract at ADS Title: Recent Observations of IC443 with the Whipple 10m Telescope Authors: Holder, J.; Badran, H. M.; Blaylock, G.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Byrum, K.; Carter-Lewis, D. A.; Celik, O.; Cogan, P.; Cui, W.; de La Calle Perez, I.; Daniel, M. K.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Guiterrez, K. J.; Hall, J.; Hanna, D.; Horan, D.; Hughes, S.; Humensky, T. B.; Jung, I.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Le Bohec, S.; Linton, E.; Lloyd-Evans, J.; Mendoza, D.; Merriman, A.; Milovanovic, A.; Moriarty, P.; Nagai, T.; Ong, R. A.; Pallassini, R.; Perkins, J.; Petry, D.; Pohl, M.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Valcarcel, L.; Vassiliev, V. V.; Wagner, R.; Wakely, S. P.; Walker, G.; Weekes, T. C.; White, R. J.; Zweerink, J.; VERITAS Collaboration Bibcode: 2005AIPC..745..275H Altcode: No abstract at ADS Title: The VERITAS Prototype and the Upcoming VERITAS Array Authors: VERITAS Collaboration; Badran, H. M.; Blaylock, G.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Byrum, K.; Carter-Lewis, D. A.; Celik, O.; Cogan, P.; Cui, W.; Daniel, M.; de La Calle Perez, I.; Dowkontt, P.; Duke, C.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Guiterrez, K. J.; Hall, J.; Hanna, D.; Holder, J.; Horan, D.; Hughes, S.; Humensky, T. B.; Jung, I.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Le Bohec, S.; Linton, E.; Lloyd-Evans, J.; Mendoza, D.; Merriman, A.; Milovanovic, A.; Moriarty, P.; Nagai, T.; Olevitch, M.; Ong, R. A.; Pallassini, R.; Perkins, J.; Petry, D.; Pizlo, F.; Pohl, M.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Valcarcel, L.; Vassiliev, V. V.; Wagner, R.; Wakely, S. P.; Walker, G.; Weekes, T. C.; White, R. J.; Zweerink, J. Bibcode: 2005AIPC..745..633V Altcode: The prototype for the VERITAS imaging atmospheric Cherenkov telescope array was successfully operated in southern Arizona between September 2003 and April 2004. The prototype consisted of 86 mirror facets mounted centrally on a 12-meter dish, which was built to accommodate up to 350 facets when converted to a complete VERITAS telescope. The camera consisted of half of the full 499 pixel camera. The signal and trigger electronics were nearly identical to those that will be used for the individual VERITAS array telescopes. By observing the Crab and Mrk421, as well as performing a variety of tests, the characteristics of the instrument were evaluated. The prototype met all performance expectations and served as a valuable test bed for the current design, as well as for the construction and operation of VERITAS. This prototype instrument is now being upgraded to a complete VERITAS telescope that will be operated during the construction of the full VERITAS array. The array is expected to be operational by November 2006. Title: The very high energy gamma ray spectra of IES 1959+650 and Mrk 421 as measured with the Whipple 10 m telescope Authors: VERITAS Collaboration; Badran, H. M.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Byrum, K.; Carter-Lewis, D. A.; Celik, O.; Cogan, P.; Cui, W.; de La Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Guiterrez, K. J.; Hall, J.; Hanna, D.; Holder, J.; Horan, D.; Hughes, S.; Humensky, T. B.; Jung, I.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Le Bohec, S.; Linton, E.; Lloyd-Evans, J.; Mendoza, D.; Merriman, A.; Milovanovic, A.; Moriarty, P.; Nagai, T.; Ong, R. A.; Pallassini, R.; Perkins, J.; Petry, D.; Pohl, M.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Valcarcel, L.; Vassiliev, V. V.; Wagner, R.; Wakely, S. P.; Walker, G.; Weekes, T. C.; White, R. J.; Zweerink, J. Bibcode: 2005AIPC..745..462V Altcode: In observations made with the Whipple 10 m telescope, 1ES 1959+650 (z = 0.048) was caught in a high flaring state in May 2002, concurrent with a high X-ray state, and in June 2002, for which there was no corresponding X-ray flare. The spectra for both of those occasions are well fitted by a power law of differential spectral index ~ -2.8. The relative stability of the spectral index for those flares argues strongly in favour of a two-component model as to the emission zones for the two radiation regimes.

Markarian 421 (z = 0.031) was observed to be in a high flaring state, at levels of >= 3 Crab, during March and April 2004. The average spectrum over this time period shows evidence for a cut-off in the spectrum at ~ 5 TeV, similar to a cut-off seen during an equivalently strong episode of flaring activity in 2001. The continued appearance of this feature indicates a long term stability, either in the physical conditions at the source, or in the intervening medium (such as attenuation on the extra-galactic infra-red background radiation). Title: Search for TeV Radiation from Selected Local Group Galaxies Authors: Hall, J. Bibcode: 2005ICRC....4...69H Altcode: 2005astro.ph..7448H; 2005ICRC...29d..69H Some candidate dark matter particles, such as neutralinos in supersymmetry, would annihilate producing GeV/TeV gamma rays. We report on recent observations of two dwarf spheroid galaxies, Draco, Ursa Minor, the compact elliptical galaxy M32, and the spiral galaxy M33 with the Whipple 10m gamma-ray telescope. No significant signal was found, and we derived upper limits for the gamma-ray flux from each object. We discuss our astrophysical selection criteria for these galaxies in the context of an indirect search for dark matter and the implications of these flux upper limits on the density of neutralinos. Title: A Search for TeV Gamma-Ray Emission from High-peaked Flat-Spectrum Radio Quasars Using the Whipple Air Cerenkov Telescope Authors: Falcone, A. D.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai, T.; Nolan, S.; Ong, R.; Pallassini, R.; Petry, D.; Pizlo, F.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Tyler, K.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2004ApJ...613..710F Altcode: 2004astro.ph..8365F Blazars have traditionally been separated into two broad categories based on their optical emission characteristics. Blazars with faint or no emission lines are referred to as BL Lacertae objects (BL Lacs), and blazars with prominent, broad emission lines are commonly referred to as flat-spectrum radio quasars (FSRQs). The spectral energy distribution of FSRQs has generally been thought of as being more akin to the low-peaked BL Lacs, which exhibit a peak in the infrared region of the spectrum, as opposed to high-peaked BL Lacs (HBLs), which exhibit a peak in UV/X-ray region of the spectrum. All blazars that are currently confirmed as sources of TeV emission fall into the HBL category. Recent surveys have found several FSRQs that exhibit spectral properties, particularly the synchrotron peak frequency, similar to HBLs. These objects are potential sources of TeV emission according to several models of blazar jet emission and the evolution of blazars. Measurements of TeV flux or flux upper limits could impact existing theories explaining the links between different blazar types and could have a significant impact on our understanding of the nature of objects that are capable of TeV emission. In particular, the presence (or absence) of TeV emission from FSRQs could confirm (or cast doubt on) recent evolutionary models that expect intermediate objects in a transitional state between FSRQ and BL Lac. The Whipple 10 m imaging air Cerenkov gamma-ray telescope is well suited for TeV gamma-ray observations. Using the Whipple telescope, we have taken data on a small selection of nearby (z<0.1 in most cases) high-peaked FSRQs. Although one of the objects, B2 0321+33, showed marginal evidence of flaring, no significant emission was detected. The implications of this paucity of emission and the derived upper limits are discussed. Title: The Chromospheric Activity and Variability of Cycling and Flat Activity Solar-Analog Stars Authors: Hall, Jeffrey C.; Lockwood, G. W. Bibcode: 2004ApJ...614..942H Altcode: We present an analysis of more than 3700 observations of the Ca II H and K lines in 57 Sun-like stars and over 3000 analogous observations of the Sun. Ten of the 57 stars under consideration are observed in flat states, but these stars do not always exhibit overall Ca II H and K core brightness below that of solar minimum. Solar activity minimum lies near the lowest level observed for stars with cyclic or irregular variability, but many flat stars have HK activity levels comparable to or exceeding that of solar minimum. While flat activity stars may be in periods of extended activity minima analogous to the solar Maunder minimum, a significant reduction in magnetic activity during such periods is not implied (although it is also not rejected) by the data. Title: Observation of M87 at 400 GeV with the Whipple 10 Meter Telescope Authors: Le Bohec, S.; Badran, H. M.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D. A.; Catanese, M.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J. A.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Müller, D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2004ApJ...610..156L Altcode: We present results from observations taken with the Whipple 10 m very high energy γ-ray telescope with maximal sensitivity at 400 GeV during 39 hr between 2000 and 2003 in the direction of the giant radio galaxy M87. Using the entire data set, we derive a 99% confidence level upper limit on the flux of γ-ray emission above 400 GeV from M87 to be <=6.9×10-12 cm-2 s-1. This suggests variability at the 90% confidence level when compared to the flux measured by the HEGRA collaboration in 1999 if the differential spectrum is steeper than a power law of index 3.75. Our search for a correlation between the Rossi X-Ray Timing Explorer all-sky monitor observation and a potential γ-ray signal is inconclusive. Title: TeV Gamma-Ray Observations of the Galactic Center Authors: Kosack, K.; Badran, H. M.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D. A.; Celik, O.; Connaughton, V.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J. A.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Gutierrez, K.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Le Bohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; McEnery, J.; Moriarty, P.; Muller, D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2004ApJ...608L..97K Altcode: 2004astro.ph..3422K We report a possible detection of TeV gamma rays from the Galactic center by the Whipple 10 m gamma-ray telescope. Twenty-six hours of data were taken over an extended period from 1995 through 2003 resulting in a total significance of 3.7 σ. The measured excess corresponds to an integral flux of 1.6×10-8+/-0.5×10-8 (stat)+/-0.3×10-8 (sys) photons m-2 s-1 above an energy of 2.8 TeV, roughly 40% of the flux from the Crab Nebula at this energy. The 95% confidence region has an angular extent of about 15' and includes the position of Sgr A*. The detection is consistent with a point source and shows no evidence of variability. Title: The Distribution and Variability of Chromospheric Activity in a Large Sample of Solar Analogs Authors: Hall, J. C.; Lockwood, G. W. Bibcode: 2004AAS...204.0302H Altcode: 2004BAAS...36..671H We present the results of approximately 9,000 spectroscopic observations of the chromospheric Ca II H&K emission in a magnitude-limited sample of solar analog stars, as well as nearly 1,000 identical observations of the Sun, taken between 1994 and 2003. We discuss the behavior of Ca variations in the nearest solar analogs relative to the contemporaneous solar record, reconcile our flux measurements with Ca K indices from the NSO as well as Mt. Wilson S, and examine the general activity level in cycling versus non-cycling stars.

