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Author name code: moore-charlotte
ADS astronomy entries on 2022-09-14
author:"Moore, Charlotte E."
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Title: Results on photon-mediated dark-matter-nucleus interactions
from the PICO-60 C<SUB>3</SUB>F<SUB>8</SUB> bubble chamber
Authors: Ali, B.; Arnquist, I. J.; Baxter, D.; Behnke, E.; Bressler,
M.; Broerman, B.; Chen, C. J.; Clark, K.; Collar, J. I.; Cooper, P. S.;
Cripe, C.; Crisler, M.; Dahl, C. E.; Das, M.; Durnford, D.; Fallows,
S.; Farine, J.; Filgas, R.; García-Viltres, A.; Giroux, G.; Harris,
O.; Hillier, T.; Hoppe, E. W.; Jackson, C. M.; Jin, M.; Krauss, C. B.;
Kumar, V.; Laurin, M.; Lawson, I.; Leblanc, A.; Leng, H.; Levine, I.;
Licciardi, C.; Linden, S.; Mitra, P.; Monette, V.; Moore, C.; Neilson,
R.; Noble, A. J.; Nozard, H.; Pal, S.; Piro, M. -C.; Plante, A.;
Priya, S.; Rethmeier, C.; Robinson, A. E.; Savoie, J.; Sonnenschein,
A.; Starinski, N.; Štekl, I.; Tiwari, D.; Vázquez-Jáuregui, E.;
Wichoski, U.; Zacek, V.; Zhang, J.; PICO Collaboration
2022PhRvD.106d2004A Altcode: 2022arXiv220410340A
Many compelling models predict dark matter coupling to the
electromagnetic current through higher multipole interactions, while
remaining electrically neutral. Different multipole couplings have
been studied, among them anapole moment, electric and magnetic dipole
moments, and millicharge. This study sets limits on the couplings
for these photon-mediated interactions using nonrelativistic contact
operators in an effective field theory framework. Using data from the
PICO-60 bubble chamber leading limits for dark matter masses between
2.7 and 24 GeV /c<SUP>2</SUP> and above 265 GeV /c<SUP>2</SUP> (anapole
moment), 2.7 and 11.7 GeV /c<SUP>2</SUP> (electric moment), 3 and 9.5
GeV /c<SUP>2</SUP> (magnetic moment), and 2.7 and 12 GeV /c<SUP>2</SUP>
(millicharged) are reported for the coupling of these photon-mediated
dark matter-nucleus interactions. The detector was filled with 52 kg
of C<SUB>3</SUB>F<SUB>8</SUB> operating at thermodynamic thresholds
of 2.45 keV and 3.29 keV, reaching exposures of 1404 kg -day and 1167
kg -day , respectively.
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Title: Determining the bubble nucleation efficiency of low-energy
nuclear recoils in superheated C$_3$F$_8$ dark matter detectors
Authors: Ali, B.; Arnquist, I. J.; Baxter, D.; Behnke, E.; Bressler,
M.; Broerman, B.; Clark, K.; Collar, J. I.; Cooper, P. S.; Cripe, C.;
Crisler, M.; Dahl, C. E.; Das, M.; Durnford, D.; Fallows, S.; Farine,
J.; Filgas, R.; García-Viltres, A.; Girard, F.; Giroux, G.; Harris,
O.; Hoppe, E. W.; Jackson, C. M.; Jin, M.; Krauss, C. B.; Kumar,
V.; Lafreniere, M.; Laurin, M.; Lawson, I.; Leblanc, A.; Leng, H.;
Levine, I.; Licciardi, C.; Linden, S.; Mitra, P.; Monette, V.; Moore,
C.; Neilson, R.; Noble, A. J.; Nozard, H.; Pal, S.; Piro, M. -C.;
Plante, A.; Priya, S.; Rethmeier, C.; Robinson, A. E.; Savoie, J.;
Scallon, O.; Sonnenschein, A.; Starinski, N.; Štekl, I.; Tiwari, D.;
Tardif, F.; Vázquez-Jáuregui, E.; Wichoski, U.; Zacek, V.; Zhang, J.