Although approximately one third of the stars in the sample show little or no long-term cyclic variability, we find that a lack of such variability does not imply very low levels of magnetic activity. Non-cycling stars exhibit a variety of baseline activity levels, from near-zero magnetic activity to levels comparable to that of the active Sun. We do not find significant evidence for transitions to or from a Maunder minimum state in our current stellar sample, or that such transitions are accompanied by a significant change in a star's overall activity level.

This work has been supported by the National Science Foundation. Title: Measurement of the Total Active 8B Solar Neutrino Flux at the Sudbury Neutrino Observatory with Enhanced Neutral Current Sensitivity Authors: Ahmed, S. N.; Anthony, A. E.; Beier, E. W.; Bellerive, A.; Biller, S. D.; Boger, J.; Boulay, M. G.; Bowler, M. G.; Bowles, T. J.; Brice, S. J.; Bullard, T. V.; Chan, Y. D.; Chen, M.; Chen, X.; Cleveland, B. T.; Cox, G. A.; Dai, X.; Dalnoki-Veress, F.; Doe, P. J.; Dosanjh, R. S.; Doucas, G.; Dragowsky, M. R.; Duba, C. A.; Duncan, F. A.; Dunford, M.; Dunmore, J. A.; Earle, E. D.; Elliott, S. R.; Evans, H. C.; Ewan, G. T.; Farine, J.; Fergani, H.; Fleurot, F.; Formaggio, J. A.; Fowler, M. M.; Frame, K.; Fulsom, B. G.; Gagnon, N.; Graham, K.; Grant, D. R.; Hahn, R. L.; Hall, J. C.; Hallin, A. L.; Hallman, E. D.; Hamer, A. S.; Handler, W. B.; Hargrove, C. K.; Harvey, P. J.; Hazama, R.; Heeger, K. M.; Heintzelman, W. J.; Heise, J.; Helmer, R. L.; Hemingway, R. J.; Hime, A.; Howe, M. A.; Jagam, P.; Jelley, N. A.; Klein, J. R.; Kos, M. S.; Krumins, A. V.; Kutter, T.; Kyba, C. C.; Labranche, H.; Lange, R.; Law, J.; Lawson, I. T.; Lesko, K. T.; Leslie, J. R.; Levine, I.; Luoma, S.; MacLellan, R.; Majerus, S.; Mak, H. B.; Maneira, J.; Marino, A. D.; McCauley, N.; McDonald, A. B.; McGee, S.; McGregor, G.; Mifflin, C.; Miknaitis, K. K.; Miller, G. G.; Moffat, B. A.; Nally, C. W.; Nickel, B. G.; Noble, A. J.; Norman, E. B.; Oblath, N. S.; Okada, C. E.; Ollerhead, R. W.; Orrell, J. L.; Oser, S. M.; Ouellet, C.; Peeters, S. J.; Poon, A. W.; Robertson, B. C.; Robertson, R. G.; Rollin, E.; Rosendahl, S. S.; Rusu, V. L.; Schwendener, M. H.; Simard, O.; Simpson, J. J.; Sims, C. J.; Sinclair, D.; Skensved, P.; Smith, M. W.; Starinsky, N.; Stokstad, R. G.; Stonehill, L. C.; Tafirout, R.; Takeuchi, Y.; Tešić, G.; Thomson, M.; Thorman, M.; van Berg, R.; van de Water, R. G.; Virtue, C. J.; Wall, B. L.; Waller, D.; Waltham, C. E.; Tseung, H. Wan; Wark, D. L.; West, N.; Wilhelmy, J. B.; Wilkerson, J. F.; Wilson, J. R.; Wouters, J. M.; Yeh, M.; Zuber, K. Bibcode: 2004PhRvL..92r1301A Altcode: 2003nucl.ex...9004C; 2003nucl.ex...9004S The Sudbury Neutrino Observatory has precisely determined the total active (νx) 8B solar neutrino flux without assumptions about the energy dependence of the νe survival probability. The measurements were made with dissolved NaCl in heavy water to enhance the sensitivity and signature for neutral-current interactions. The flux is found to be 5.21±0.27(stat)±0.38(syst)×106 cm-2 s-1, in agreement with previous measurements and standard solar models. A global analysis of these and other solar and reactor neutrino results yields Δm2=7.1+1.2-0.6×10-5 eV2 and θ=32.5+2.4-2.3 degrees. Maximal mixing is rejected at the equivalent of 5.4 standard deviations. Title: VERITAS: the Very Energetic Radiation Imaging Telescope Array System Authors: Krennrich, F.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Müller, D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Walker, G.; Wakely, S. P.; Weekes, T. C.; Zweerink, J. Bibcode: 2004NewAR..48..345K Altcode: The Very Energetic Radiation Imaging Telescope Array System (VERITAS) is the major next generation imaging atmospheric Cherenkov γ-ray telescope in the western hemisphere and will be located in southern Arizona nearby Kitt Peak National Observatory. The VERITAS observatory will provide unprecedented sensitivity to photon energies between 50 GeV and 50 TeV. The first stage is an array of four telescopes to be fully operational in early 2006, with an expansion to seven telescopes envisioned for 2008. The construction of a prototype telescope is underway, for which first light is expected in Fall 2003. The technical concept is outlined and a progress report is given. Title: Mars Analog Rio Tinto Experiment (MARTE): 2003 Drilling Campaign to Search for a Subsurface Biosphere at Rio Tinto Spain Authors: Stoker, C.; Dunagan, S.; Stevens, T.; Amils, R.; Gómez-Elvira, J.; Fernández, D.; Hall, J.; Lynch, K.; Cannon, H.; Zavaleta, J.; Glass, B.; Lemke, L. Bibcode: 2004LPI....35.2025S Altcode: The results of an drilling experiment to search for a subsurface biosphere in a pyritic mineral deposit at Rio Tinto, Spain, are described. The experiment provides ground truth for a simulation of a Mars drilling mission to search for subsurface life. Title: Constraints on the Very High Energy Emission from BL Lacertae Objects Authors: Horan, D.; Badran, H. M.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D. A.; Catanese, M.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J. A.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Le Bohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2004ApJ...603...51H Altcode: 2003astro.ph.11397H We present results from observations of 29 BL Lacertae objects, taken with the Whipple Observatory 10 m gamma-ray telescope between 1995 and 2000. The observed objects are mostly at low redshift (z<0.2), but observations of objects of up to z=0.444 are also reported. Five of the objects are EGRET sources and two are unconfirmed TeV sources. Three of the confirmed sources of extragalactic TeV gamma rays were originally observed as part of this survey and have been reported elsewhere. No significant excesses are detected from any of the other objects observed, on timescales of days, months, or years. We report 99.9% confidence level flux upper limits for the objects for each observing season. The flux upper limits are typically 20% of the Crab flux, although for some sources, limits as sensitive as 6% of the Crab flux were derived. The results are consistent with the synchrotron self-Compton model predictions considered in this work. Title: Scientific Ballooning at the Planets Authors: Cutts, J.; Beauchamp, P.; Elfes, A.; Hall, J.; Johnson, T.; Jones, J.; Kerzhanovich, V.; Yavrouian, A.; Zimmerman, W. Bibcode: 2004cosp...35.2466C Altcode: 2004cosp.meet.2466C NASA's Solar System Exploration Roadmap published in May 2003 calls for an investment in aerial mobility in planetary atmospheres to enable key scientific observations at Titan, Venus and Mars. In the case of Venus, the only planet so far explored by balloon, future mission prospects range from extended reconnaissance missions in the high atmosphere to the use of balloons in sample return. At Titan, a balloon or blimp mission might be the next logical step in the exploration of the surface and atmosphere of that body to follow the Cassini observations of Titan from Saturn orbit that begin in July 2004 and the Huygens probe entry of January 05. An aerial mission to the Titan surface would most likely be coupled with a means of sampling potential organic lakes and/or the icy surface. At Mars, balloon missions provide the opportunity to traverse much longer distances than surface missions like the Mars rover and to exploit a vantage point within a few kilometers of the surface to make unique scientific observations. Except for technologies for balloons themselves and their aerial deployment where significant progress has been made recently, a key technology for planetary lighter than air vehicles, especially for Titan, is autonomy. Much higher levels of autonomy than those to date in planetary exploration will be needed for robust scientifically productive exploration. In this presentation we review the mission opportunities and the key technology challenges. Title: An Aerobot for Global In Situ Exploration of Titan Authors: Hall, J.; Kerzhanovich, V.; Yavrouian, A.; Jones, J.; White, C.; Dudik, B.; Elfes, A. Bibcode: 2004cosp...35..198H Altcode: 2004cosp.meet..198H This paper describes the design and component testing of an aerobot that will be capable of global in situ exploration of Saturn's moon, Titan, over a 6 to 12 month mission lifetime. The proposed aerobot is a propeller-driven, buoyant vehicle that resembles terrestrial airships. However, the extremely cold Titan environment requires the use of cryogenic materials of construction and careful thermal design for protection of temperature-sensitive payload elements. Multiple candidate balloon materials have been identified based on extensive laboratory testing at 77 K. The most promising materials to date are laminates comprised of polyester fabrics and/or films with areal densities in the range of 40-100 g/m^2. The aerobot hull is a streamlined ellipsoid 12 meters in length with a maximum diameter of 3 meters. The enclosed volume of 56 