2022arXiv220505771A Altcode:
The bubble nucleation efficiency of low-energy nuclear recoils in
superheated liquids plays a crucial role in interpreting results
from direct searches for weakly interacting massive particle (WIMP)
dark matter. The PICO Collaboration presents the results of the
efficiencies for bubble nucleation from carbon and fluorine recoils
in superheated C$_3$F$_8$ from calibration data taken with 5 distinct
neutron spectra at various thermodynamic thresholds ranging from 2.1
keV to 3.9 keV. Instead of assuming any particular functional forms
for the nuclear recoil efficiency, a generalized piecewise linear model
is proposed with systematic errors included as nuisance parameters to
minimize model-introduced uncertainties. A Markov-Chain Monte-Carlo
(MCMC) routine is applied to sample the nuclear recoil efficiency for
fluorine and carbon at 2.45 keV and 3.29 keV thermodynamic thresholds
simultaneously. The nucleation efficiency for fluorine was found
to be $\geq 50\, \%$ for nuclear recoils of 3.3 keV (3.7 keV) at a
thermodynamic Seitz threshold of 2.45 keV (3.29 keV), and for carbon
the efficiency was found to be $\geq 50\, \%$ for recoils of 10.6 keV
(11.1 keV) at a threshold of 2.45 keV (3.29 keV). Simulated data
sets are used to calculate a p-value for the fit, confirming that
the model used is compatible with the data. The fit paradigm is also
assessed for potential systematic biases, which although small, are
corrected for. Additional steps are performed to calculate the expected
interaction rates of WIMPs in the PICO-60 detector, a requirement for
calculating WIMP exclusion limits.
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Title: H.E.S.S. ToO program on nearby core-collapse Supernovae :
search for very-high energy gamma-ray emission towards the SN
candidate AT2019krl in M74
Authors: Hess; Abdalla, H.; Aharonian, F.; Ait-Benkhali, F.; Anguener,
O.; Arcaro, C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes,
M.; Baghmanyan, V.; Barbosa Martins, V.; Barnacka, A.; Barnard,
M.; Batzofin, R.; Becherini, Y.; Berge, D.; Bernloehr, K.; Bi, B.;
Böttcher, M.; Boisson, C.; Bolmont, J.; Bony (de), M.; Breuhaus, M.;
Brose, R.; Brun, F.; Bulik, T.; Bylund, T.; Cangemi, F.; Caroff, S.;
Casanova, S.; Catalano, J.; Chambery, P.; Chand, T. B.; Chen, A.;
Cotter, G.; Curlo, M.; Dalgleish, H.; Damascene Mbarubucyeye, J.;
Davids, I. D.; Davies, J.; Devin, J.; Djannati-Ataï, A.; Dmytriiev,
A.; Donath, A.; Doroshenko, V.; Dreyer, L.; Du Plessis, L.; Duffy,
C.; Egberts, K.; Einecke, S.; Ernenwein, J. P.; Fegan, S.; Feijen,
K.; Fiasson, A.; Fichet de Clairfontaine, G.; Fontaine, G.; Frans,
L.; Fuessling, M.; Funk, S.; Gabici, S.; Gallant, Y.; Giavitto, G.;
Giunti, L.; Glawion, D.; Glicenstein, J. F.; Grondin, M. H.; Hattingh,
S.; Haupt, M.; Hermann, G.; Hinton, J.; Hofmann, W.; Hoischen, C.;
Holch, T.; Holler, M.; Horns, D.; Huang, Z.; Huber, D.; Hörbe,
M.; Jamrozy, M.; Jankowsky, F.; Joshi, V.; Jung, I.; Kasai, E.;
Katarzynski, K.; Katz, U.; Khangulyan, D.; Khelifi, B.; Klepser, S.;
Kluzniak, W.; Komin, N.; Konno, R.; Kosack, K.; Kostunin, D.; Kreter,
M.; Kukec Mezek, G.; Kundu, A.; Lamanna, G.; Le Stum, S.; Lemiere, A.;
Lemoine-Goumard, M.; Lenain, J. P.; Leuschner, F.; Levy, C.; Lohse,
T.; Luashvili, A.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev, D.;
Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares, A.;