m^3 is sufficient to float a mass of 200 kg at a maximum altitude of 8 km at Titan. Forward and aft ballonets are located inside the hull to enable the aerobot to descend to the surface while preserving a fully inflated streamlined shape. Altitude changes are effected primarily through thrust vectoring of the twin main propellers, with pressure modulated buoyancy change via the ballonets available as a slower backup option. A total of 100 W of electrical power is provided to the vehicle by a radioisotope thermal generator. Up to half of this power is available to the propulsion system to generate a top flight speed in the range of 1-2 m/s. This speed is expected to be greater than the near surface winds at Titan, enabling the aerobot to fly to and hover over targets of interest. A preliminary science payload has been devised for the aerobot to give it the capability for aerial imaging of the surface, atmospheric observations and sampling, and surface sample acquisition and analysis. Targeting, hovering, surface sample acquisition and vehicle health monitoring and reflexive safing actions will all require significant on-board autonomy due to the over two hour round trip light time between Titan and Earth. An autonomy architecture and a core set of perception, reasoning and control technologies is under development using a free-flying airship testbed of approximately the same size as the proposed Titan aerobot. Data volume from the Titan science mission is expected to be on the order of 100-300 Mbit per day transmitted either direct to Earth through an 0.8 m high gain antenna or via an orbiter relay using an omni-directional antenna on the aerobot. Title: Search for High-Energy Gamma Rays from an X-Ray-selected Blazar Sample Authors: de la Calle Pérez, I.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D. A.; Celik, O.; Cui, W.; Dowdall, C.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L.; Gaidos, J. A.; Gibbs, K.; Gammell, S.; Hall, J.; Hall, T. A.; Hillas, A. M.; Holder, J.; Horan, D.; Jordan, M.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; LeBohec, S.; Linton, E. T.; Lloyd-Evans, J.; Moriarty, P.; Müller, D.; Nagai, T. N.; Ong, R. A.; Page, M.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C. Bibcode: 2003ApJ...599..909D Altcode: 2003astro.ph..9063D; 2003astro.ph..9063P Our understanding of blazars has been greatly increased in recent years by extensive multiwavelength observations, particularly in the radio, X-ray, and gamma-ray regions. Over the past decade the Whipple 10 m telescope has contributed to this with the detection of five BL Lacertae objects at very high gamma-ray energies. The combination of multiwavelength data has shown that blazars follow a well-defined sequence in terms of their broadband spectral properties. Together with providing constraints on emission models, this information has yielded a means by which potential sources of TeV emission may be identified and predictions made as to their possible gamma-ray flux. We have used the Whipple telescope to search for TeV gamma-ray emission from eight objects selected from a list of such candidates. No evidence has been found for very high energy emission from the objects in our sample, and upper limits have been derived for the mean gamma-ray flux above 390 GeV. These flux upper limits are compared with the model predictions, and the implications of our results for future observations are discussed. Title: The VERITAS Prototype Authors: Wakely, S. P.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2003ICRC....5.2803W Altcode: 2003ICRC...28.2803W We give an up date on the status of the prototype telescope of the Very Energetic Radiation Imaging telescope Array System (VERITAS), a next-generation ˇ atmospheric imaging Cerenkov array currently under construction in southern Arizona. VERITAS will feature significant improvements over previous instruments, including better energy resolution, lower energy threshold, improved an- Title: Calibration Systems for the VERITAS Observatory Authors: Allen, D.; Hall, J.; Kieda, D. B.; Nagai, T.; Snure, M.; Vassiliev, V. V.; Walker, G. Bibcode: 2003ICRC....5.2831A Altcode: 2003ICRC....5.2831K; 2003ICRC...28.2831A We describe the calibration systems used in the VERITAS Imaging Atmoˇ spheric Cerenkov detector. Calibration systems include a charge injection system for measuring electronic gain and testing pattern trigger functionality, optical injection for flat-fielding PMT gains as well as measuring mirror reflectivity, and atmospheric monitoring for measuring changes in atmospheric attenuation, including ground level aerosol concentrations. Title: Search for Very High Energy Gamma Rays from an X-Ray Selected Blazar Sample Authors: de la Calle Perez, I.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2003ICRC....5.2571D Altcode: 2003ICRC...28.2571D; 2003ICRC....5.2571H; 2003astro.ph..5573D; 2003astro.ph..5573P In recent years, blazar surveys at radio and X-ray energies have greatly increased our understanding of this type of active galaxy. The combination of multi-wavelength data has shown that blazars follow a well defined sequence in terms of their broad band spectral properties. Together with increasingly detailed emission models, this information has provided not only to ols with which to identify potential sources of TeV emission but also predictions of their gamma-ray flux. A list of such candidates has been used in this work to investigate the best targets for TeV observations. Observations reported here have resulted in upper limits which do not conflict with the latest model predictions. Title: Signal Cable Selection for the VERITAS Observatory Authors: Kieda, D. B.; Allen, D.; Hall, J.; Nagai, T.; Snure, M.; Vassilev, V. V.; Walker, G. Bibcode: 2003ICRC....5.2835A Altcode: 2003ICRC....5.2835K; 2003ICRC...28.2835A We describe electrical and mechanical tests performed on various coaxial cables to characterize their electrical properties and reliabilities. We use these properties, combined with additional information concerning weight, diameter, and cost, to select the optimum signal cables for the VERITAS observatory. We find significant advantages in using RG-59 Coaxial cable over traditional RG-58 cable. Stranded core RG-59 results in an 30-50% increase in effective mirror area over RG 58; solid core RG59 would result in a 84% increase in effective mirror area. Reliability tests demonstrate that although RG59 solid core will fatigue and fail after repeated twisting, this fatigue would result in a loss of approximately 10 cables over the lifetime of the VERITAS array. Title: Search for TeV Emission at the Location of Milagro Sky Survey Hot Spot Using the Whipple Gamma-Ray Telescope Authors: Falcone, A.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2003ICRC....5.2579F Altcode: 2003ICRC...28.2579F; 2003astro.ph..5575F; 2003ICRC....5.2579G A recent report from the Milagro collab oration included an all-sky map created using one year of data from Milagro (peak sensitivity at 3-4 TeV for Crab-like spectra). This map included an unidentified excess that was brighter than the Crab and was the second brightest spot on the map. The hot spot was within the error box of the EGRET unidentified source 3EG J0520+2556. No strong and steady emission was detected by the Whipple telescope at, or in the vicinity of, either position. The 95% confidence level flux upper limits from Whipple observations at the locations of the Milagro hot spot and the EGRET UnID position are 0.09 Crabs and 0.14 Crabs, respectively. Title: Search for TeV Annihilation Radiation from Supersymmetric Dark Matter in nearby Galaxies Authors: Vassiliev, V. V.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J.; Bromley, B. C. Bibcode: 2003ICRC....5.2679V Altcode: 2003ICRC...28.2679V; 2003astro.ph..5584V During the 2002-2003 observing season the Whipple 10m imaging atmoˇ spheric Cherenkov telescope was used to search for dark matter annihilation radiation in four nearby galaxies: M32, M33, Draco, and Ursa Minor. Scientific motivations for this choice of targets are discussed as well as accumulated exposure. The analysis results are to be reported in the conference presentation. Title: Observation of M87 with the Whipple 10m Telescope Authors: LeBohec, S.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2003ICRC....5.2627L Altcode: 2003astro.ph..5582L; 2003ICRC...28.2627L The Whipple 10-m telescope was used to observe M87 since 2000. No significant gamma-ray signal was found and upper limits compared to the HEGRA detection suggest the source may be variable. We found weak evidence for a correlation with the X-ray activity in 2000-2001 but this tendency did not persist in 2002-2003. Title: VHE Observations of BL Lacertae Objects: 1995-2000 Authors: Horan, D.; Catanese, M. A.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2003ICRC....5.2567H Altcode: 2003ICRC...28.2567H The results of observations of 29 BL Lacertae objects taken with the Whipple Observatory 10 m gamma-ray telescope between 1995 and 2000 are presented. Title: A Search for Pulsed TeV Gamma-Ray Emission from the Crab Pulsar Using the Whipple High Resolution GRANITE III Camera Authors: Kildea, J.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2003ICRC....4.2377K Altcode: 2003astro.ph..5580K; 2003ICRC...28.2377K; 2003ICRC....4.2377G We present the results of a search for pulsed TeV emission from the Crab pulsar using 97 hours of data recorded with the high-resolution GRANITE I I I camera of the Whipple 10 m gamma-ray telescope. Title: Whipple Observations of 1ES1959+650: An Update Authors: Holder, J.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2003ICRC....5.2619H Altcode: 2003astro.ph..5577H; 2003ICRC...28.2619H Strong flares of TeV gamma-ray emission up to a level of ∼ 5 Crab were ˇ detected by the Whipple 10 m atmospheric Cerenkov telescope from the BL Lacertae object 1ES1959+650 during May July 2002. We report here the results of follow up observations during 2002 2003. Title: Performance of the VERITAS-4 Array Authors: Fegan, S. J.; Hall, J.; Vassiliev, V. V. Bibcode: 2003ICRC....5.2847F Altcode: 2003ICRC...28.2847F We present the simulated characteristics of VERITAS-4, a four telescope instrument, scheduled to be operational in 2005. Title: Search for a WIMP Annihilation Signature in the Core of the Globular Cluster M15 Authors: LeBohec, S.; Baltz, E. A.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2003ICRC....4.2521L Altcode: 2003ICRC...28.2521L; 2003astro.ph..5581L The Whipple 10m Very High Energy gamma-ray telescope has been used to search for indications of WIMP annihilation in the direction of the globular cluster M15. The upper limits derived constrain the amount of super-symmetric dark matter that may reside in globular clusters. Title: Whipple Telescope Observations of Potential TeV Gamma-Ray Sources Found by the Tibet Air Shower Array Authors: Walker, G.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Weekes, T. C.; Zweerink, J. Bibcode: 2003ICRC....5.2563W Altcode: 2003ICRC...28.2563W An all-sky survey performed with the Tibet Air Shower Array (Tib et AS) has found a number of potential point sources of TeV gamma rays. If they are steady sources, the implied Tibet AS fluxes should be visible with strong significance to the Whipple 10-m gamma-ray telescope (E > 400 GeV) with only a short (5 hour) exposure. We have observed four candidate directions from the Tibet-I I HD dataset for ∼5 hours each with the Whipple telescope. In addition, we observed a new candidate direction from the Tibet-I I I Phase 1 dataset for 7.5 hours. We have found no corresponding excesses at the flux levels implied, and we have set upper limits for each candidate. Title: Hourly Spectral Variability of Mrk 421 Authors: Krennrich, F.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2003ICRC....5.2603K Altcode: 2003ICRC...28.2603K; 2003astro.ph..5419K Mrk 421 is the first TeV blazar found to exhibit significant spectral variability during strong flaring activity, showing hardening of the TeV spectrum in high emission states. Mrk 421 is also known to exhibit flux variability on time scales as short as 15 minutes. In this paper we present studies of hourly spectral variability of Mrk 421 in 2001 using data from the Whipple Observatory 10 m gamma-ray telescope. Title: Very High Energy Observations of PSR B1823-13 Authors: Hall, T. A.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2003ICRC....4.2497H Altcode: 2003astro.ph..5576H; 2003ICRC....4.2497M; 2003ICRC...28.2497H To date three plerionic systems have been detected as emitters of very energetic photons. As part of an ongoing study of pulsar systems at the Whipple observatory, observations of the plerion PSR B1823-13 are being conducted. Observations were made with the Whipple 10 m gamma-ray telescope utilizing the high resolution, 490 pixel camera. Title: Observations of Starburst Galaxies Authors: Nagai, T.; Vassiliev, V. V.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2003ICRC....5.2635N Altcode: 2003ICRC...28.2635N The search for TeV gamma-ray radiation from starburst galaxies (SBGs) has been conducted by the Whipple 10-m gamma-ray telescope from January 2001 to March 2003. The regions with high star formation rates (SFRs) observed in SBGs are frequently accompanied by high density clouds of interstellar matter (ISM). This seems to create nearly perfect conditions for generating diffuse gamma-ray radiation as high energy cosmic rays interact with the ISM. If the current paradigm that supernovae are the origin of high energy cosmic rays is valid, then star forming regions rich in type Ib/c, I I supernovae may become the lab oratories to test the hypothesis. Using the Whipple telescope we have conducted a survey of several plausible SBGs selected based on their distance, density of gas clouds, age of star forming regions, SFRs, and magnetic fields, as well as the presence of radio flux and X-ray point sources. We discuss the selection criteria based on gamma-ray flux estimates, as well as the results of a novel spectrum dependent analysis (to be reported during presentation) of SBG observations for which a total exposure of 10-30 hours per source have been accumulated. Title: Intensive TeV Gamma-Ray and X-Ray Observations of the Blazar Mrk 421 in December 2002 and January 2003 Authors: Rebillot, P. F.; Hughes, S. B.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2003ICRC....5.2599R Altcode: 2003ICRC...28.2599R; 2003astro.ph..5583R We report on observations of Markarian 421 made with the Whipple 10m ˇ erenkov telescope and the RXTE satellite during a multi-wavelength campaign C in December 2002 and January 2003, initiated by a Whipple target of opportunity. The observations revealed several flares with flux levels between 1 and 2 times the flux of the Crab Nebula. We will discuss the temporal properties, including evidence of X-ray/TeV gamma-ray flux correlation. Title: Veritas CFDs Authors: Hall, J.; Vassiliev, V. V.; Kieda, D. B.; Moses, J.; Nagai, T.; Smith, J. Bibcode: 2003ICRC....5.2851H Altcode: 2003ICRC....5.2851V; 2003ICRC...28.2851H The Level 1 (pixel) trigger of a VERITAS telescope is described. The trigger uses a constant fraction discriminator (CFD) to decrease VERITAS operation energy threshold by reducing the coincidence resolving time between neighb oring pixels to ∼ 5 ns. We discuss the optimization of the CFD design as well as ˇ unique requirements of the CFD application in a Imaging Atmospheric Cerenkov telescope (IACT). We describe a novel feedback circuit to provide real time optimization of CFD performance under variable NSB conditions. Tests of the Level 1 trigger demonstrate jitter < 1 ns with background noise values up to 0.8 pe/ns. Title: TeV Observations of the Galactic Center Authors: Kosack, K.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2003ICRC....4.2513K Altcode: 2003astro.ph..5592K; 2003ICRC....4.2513R; 2003ICRC...28.2513K We present the results of 16 hours of ongoing observations of the galactic center region (including Sagittarius A*) with the Whipple High Energy GammaRay telescope. We apply a data analysis method optimized for large zenith angle observations on an indep endent Crab Nebula data set. We discuss possible systematic problems associated with observations of extended sources in the galactic plane. Title: Observations of H1426+428 from 1999 to 2002 with the Whipple Observatory 10 m Telescope Authors: Horan, D.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. Bibcode: 2003ICRC....5.2647H Altcode: 2003ICRC...28.2647H; 2003astro.ph..5579H The BL Lacertae object H1426+428 is the most distant, confirmed source of TeV gamma rays. At a redshift of 0.129, its detection at TeV energies has important implications for estimating the density of the extragalactic infra-red background radiation. H1426+428 was observed extensively during the 2001/2002 observing season with the Whipple 10 m gamma-ray telescope. The results of these observations are presented here and are combined with the results of previous observations made between 1999 and 2001 at Whipple. Title: Chromospheric Activity in Solar-Type Stars Authors: Giampapa, M. S.; Hall, J. C.; Radick, R. R.; Baliunas, S. L. Bibcode: 2003SPD....34.0710G Altcode: 2003BAAS...35..821G We present an update on the results of a survey of chromospheric activity in the solar-age and solar-metallicity open cluster, M67. The objective of the survey is to gain insight on the potential range of amplitudes of the solar cycle through observations of solar analogs that are presumably at random phases in their cycles of magnetic activity. We find that there is a significant overlap of the levels of Ca II H and K emission in the sun-like stars in M67 with the range of activity seen in the contemporary solar cycle. However, there are also stars that exhibit levels of activity outside of this range, including stars that are "super-solar" in their Ca II H and K emission. The implications of these results will be discussed.