Marti'i-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P.; Meyer, M.;
Mitchell, A.; Moderski, R.; Mohrmann, L.; Montanari, A.; Moore, C.;
Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.; Naurois
(de), M.; Nayerhoda, A.; Davids, H.; Niemiec, J.; Noel, A.; O'Brien,
P.; Oberholzer, L. L.; Ohm, S.; Olivera-Nieto, L.; Ona-Wilhelmi (de),
E.; Ostrowski, M.; Panny, S.; Panter, M.; Parsons, D.; Peron, G.;
Pita, S.; Poireau, V.; Prokhorov, D.; Prokoph, H.; Puehlhofer, G.;
Punch, M.; Quirrenbach, A.; Reichherzer, P.; Reimer, A.; Reimer, O.;
Remy, Q.; Renaud, M.; Reville, B.; Rieger, F.; Romoli, C.; Rowell,
G.; Rudak, B.; Rueda Ricarte, H.; Ruiz Velasco, E.; Sahakian, V.;
Sailer, S.; Salzmann, H.; Sanchez, D.; Santangelo, A.; Sasaki, M.;
Schaefer, J.; Schutte, H.; Schwanke, U.; Schüssler, F.; Senniappan,
M.; Seyffert, A.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.;
Sinha, A.; Sol, H.; Spackman, H.; Specovius, A.; Spencer, S. T.;
Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steinmassl,
S.; Steppa, C.; Sun, L.; Takahashi, T.; Tanaka, T.; Tavernier, T.;
Taylor, A.; Terrier, R.; Thiersen, H.; Thorpe-Morgan, C.; Tluczykont,
M.; Tomankova, L.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.;
van der Walt, J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.;
Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Völk,
H. J.; Wagner, S.; Watson, J. J.; Werner, F.; White, R.; Wierzcholska,
A.; Wong, Y. W.; Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin, R.;
Zargaryan, D.; Zdziarski, A.; Zech, A.; Zhu, S.; Zmija, A.; Zouari,
S.; Żywucka, N.; Ryder, S.
2022icrc.confE.809H Altcode: 2021arXiv210803839K; 2022PoS...395E.809H
While the youngest known supernova remnants, such as Cassiopeia A,
have been proven to be able to accelerate cosmic rays only up to
$\sim$10$^{14}\,\mathrm{eV}$ at their present evolutionary stages,
recent studies have shown that particle energies larger than a
few PeV ($10^{15}\,\mathrm{eV}$) could be reached during the early
stages of a core-collapse Supernova, when the high-velocity forward
shock expands into the dense circumstellar medium shaped by the
stellar progenitor wind. Such environments, in particular the type
IIn SNe whose progenitors may exhibit mass-loss rates as high as
$10^{-2}M_\odot\,\mathrm{yr}^{-1}$ \cite{smith14}, could thus lead
to $\gamma$-ray emission from $\pi^0$ decay in hadronic interactions,
potentially detectable with current Cherenkov telescopes at very-high
energies. Such a detection would provide direct evidence for efficient
acceleration of CR protons/nuclei in supernovae, and hence new insights
on the long-standing issue of the origin of Galactic Cosmic Rays. In
that context, the High Energy Stereoscopic System (\hess) has been
carrying out a Target of Opportunity program since 2016 to search
for such an early very-high-energy $\gamma$-ray emission towards
nearby core-collapse supernovae and supernova candidates (up to $\sim
10~\mathrm{Mpc}$), within a few weeks after discovery. After giving an
overview of this \hess\ Target of Opportunity program, we present the
results obtained from the July 2019 observations towards the transient
\at, originally classified as a type IIn supernova, which occurred in
the galaxy M74 at $\sim 9.8\,\mathrm{Mpc}$. Although its nature still
remains unclear, the derived \hess\ constraints on this transient are
placed in the general context of the expected VHE $\gamma$-ray emission
from core-collapse supernovae.