The data presented in this investigation were obtained with the WIYN 3.5-m telescope on Kitt Peak. The WIYN Observatory is a joint facility of the University of Wisconsin-Madison, Indiana University, Yale University, and the NOAO. The NSO and the NOAO are operated by AURA for the National Science Foundation. Title: Detection of TeV Gamma Rays from the BL Lacertae Object 1ES 1959+650 with the Whipple 10 Meter Telescope Authors: Holder, J.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D. A.; Cui, W.; Dowdall, C.; Duke, C.; de la Calle Perez, I.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L.; Gaidos, J. A.; Gibbs, K.; Gammell, S.; Hall, J.; Hall, T. A.; Hillas, A. M.; Horan, D.; Jordan, M.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; LeBohec, S.; Linton, E. T.; Lloyd-Evans, J.; Moriarty, P.; Müller, D.; Nagai, T. N.; Ong, R.; Page, M.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C. Bibcode: 2003ApJ...583L...9H Altcode: 2002astro.ph.12170H We present the first strong detection of very high energy γ-rays from the close (z=0.048) X-ray-selected BL Lacertae object 1ES 1959+650. Observations were made with the Whipple 10 m telescope on Mount Hopkins, Arizona, using the atmospheric Cerenkov imaging technique. The flux between 2002 May and July was highly variable, with a mean of 0.64+/-0.03 times the steady flux from the Crab Nebula and reaching a maximum of 5 crab, with variability on timescales as short as 7 hr. Title: The TeV Spectrum of H1426+428 Authors: Petry, D.; Bond, I. H.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D. A.; Cui, W.; Duke, C.; de la Calle Perez, I.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Gaidos, J. A.; Gibbs, K.; Gammell, S.; Hall, J.; Hall, T. A.; Hillas, A. M.; Holder, J.; Horan, D.; Jordan, M.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krennrich, F.; LeBohec, S.; Moriarty, P.; Müller, D.; Nagai, T. N.; Ong, R.; Page, M.; Pallassini, R.; Power-Mooney, B.; Quinn, J.; Reay, N. W.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Sidwell, R.; Stanton, N.; Swordy, S. P.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C. Bibcode: 2002ApJ...580..104P Altcode: 2002astro.ph..7506P The BL Lac object H1426+428 was recently detected as a high-energy γ-ray source by the VERITAS collaboration (Horan et al.). We have reanalyzed the 2001 portion of the data used in the detection in order to examine the spectrum of H1426+428 above 250 GeV. We find that the time-averaged spectrum agrees with a power law of the shape(dF/dE)(E)=10-7.31+/-0.15stat+/- 0.16systE-3.50+/-0.35stat+/- 0.05systm-2s-1TeV- 1.The statistical evidence from our data for emission above 2.5 TeV is 2.6 σ. At the 95% confidence level, the integral flux of H1426+428 above 2.5 TeV is larger than 3% of the corresponding flux from the Crab Nebula. The spectrum is consistent with the (noncontemporaneous) measurement by Aharonian et al. both in shape and in normalization. Below 800 GeV, the data clearly favor a spectrum steeper than that of any other TeV blazar observed so far, indicating a difference in the processes involved either at the source or in the intervening space. Title: Past and future trends in stellar activity cycle research: beyond Ca II H&K Authors: Hall, Jeffrey C. Bibcode: 2002ESASP.508..121H Altcode: 2002soho...11..121H Olin C. Wilson began stellar activity cycle research in 1966, and work has since proceeded along a number of observational and theoretical lines. Long-term ground-based spectroscopic monitoring of the Ca II H&K activity proxies has demonstrated the existence of varying types of stellar cycles, while complementary photometric studies have revealed luminosity variations both in phase and in antiphase with chromospheric activity. Beginning in the late 1970s, space-based observations greatly affected our understanding of stellar chromospheres, spurring a complementary evolution in interpretation of the ground-based results. Excellent recent reviews of the results of these programs have appeared, so in this paper, I will summarize the results and review them in the broad context of the development of our present state of knowledge, current outstanding questions and pitfalls facing workers in the field today, and the lines of investigation likely to be fruitful in the next decade. Title: Gauging the Sun: Comparative photometric and magnetic activity measurements of sunlike stars, 1984-2001 Authors: Lockwood, G. W.; Hall, J. C.; Skiff, B. A.; Henry, G. W.; Radick, R. R.; Baliunas, S. L.; Soon, W.; Donahue, R. A. Bibcode: 2002AAS...200.0709L Altcode: 2002BAAS...34..651L Visible light photometric observations of a small sample of sunlike stars with mean chromospheric activity levels similar to or slightly lower than the Sun's suggest that total solar irradiance variations on activity cycle timescales may be comparatively small (Lockwood et al. 1992, Nature 360, 653; Radick et al. 1998, ApJS 118, 239). The Sun's irradiance variation over the past two cycles is 0.04% rms compared with 0.1% rms for the stellar sample measured at Lowell from 1984 to 1995. This assertion can now be tested using new photometric measurements from Fairborn Observatory automated telescopes (1993-2001) that extend the duration of stellar observations to 17 years. Chromospheric activity measurements for these stars come from the Mount Wilson HK program (1966-2001) and the Lowell Observatory Solar Stellar Spectrograph program (1993-2001). In this presentation we will describe efforts to merge the overlapping Lowell and Fairborn photometry and the Mt. Wilson and Lowell HK measurements with the goal of reducing the uncertainties in previous efforts to characterize stellar photometric variations near the limit of detection. Title: Evidence of a Pronounced Activity Cycle in the Solar Twin 18 Scorpii Authors: Hall, Jeffrey C.; Lockwood, G. W. Bibcode: 2000ApJ...545L..43H Altcode: The star 18 Scorpii (HD 146233, HR 6060) is currently regarded as the nearest solar twin. We have been observing this star on our solar-stellar spectrograph program since 1995. In this Letter we present our Ca K observations of 18 Sco through 2000 July. The data show a pronounced rise that suggests 18 Sco has a well-defined activity cycle that reached an apparent minimum in 1998 and showed a rapid rise through the most recent of our year 2000 data. Comparison with contemporaneous solar data, obtained with the same instrument, suggests that the activity cycle of 18 Sco may be of greater amplitude than the Sun's and that its overall chromospheric activity level is noticeably greater than the Sun's. This excellent solar photometric twin therefore may be a less perfect spectroscopic twin. Title: Composite Spectral Indices: A New Method for the Interpretation of Solar and Stellar Activity Authors: Hall, Jeffrey C.; Lockwood, G. W. Bibcode: 2000ApJ...541..436H Altcode: Activity in solar-like stars is often characterized by one, or at most a handful, of proxy spectral indicators such as Ca II H and K or Hα. In this paper we define and explore composite spectral indices (CSIs), which are derived from consideration of the simultaneous behavior of larger sets of related spectral lines. With judiciously defined CSIs, we can examine the short- and long-term variability in a set of solar or stellar spectra in a complementary way to the traditional K index. In this paper we demonstrate this method, using our solar data series spanning the cycle 22/23 minimum and the initial rise of cycle 23, from 1994 through 1999, and using initial CSIs chosen to be sensitive to the presence of sunspots. We find that despite the relative inactivity of the Sun during the time period in question, analysis of the CSIs reveals the change in sunspot number through solar minimum in a well-defined way. Manifestation of this solar property in the CSIs indicates their utility for study of other physical characteristics in the same way, as well as for comparison of the Sun's physical properties and low-level variability to individual solar analogs. Title: A Survey of Activity in the Solar-Type Stars in M67 Authors: Giampapa, M. S.; Radick, R. R.; Hall, J. C.; Baliunas, S. L. Bibcode: 2000SPD....3102120G Altcode: 2000BAAS...32..832G We present an update on a long-term study of the solar-type stars in the solar-age and solar-metallicity open cluster, M67. The primary objective of this program is to gain insight on the possible range of solar chromospheric activity and the associated, potential long-term variability of the Sun through the observation of stellar analogs of the Sun. Spectra in the Ca II H & K line region of over 100 stars in M67, including 76 `solar-type' stars (with unreddened colors in the range +0.60 <= B-V <= +0.76) and 21 `solar-twins' (+0.63 <= B-V <= +0.67), were obtained with the 3.5-m WIYN telescope on Kitt Peak in conjunction with the Hydra multi-fiber positioner to perform multi-object spectroscopy over a 1 degree field. We find that the distribution of chromospheric H&K line strengths in the solar-type stars is broader than the distribution of H&K line emission recorded in modern observations of the Sun, suggesting that the potential excursion in the amplitude of the solar cycle is greater than what we have seen so far in the contemporary record. Approximately 30% of the solar-type stars in M67 exhibit levels of activity that are outside the present envelope of solar activity. We interpret this to mean that the Sun can be in a state of magnetic activity---either exceptional quiescence similar to the Maunder-minimum episode or enhanced activity---about 30% of the time. The authors gratefully acknowledge both the NOAO Telescope Allocation Committee and the WIYN Queue Program for their support of this investigation. The WIYN Observatory is a joint facility of the University of Wisconsin-Madison, Indiana University, Yale University, and the NOAO. The NSO and NOAO are operated by AURA, Inc., under cooperative agreement with the National Science Foundation. Title: Evaluation of Solar Activity in Multiple Spectral Lines, 1994-1998 Authors: Hall, J. C.; Lockwood, G. W. Bibcode: 1999AAS...19510704H Altcode: 1999BAAS...31.1531H We present a method for evaluating solar and stellar activity in terms of the ensemble behavior of many related spectral lines, rather than using just the classic chromospheric proxy lines such as Ca II H&K. Manifestations of solar and stellar activity that are undetectable in a single spectral line become apparent when many lines are used in tandem. The resulting activity indices (1) allow us to examine solar activity with greater precision than would otherwise be possible and (2) allow us to make meaningful comparisons between the Sun and individual solar analogs. In this poster, we show how these indices have reliably tracked solar activity through the Cycle 22/23 minimum. This work is supported by a grant from the National Science Foundation. Title: Cycles and Long-Term Variability in Solar-Type Stars Authors: Giampapa, Mark S.; Radick, Richard R.; Hall, Jeffrey C.; Baliunas, Sallie L. Bibcode: 1999noao.prop..226G Altcode: We propose a long-term extension of our current WIYN/Hydra program to study chromospheric activity cycles in the `Suns of M67.' Our results thus far have revealed that the distribution of activity among the solar- type stars in M67 is broader than what would be expected from a comparison with the solar cycle. The next step is to determine whether our results arise from the cyclic modulation of activity alone or if the relative amplitudes of cycles in solar-type stars and the Sun are actually similar and the spread in M67 is due to differences in the mean level of activity. Only a long-term monitoring program of regular observations can address these questions. The results of this program are expected to reveal all the potential modes and amplitudes of magnetic cycles in sun-like stars and, by inference, in the Sun itself, with important implications for dynamo models and models of global climate change. Title: Fixed-Phase Observations of RS Canum Venaticorum and BY Draconis Systems Authors: Hall, Jeffrey C.; Wolovitz, Jeffrey B. Bibcode: 1998AJ....115.2571H Altcode: We present our data set of same-hemisphere, or fixed-phase, observations of five RS Canum Venaticorum and BY Draconis binaries made with the Solar-Stellar Spectrograph at Lowell Observatory. The purpose of this study is to evaluate the level of intrinsic variability in the components of these systems, and to compare it with variability arising from rotational modulation and from long-term, activity cycle-related variability. We obtain fixed-phase observations by observing tidally locked binaries with near-integral-day periods. The fixed-phase observations reveal that the intrinsic variability of the stellar hemispheres is significantly less than the variability induced by rotational modulation or by long-term, activity-cyclic evolution, but only when several spectral features are considered in tandem. Fixed-phase ``flickering'' of the stellar hemispheres is often apparent at a higher level than the rotational or long-term modulation in individual activity indicators. Interpretation of rotational or long-term modulation in active, late-type stars using data that do not allow quantification of the fixed-phase variability of the stars (i.e., data that do not span several rotational periods) is extremely risky. Title: The Solar Activity Cycle. I. Observations of the End of Cycle 22, 1993 September--1997 February Authors: Hall, Jeffrey C.; Lockwood, G. W. Bibcode: 1998ApJ...493..494H Altcode: We have monitored the Sun through a large portion of the near-IR, optical, and near-UV spectrum since late 1993 as part of our long-term observing program with the Solar-Stellar Spectrograph (SSS) at Lowell Observatory. In this paper we present our database through early 1997, which covers the end of solar cycle 22 and the first months of cycle 23. Our goals in this paper are fourfold: (1) to establish the absolute consistency of our data using an automated, completely objective reduction protocol, (2) to establish a calibration to physical flux across the entire SSS spectrum for our solar data, (3) to examine the record of the main chromospheric activity indicator, Ca II K, in our data, and (4) to search for the Sun's rotational signal in our data set, to the end that clear detection of the solar rotation at activity minimum would bode well for our ability to detect rotational signals in other, more active stars. Further analysis and modeling of these solar data will appear in forthcoming papers in this series. Title: Composite Spectral Indices: a New Method for the Interpretation of Activity in the Sun and Solar Analogs Authors: Hall, Jeffrey C. Bibcode: 1998saco.conf..143H Altcode: No abstract at ADS Title: Solar analogs : characteristics and optimum candidates /edited by Jeffrey Authors: Hall, Jeffrey C. Bibcode: 1998saco.conf.....H Altcode: No abstract at ADS Title: Multiwavelength Activity Profiles of Cool Stars Authors: Hall, J. C.; Baliunas, S. L. Bibcode: 1996AAS...189.8108H Altcode: 1996BAAS...28.1383H We have constructed detailed observing histories of a large number of cool stars by combining measurements of magnetic-activity-sensitive lines in ground-based data and space archival data into what we term multiwavelength activity profiles (MAPs) of these stars. To construct a MAP, we first combine the Mt. Wilson Observatory HK project data and the Lowell Observatory Solar-Stellar Spectrograph (SSS) near-UV to near-IR data for a given target into absolute-flux-calibrated records of the star's chromospheric variability. We then add IUE NEWSIPS-processed spectra and available EUV and X-ray data to produce the final MAP, which provides a comprehensive picture of the long-term variability in the target stars from their low chromospheres to their coronae. In this poster we present representative MAPs for nine stars with large space-based data sets (HDs 20630, 22049, 35296, 39587, 61421, 72905, 115383, 131156A, and 201091). We first describe how we combine the various data into a uniformly calibrated MAP, and then examine the response of different regions of the stellar atmospheres to cyclic, rotational, and short-term variability. Title: VizieR Online Data Catalog: Empirical stellar flux scales (Hall 1996) Authors: Hall, J. C. Bibcode: 1996yCat..61080313H Altcode: Several studies have appeared in the literature describing methods for deriving stellar continuum fluxes as simple functions of Johnson color indices. In previous papers, we have used similar relations to derive Ca II H & K line core fluxes for dwarf stars on Lowell Observatory's Solar-Stellar Spectrograph (SSS) program. Our desire is to present our data, and complementary data from the Mt. Wilson and National Solar Observatory stellar and solar programs, in terms of physical fluxes. However, our existing relations break down for mid-K and later stars and for giant stars, which form an important element of our target list. In this work I have used a broader range of spectrophotometry and angular diameters than in our previous work to derive empirical flux scales for spectral types A to early M, luminosity classes I to V, and for four color indices, Johnson B-V, V-R, R-I, and Stromgren b-y. In this paper I describe the methods I used and present the derived flux scales. I compare the results with those from earlier studies and present examples of the use of the flux scales. The data and results are available on the World Wide Web home page. Access http://www.lowell.edu, select "Lowell staff", and select the author's home page. (4 data files). Title: On the Determination of Empirical Stellar Flux Scales Authors: Hall, Jeffrey C. Bibcode: 1996PASP..108..313H Altcode: Several studies have appeared in the literature describing methods for deriving stellar continuum fluxes as simple functions of Johnson color indices. In previous papers, we have used similar relations to derive Ca II H and K line core fluxes for dwarf stars on Lowell Observatory's Solar-Stellar Spectrograph (SSS) program. Our desire is to present our data, and complementary data from the Mt. Wilson and National Solar Observatory stellar and solar programs, in terms of physical fluxes. However, our existing relations break down for mid-K and later stars and for giant stars, which form an important element of our target list. In this work I have used a broader range of spectrophotometry and angular diamters than in our previous work to derive empirical flux scales for spectral types A to early M, luminosity classes I to V, and for four color indices, Johnson B-V, V-R, R-I, and Stromgren b-y. In this paper, I describe the methods I used and present the desired flux scales. I compare the results with those from earlier studies and present examples of the use of the flux scales. The data and results are available on the World Wide Web. (SECTION: Stars) Title: Cross-correlation radial velocity measurements of chromospherically active binaries. Authors: Gunn, A. G.; Hall, J. C.; Lockwood, G. W.; Doyle, J. G. Bibcode: 1996A&A...305..146G Altcode: We present observational radial velocity curves for 12 chromospherically active binary systems and individual measurements for a further 5 systems. These binaries are LX Per, V 471 Tau, EI Eri, OU Gem, GK Hya, TY Pyx, Z Her, MM Her, V772 Her, ER Vul, BD-004234, MY Cyg, AR Lac, KZ And, RT And, SZ Psc and EZ Peg. Six of our target binaries do not agree with published ephemerides or orbital parameters. We also present a rigorous derivation of