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Title: Astronomy outreach in Namibia: H.E.S.S. and beyond
Authors: Dalgleish, H.; Prokoph, H.; Zhu, S.; Backes, M.; Cotter, G.;
Catalano, J.; Ruiz Velasco, E.; Kasai, E.; Abdalla, H.; Aharonian, F.;
Ait-Benkhali, F.; Anguener, O.; Arcaro, C.; Armand, C.; Armstrong,
T.; Ashkar, H.; Baghmanyan, V.; Barbosa Martins, V.; Barnacka, A.;
Barnard, M.; Batzofin, R.; Becherini, Y.; Berge, D.; Bernloehr, K.; Bi,
B.; Böttcher, M.; Boisson, C.; Bolmont, J.; Bony (de), M.; Breuhaus,
M.; Brose, R.; Brun, F.; Bulik, T.; Bylund, T.; Cangemi, F.; Caroff,
S.; Casanova, S.; Catalano, J.; Chambery, P.; Chand, T. B.; Chen,
A.; Curlo, M.; Damascene Mbarubucyeye, J.; Davids, I. D.; Davies, J.;
Devin, J.; Djannati-Ataï, A.; Dmytriiev, A.; Donath, A.; Doroshenko,
V.; Dreyer, L.; Du Plessis, L.; Duffy, C.; Egberts, K.; Einecke,
S.; Ernenwein, J. P.; Fegan, S.; Feijen, K.; Fiasson, A.; Fichet
de Clairfontaine, G.; Fontaine, G.; Frans, L.; Fuessling, M.; Funk,
S.; Gabici, S.; Gallant, Y.; Giavitto, G.; Giunti, L.; Glawion, D.;
Glicenstein, J. F.; Grondin, M. H.; Hattingh, S.; Haupt, M.; Hermann,
G.; Hinton, J.; Hofmann, W.; Hoischen, C.; Holch, T.; Holler, M.;
Horns, D.; Huang, Z.; Huber, D.; Hörbe, M.; Jamrozy, M.; Jankowsky,
F.; Joshi, V.; Jung, I.; Katarzynski, K.; Katz, U.; Khangulyan,
D.; Khelifi, B.; Klepser, S.; Kluzniak, W.; Komin, N.; Konno, R.;
Kosack, K.; Kostunin, D.; Kreter, M.; Kukec Mezek, G.; Kundu, A.;
Lamanna, G.; Le Stum, S.; Lemiere, A.; Lemoine-Goumard, M.; Lenain,
J. P.; Leuschner, F.; Levy, C.; Lohse, T.; Luashvili, A.; Lypova, I.;
Mackey, J.; Majumdar, J.; Malyshev, D.; Malyshev, D.; Marandon, V.;
Marchegiani, P.; Marcowith, A.; Mares, A.; Marti'i-Devesa, G.; Marx,
R.; Maurin, G.; Meintjes, P.; Meyer, M.; Mitchell, A.; Moderski, R.;
Mohrmann, L.; Montanari, A.; Moore, C.; Morris, P.; Moulin, E.; Muller,
J.; Murach, T.; Nakashima, K.; Naurois (de), M.; Nayerhoda, A.; Davids,
H.; Niemiec, J.; Noel, A.; O'Brien, P.; Oberholzer, L. L.; Ohm, S.;
Olivera-Nieto, L.; Ona-Wilhelmi (de), E.; Ostrowski, M.; Panny, S.;
Panter, M.; Parsons, D.; Peron, G.; Pita, S.; Poireau, V.; Prokhorov,
D.; Puehlhofer, G.; Punch, M.; Quirrenbach, A.; Reichherzer, P.;
Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Reville, B.; Rieger,
F.; Romoli, C.; Rowell, G.; Rudak, B.; Rueda Ricarte, H.; Sahakian,
V.; Sailer, S.; Salzmann, H.; Sanchez, D.; Santangelo, A.; Sasaki, M.;
Schaefer, J.; Schutte, H.; Schwanke, U.; Schüssler, F.; Senniappan,
M.; Seyffert, A.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.;
Sinha, A.; Sol, H.; Spackman, H.; Specovius, A.; Spencer, S. T.;
Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steinmassl,
S.; Steppa, C.; Sun, L.; Takahashi, T.; Tanaka, T.; Tavernier, T.;
Taylor, A.; Terrier, R.; Thiersen, H.; Thorpe-Morgan, C.; Tluczykont,
M.; Tomankova, L.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.;
van der Walt, J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.;
Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Völk,
H. J.; Wagner, S.; Watson, J. J.; Werner, F.; White, R.; Wierzcholska,
A.; Wong, Y. W.; Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin,
R.; Zargaryan, D.; Zdziarski, A.; Zech, A.; Zmija, A.; Zouari, S.;
Żywucka, N.