the resolution limit for binary star cross-correlation radial velocities. Using synthetic spectral data we investigate the errors induced by rotational broadening, signal-to-noise ratio, spectral-type mismatch and luminosity ratio. Title: Activity Cycles in Cool Stars. I. Observation and Analysis Methods and Case Studies of Four Well-observed Examples Authors: Hall, Jeffrey C.; Lockwood, G. W.; Gibb, Erika L. Bibcode: 1995ApJ...442..778H Altcode: This is the first in a series of papers devoted to the ongoing long-term monitoring program of activity cycles in cool stars at Lowell Observatory. In this paper we discuss the various spectral diagnostics we have at our disposal and how we calibrate these diagnostics to flux. We then present our current database for four well-studied stars, HD 10700, HD 22049, HD 39587, and the Sun, comparing our results to results obtained by other investigators and discussing how our new database complements existing work. With the same data we demonstrate our ability to detect activity cycles and rotational modulation in a variety of diagnostic lines for stars of widely differing activity levels and spectral types. Title: The Solar-Stellar Spectrograph: Project Description, Data Calibration, and Initial Results Authors: Hall, Jeffrey C.; Lockwood, G. W. Bibcode: 1995ApJ...438..404H Altcode: The Solar-Stellar Spectrograph (SSS) is a project initiated in the 1980s by scientists from the High Altitude Observatory, Lowell Observatory, the Pennsylvania State Universty, and the Sacramento Peak Observatory. The instrument is comprised of two spectrographs: one is an echelle covering the wavelength range lambda lambda 5000-9200, while the second is a Littrow spectrograph covering the Ca II and H and K region around lambda 3950. This project is designed to address a broad range of outstanding questions regarding the nature of stellar activity cycles. The unique capability of the spectrograph is its ability to record both solar and stellar spectra, allowing more accurate placement of the Sun in the stellar context than has been feasible previously. In this report we discuss the motivation for this project, the instrumental characteristics, the observing programs, the methods being used to reduce, calibrate, and analyze the data, and the connection of our databases to extant databases. A central part of the discussion is the connection of the Sun with the stars both in terms of existing solar and stellar activity indices as well as physical flux. This work resolves a long-standing discrepancy in this area and establishes a protocol for relating the large set of observations from the Mount Wilson Ca II H and K project to physical flux, in preparation for future comparison to our observations and results from theory. Title: The Solar-Stellar Spectrograph: Unification of Solar and Stellar Flux Scales and Initial Results Authors: Hall, Jeffrey C.; Lockwood, G. W.; Gibb, Erika L. Bibcode: 1994AAS...185.8017H Altcode: 1994BAAS...26Q1449H We present the science results from the first two years of the Solar-Stellar Spectrograph (SSS) project. These results will include (1) representative observations from our current database of ~ 1500 spectra of about 200 solarlike stars, (2) a discussion of their calibration to flux, (3) our initial detections of cyclic as well as shorter-term variability, (4) variability correlations between various diagnostic lines, (5) the unification of our flux-calibrated data to all extant datasets, in particular the Mt. Wilson S index, and (6) the consistent placement of the Sun among the stellar sample. Title: The Solar-Stellar Spectrograph: The Sun in 1994 Authors: Lockwood, G. W.; Hall, Jeffrey C.; Gibb, Erika L. Bibcode: 1994AAS...185.8016L Altcode: 1994BAAS...26.1449L We present Ca II HK and IRT and Hα observations of the end of solar cycle 22 in 1994. We discuss the calibration of these activity diagnostics to flux and compare the results with similarly determined fluxes from stellar analogs of the Sun. We reconcile these data with the long-term NSO datasets and with the Mt. Wilson S index of stellar activity, establishing a spectroscopic context for accurate placement of the Sun among the stars. Title: Multiwavelength Study of the Magnetically Active T Tauri Star HD 283447 Authors: Feigelson, Eric D.; Welty, Alan D.; Imhoff, Catherine; Hall, Jeffrey C.; Etzel, Paul B.; Phillips, Robert B.; Lonsdale, Colin J. Bibcode: 1994ApJ...432..373F Altcode: We observed the luminous T Tauri star HD 283447 = V773 Tauri simultaneously at X-ray, ultraviolet, optical photometric and spectroscopic, and radio wavelengths for several hours on UT 1992 September 11. ROSAT, IUE, Very Large Array (VLA) and an intercontinental Very Long Baseline Interferometry (VLBI) network, and three optical observatories participated in the campaign. The star is known for its unusually high and variable nonthermal radio continuum emission. High levels of soft X-ray and Mg II line emission are discovered, with luminosity Lx = 5.5 x 1030 ergs/s (0.2 - 2 keV) and LMg II = 1 x 1029 ergs/s, respectively. Optically, the spectrum exhibits rather weak characteristics of `classical' T Tauri stars. A faint, broad emission line component, probably due to a collimated wind or infall, is present. During the campaign, the radio luminosity decreased by a factor of 4, while optical/UV lines and X-ray emission remained strong but constant. The large gyrosynchrotron-emitting regions are therefore decoupled from the chromospheric and coronal emission. Five models for the magnetic geometry around the star are discussed; solar-type activity, dipole magnetosphere, star-disk magnetic coupling, disk magnetic fields, and close binary interaction. The data suggest that two magnetic geometries are simultaneously present: complex multipolar fields like those on the Sun, and a large-scale field possibly associated with the circumstellar disk. Title: Eclipse Observations of RS CVN Binaries II. A Parametric Model of Extended Matter Authors: Hall, Jeffrey C.; Ramsey, Lawrence W. Bibcode: 1994AJ....107.1149H Altcode: We have surveyed ten RS CVn binary systems and have detected large regions of extended, prominencelike material which we have shown to be a common feature in these systems. These extended regions are apparent as anomalous absorption features in the spectra when they obscure the disk of the eclipsed star and as weak emission features when they appear with no disk behind. We have constructed a first-generation model to verify the general prominencelike nature of the material and to estimate its extent and its most basic physical characteristics. In this paper we present our results of our modeling on four of the systems in our survey that showed clear signatures of extended material: AW Her, MM Her, SS Boo, and UV Psc. We find that these stellar prominencelike structures are very much larger than their solar counterparts, though their gross physical characteristics (i.e., their electron density and temperature and their general appearance as tenuous, vertically oriented, magnetically confined structures) are similar to those seen in solar prominences. These features appear to evolve fairly rapidly, since moderate- to high-velocity flows ranging from several tens of km/s to 170 km/s are apparent. However, in at least one case (SS Boo) they are recurrent over a time scale of at least a year. We conclude by discussing the implications of this work regarding the nature of close binary star active structures and their evolution. Title: The Reduction of Fiber-Fed Echelle Spectrograph Data: Methods and an IDL-Based Solution Procedure Authors: Hall, Jeffrey C.; Fulton, Eliza E.; Huenemoerder, David P.; Welty, Alan D.; Neff, James E. Bibcode: 1994PASP..106..315H Altcode: Echelle spectrograph data present several challenges in data reduction. In this paper we address the general problem of accurately extracting spectra from a night's worth of raw CCD fiber-fed echelle data frames. We first briefly review echelle spectroscopy: properties of the basic echelle spectrograph, how the orders are arranged on the CCD, and what demands and constraints this data format places on reduction algorithms. We then discuss solutions to the various problems for fiber-fed data, with particular emphasison the removal of the scattered light background. Finally, we discuss our implementation of these solutions. We have written a package using the Interactive Data Language (IDL) that uses the methods described in this paper to give accurate extractions of spectra from fiber-fed echelle frames with any number of spectral orders of arbitrary tilt and curvature. We describe how interested persons may obtain the package through anonymous FTP. (SECTION: Instrumentation and Data Analysis) Title: Evidence for physically distinct source regions for Balmer and Ca II excess emission in RS CVn binaries. Authors: Chester, M. M.; Hall, J. C.; Buzasi, D. L. Bibcode: 1994ASPC...64..390C Altcode: 1994ASPC...64..390M; 1994csss....8..390C Quantitative statistical comparisons of Balmer and Ca II infrared triplet excess emission diagnostics for solar plages and five active RS CVn binaries are discussed. Models of Balmer line emission by Buzasi and the study of eclipsing systems by Hall and Ramsey previously demonstrated the presence of significant amounts of extended, prominence-like material in RS CVns. In contrast to the Balmer emission, the Ca II infrared triplet appears to arise predominantly in chromospheric plage. The RS CVns are not simply scaled-up solar active regions. Title: Multiwavelength Campaign of the Magnetically Active T Tauri Star HD 283447 Authors: Feigelson, Eric D.; Welty, Alan D.; Imhoff, Catherine L.; Hall, Jeffrey C.; Etzel, Paul B.; Deeney, Bryan D.; Phillips, Robert