2022icrc.confE1397D Altcode: 2021arXiv210801379D; 2022PoS...395E1397D
Astronomy plays a major role in the scientific landscape of
Namibia. Because of its excellent sky conditions, Namibia is home to
ground-based observatories like the High Energy Spectroscopic System
(H.E.S.S.), in operation since 2002. Located near the Gamsberg mountain,
H.E.S.S. performs groundbreaking science by detecting very-high-energy
gamma rays from astronomical objects. The fascinating stories behind
many of them are featured regularly in the “Source of the Month”,
a blog-like format intended for the general public with more than
170 features to date. In addition to other online communication via
social media, H.E.S.S. outreach activities have been covered locally,
e.g. through `open days' and guided tours on the H.E.S.S. site
itself. An overview of the H.E.S.S. outreach activities are presented
in this contribution, along with discussions relating to the current
landscape of astronomy outreach and education in Namibia. There
has also been significant activity in the country in recent months,
whereby astronomy is being used to further sustainable development via
human capacity-building. Finally, as we take into account the future
prospects of radio astronomy in the country, momentum for a wider
range of astrophysics research is clearly building -- this presents
a great opportunity for the astronomy community to come together to
capitalise on this movement and support astronomy outreach, with the
overarching aim to advance sustainable development in Namibia.
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Title: Combined dark matter searches towards dwarf spheroidal galaxies
with Fermi-LAT, HAWC, H.E.S.S., MAGIC, and VERITAS
Authors: Armand, C.; Moulin, E.; Poireau, V.; Harding, J. P.;
Tollefson, K.; Giuri, C.; Pueschel, E.; Hess; Abdalla, H.; Aharonian,
F.; Ait-Benkhali, F.; Anguener, O.; Arcaro, C.; Armstrong, T.;
Ashkar, H.; Backes, M.; Barbosa Martins, V.; Barnacka, A.; Barnard,
M.; Batzofin, R.; Becherini, Y.; Berge, D.; Bernloehr, K.; Bi, B.;
Böttcher, M.; Boisson, C.; Bolmont, J.; Bony (de), M.; Breuhaus,
M.; Brose, R.; Brun, F.; Bulik, T.; Bylund, T.; Cangemi, F.; Caroff,
S.; Catalano, J.; Chambery, P.; Chand, T. B.; Chen, A.; Cotter, G.;
Curlo, M.; Dalgleish, H.; Damascene Mbarubucyeye, J.; Davids, I. D.;
Davies, J.; Devin, J.; Djannati-Ataï, A.; Dmytriiev, A.; Donath, A.;
Doroshenko, V.; Dreyer, L.; Du Plessis, L.; Duffy, C.; Egberts, K.;
Einecke, S.; Ernenwein, J. P.; Fegan, S.; Feijen, K.; Fiasson, A.;
Fichet de Clairfontaine, G.; Fontaine, G.; Frans, L.; Fuessling, M.;
Funk, S.; Gabici, S.; Gallant, Y.; Giavitto, G.; Giunti, L.; Glawion,
D.; Glicenstein, J. F.; Grondin, M. H.; Hattingh, S.; Haupt, M.;
Hermann, G.; Hofmann, W.; Hoischen, C.; Holch, T.; Holler, M.; Horns,
D.; Huang, Z.; Huber, D.; Hörbe, M.; Jamrozy, M.; Jankowsky, F.; Jung,
I.; Kasai, E.; Katarzynski, K.; Katz, U.; Khangulyan, D.; Khelifi, B.;
Klepser, S.; Kluzniak, W.; Komin, N.; Konno, R.; Kosack, K.; Kostunin,
D.; Kreter, M.; Kukec Mezek, G.; Kundu, A.; Lamanna, G.; Le Stum, S.;
Lemiere, A.; Lemoine-Goumard, M.; Lenain, J. P.; Leuschner, F.; Levy,