B.; Lonsdale, Colin J. Bibcode: 1994ASPC...64..405F Altcode: 1994csss....8..405F No abstract at ADS Title: A reduction package for cross-dispersed echelle spectrograph data in IDL Authors: Hall, Jeffrey C.; Neff, James E. Bibcode: 1992AAS...181.1301H Altcode: 1992BAAS...24R1139H We have written in IDL a data reduction package that performs reduction and extraction of cross-dispersed echelle spectrograph data. The present package includes a complete set of tools for extracting data from any number of spectral orders with arbitrary tilt and curvature. Essential elements include debiasing and flatfielding of the raw CCD image, removal of scattered light background, either nonoptimal or optimal extraction of data, and wavelength calibration and continuum normalization of the extracted orders. A growing set of support routines permits examination of the frame being processed to provide continuing checks on the statistical properties of the data and on the accuracy of the extraction. We will display some sample reductions and discuss the algorithms used. The inherent simplicity and user-friendliness of the IDL interface make this package a useful tool for spectroscopists. We will provide an email distribution list for those interested in receiving the package, and further documentation will be distributed at the meeting. Title: A reduction package for cross-dispersed echelle spectrograph data in IDL. Authors: Hall, J. C.; Neff, J. E. Bibcode: 1992BAAS...24Q1139H Altcode: No abstract at ADS Title: Eclipse Observations of RS CVn Binaries. I. A Survey for Extended Matter Authors: Hall, Jeffrey C.; Ramsey, Lawrence W. Bibcode: 1992AJ....104.1942H Altcode: We survey a number of RS CVn systems to determine the frequency and nature of circumstellar matter in these chromospherically active binaries. A growing body of data suggests that large extended regions of cool, prominence-like matter may be a common phenomenon in these systems. Our targets are eclipsing systems as the established geometries and occultations are useful probes for such extended material. In this paper we discuss our methods and present the results of our survey and our spectroscopic phase monitoring of these systems. We find extended material in eight of the ten systems on our present survey. Title: Optical Spectroscopy of Chromospherically Active Binary Systems in Conjunction with the ROSAT All-Sky Survey Authors: Welty, A. D.; Hall, J. C.; Patterer, R. J.; Ramsey, L. W.; Huenemoerder, D. P. Bibcode: 1992ASPC...26..116W Altcode: 1992csss....7..116W No abstract at ADS Title: A Study of Extended Matter in RS CVn Systems Authors: Hall, J. C.; Ramsey, L. W. Bibcode: 1992ASPC...26..359H Altcode: 1992csss....7..359H No abstract at ADS Title: A Spectroscopic Analysis of Extended Matter in Eclipsing RS CVN Binaries. Authors: Hall, Jeffrey Clifton Bibcode: 1991PhDT........73H Altcode: I have conducted a survey of a number of eclipsing RS CVn binaries to search for the presence of extended matter associated with the component stars. Previous evidence indicates that this extended matter is more like solar quiescent prominences than other structures such as plage; as such, it is most identifiable when viewed off the stellar limb. In eclipsing systems, the matter can be seen indirectly as it obscures a portion of the eclipsed star's limb. My survey has identified some systems in which this is the case. Parameterization of the physical extent of the extended matter is a geometrical problem wherein the amount of obscuration caused by the prominence depends on its size and orientation as well as its optical depth in the line of interest. I have done this using a Simplex algorithm which I have developed and specifically tailored to the problem at hand. I classify the extended components I have seen and discuss their effect on the spectral profiles. Other spectral diagnostics provide clues as to their origin, and I discuss this in the context of the present "solar analogy" paradigm. Title: Fixed Phase Observations of RS CVn Stars Authors: Hall, J. C.; Huenemoerder, D. P.; Ramsey, L. W.; Patterer, R. J.; Chester, M. M. Bibcode: 1990BAAS...22.1292H Altcode: No abstract at ADS Title: Fiber-optic Echelle CCD Observations of SS Bootis Authors: Hall, Jeffrey C.; Huenemoerder, David P.; Ramsey, Lawrence W.; Buzasi, Derek L. Bibcode: 1990ApJ...358..610H Altcode: The faint RS CVn system SS Bootis was observed over two seasons, and the most prominent surface activity indicators in this spectroscopically understudied object were examined. The first two Balmer lines are consistently strong in emission, as are the Ca II infrared triplet and Ca II H line; there is no significant modulation with phase in any of these lines. No excess emission is evident in He I D3. The ratio of energy emitted in H-alpha to that in H-beta is typically between three and six for the more active subgiant primary, and between two and five for the dwarf secondary. Of special interest is an excess absorption feature in the Balmer lines near primary eclipse in both seasons. The feature lies near the velocity of the secondary, and as there is no similar feature in secondary eclipse, it is suggested that it arises from obscuring material associated with the primary. From the extent of the feature and the system's geometry, limits were placed on the parameters of such material. Title: Evidence for Extended Material in the Eclipsing RS CVn System SS Bootis Authors: Hall, J. C.; Huenemoerder, D. P.; Ramsey, L. W.; Buzasi, D. L. Bibcode: 1990BAAS...22..739H Altcode: No abstract at ADS Title: Tests of a Multi-site Scintillation Gamma-Ray Detector Authors: Hall, J. C.; Agrinier, B.; Dean, J. A.; Labanti, C. Bibcode: 1990ICRC....4..171H Altcode: 1989ICRC....4..171H; 1990ICRC...21d.171H No abstract at ADS Title: MAVIS?an upper crustal seismic refraction experiment in the Midland Valley of Scotland Authors: Dentith, M. C.; Hall, J. Bibcode: 1989GeoJI..99..627D Altcode: No abstract at ADS Title: Superluminal Motion toward a Stationary Knot in the Radio Core of the Quasar 3C 395 Authors: Simon, R. S.; Hall, J.; Johnston, K. J.; Spencer, J. H.; Waak, J. A.; Mutel, R. L. Bibcode: 1988ApJ...326L...5S Altcode: We have recently confirmed that the quasar 3C 395 (1901+319) is a superluminal radio source, based upon one 18 cm and three 6 cm VLBI images of the compact radio emission in 3C 395 obtained over a 5.5 yr period. The compact structure in 3C 395 (at 6 cm with a convolving beam of 2.4 x 1.8 mas, position angle 162^deg^) is dominated by three components: (1) A bright, unresolved component to the northwest, almost certainly the central core of 3C 395. It has apparently brightened by about 0.4 Jy between 1983.3 and 1985.4, from 0.6 Jy to 1.0 Jy. (2) A moderately resolved component 15.8+/-0.2 mas to the southeast along position angle 118^deg^. The position of this component relative to the core has changed by less than 0.2 mas in 6 yr. The flux density of this component has remained nearly constant over the past 6 yr. (3) A component whose flux density has remained constant between 1983.3 and 1985.4 moving rapidly away from the core toward component 2 with a proper motion of 0.64+/-0.1 mas per year. At the distance of 3C 395 (z = 0.635), this corresponds to an apparent velocity of ~15h^-1^ c for H_0_ = 100h km s^-1^ Mpc^-1^ and q_0_ = 0.05. The object 3C 395 is unique among the dozen or so superluminals, in that on milliarcsecond scales it has a superluminal component moving between two relatively stationary components. Title: Superluminal motion towards a stationary component in quasar 3C 395. Authors: Simon, R. S.; Johnston, K. J.; Hall, J.; Spencer, J. H.; Waak, J. A. Bibcode: 1987slrs.work...72S Altcode: 3C395 has been observed to be unique among superluminals in that it has a superluminal component moving between two relatively stationary components. In this paper, VLBI observations at 6 cm are reported which confirm the three-component structure and the superluminal motion of the middle component. A speculative interpretation of the object is offered in which 3C395 is a core-jet radio source in which the jet, originating nearly along the line of sight, bends back through the line of sight. Title: Superluminal Motion in the Quasar 3C 395 Authors: Simon, R. S.; Hall, J.; Johnston, K. J.; Spencer, J. H.; Waak, J. A. Bibcode: 1986BAAS...18..993S Altcode: No abstract at ADS Title: Stabilized Lasers Authors: Baer, T.; Hall, J. Bibcode: 1981siwn.conf..142B Altcode: No abstract at ADS Title: Vp measurements on crustal xenoliths from San Juan County Utah Authors: Padovani, E. R.; Hall, J.; Simmons, G. Bibcode: 1978LPICo.329...34P Altcode: No abstract at ADS Title: Shift and Broadening of Saturated Absorption Resonances Due to Curvature of the Laser Wavefronts Authors: Hall, J.; Borde, C. Bibcode: 1976sfsm.conf..115H Altcode: No abstract at ADS Title: Direct Optical Resolution of the Recoil Effect Using Saturated Absorption Spectroscopy Authors: Hall, J.; Borde, C. Bibcode: 1976sfsm.conf..125H Altcode: No abstract at ADS Title: Discussion of the relation of palaeogene ridge and basin structures of Britain to the North Atlantic Authors: Hall, J.; Smythe, D. K. Bibcode: 1973E&PSL..19...54H Altcode: The evidence of Tertiary ridges, basins and volcanicity in Britain is at variance with a simple relation to the Atlantic opening as proposed recently by Hallam. The structural complexity of the continental margin off Britain needs further investigation before its development can be related satisfactorily to the several phases of opening of the North Atlantic. In particular, Mesozoic and Tertiary basins and ridges do not consistently show the elongation and asymmetry required by Hallam's model, and many were initiated too early to be related to the Reykjanes spreading.