C.; Lohse, T.; Luashvili, A.; Lypova, I.; Mackey, J.; Majumdar, J.;
Malyshev, D.; Malyshev, D.; Marchegiani, P.; Marcowith, A.; Mares, A.;
Marti'i-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P.; Meyer, M.;
Mitchell, A.; Moderski, R.; Mohrmann, L.; Montanari, A.; Moore, C.;
Morris, P.; Muller, J.; Murach, T.; Nakashima, K.; Naurois (de), M.;
Davids, H.; Niemiec, J.; Noel, A.; O'Brien, P.; Oberholzer, L. L.;
Ohm, S.; Ona-Wilhelmi (de), E.; Ostrowski, M.; Panny, S.; Panter,
M.; Parsons, D.; Peron, G.; Pita, S.; Prokhorov, D.; Prokoph, H.;
Puehlhofer, G.; Punch, M.; Quirrenbach, A.; Reichherzer, P.; Reimer,
A.; Reimer, O.; Remy, Q.; Renaud, M.; Reville, B.; Rieger, F.;
Romoli, C.; Rowell, G.; Rudak, B.; Rueda Ricarte, H.; Ruiz Velasco,
E.; Sahakian, V.; Sailer, S.; Salzmann, H.; Sanchez, D.; Santangelo,
A.; Sasaki, M.; Schaefer, J.; Schutte, H.; Schwanke, U.; Schüssler,
F.; Senniappan, M.; Seyffert, A.; Shapopi, J. N. S.; Shiningayamwe,
K.; Simoni, R.; Sinha, A.; Sol, H.; Spackman, H.; Specovius, A.;
Spencer, S. T.; Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann,
C.; Steinmassl, S.; Steppa, C.; Sun, L.; Takahashi, T.; Tanaka, T.;
Tavernier, T.; Taylor, A.; Terrier, R.; Thiersen, H.; Thorpe-Morgan,
C.; Tluczykont, M.; Tomankova, L.; Tsirou, M.; Tsuji, N.; Tuffs, R.;
Uchiyama, Y.; van der Walt, J.; van Eldik, C.; van Rensburg, C.; van
Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink,
J.; Völk, H. J.; Wagner, S.; Watson, J. J.; White, R.; Wierzcholska,
A.; Wong, Y. W.; Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin, R.;
Zargaryan, D.; Zdziarski, A.; Zech, A.; Zhu, S.; Zmija, A.; Zouari,
S.; Żywucka, N.; Hawc; Abeysekara, A. U.; Albert, A.; Alfaro, R.;
Alvarez, C.; Álvarez Romero, J. d. D.; Camacho, J. R. Angeles;
Arteaga Velazquez, J. C.; Kollamparambil, A. B.; Avila Rojas, D. O.;
Ayala Solares, H. A.; Babu, R.; Baghmanyan, V.; Barber, A. S.; Becerra
González, J.; Belmont-Moreno, E.; BenZvi, S.; Berley, D.; Brisbois,
C.; Caballero Mora, K. S.; Capistrán Rojas, T.; Carramiñana, A.;
Casanova, S.; Chaparro-Amaro, O.; Cotti, U.; Cotzomi, J.; Coutiño de
Leon, S.; de la Fuente, E.; de León, C. L.; Diaz, L.; Diaz Hernandez,
R.; Díaz Vélez, J. C.; Dingus, B.; Durocher, M.; DuVernois, M.;
Ellsworth, R.; Engel, K.; Espinoza Hernández, M. C.; Fan, J.;
Fang, K.; Fernandez Alonso, M.; Fick, B.; Fleischhack, H.; Flores,
J. L.; Fraija, N. I.; Garcia Aguilar, D.; Garcia-Gonzalez, J. A.;
García-Luna, J. L.; García-Torales, G.; Garfias, F.; Giacinti, G.;
Goksu, H.; González, M. M.; Goodman, J. A.; Hernández Cadena, S.;
Herzog, I.; Hinton, J.; Huang, D.; Hueyotl-Zahuantitla, F.; Hui, M.;
Humensky, B.; Hüntemeyer, P.; Iriarte, A.; Jardin-Blicq, A.; Jhee,
H.; Joshi, V.; Kunde, G. J.; Kunwar, S.; Lara, A.; Lee, J.; Lee,
W. H.; Lennarz, D.; Vargas, H. Leon; Linnemann, J.; Longinotti, A. L.;
López-Coto, R.; Luis-Raya, G.; Lundeen, J.; Malone, K.; Marandon,
V.; Martinez, O.; Martinez Castellanos, I.; Martínez Huerta, H.;
Martínez-Castro, J.; Matthews, J.; McEnery, J.; Miranda-Romagnoli,
P.; Morales Soto, J. A.; Moreno Barbosa, E.; Mostafa, M.; Nayerhoda,
A.; Nellen, L.; Newbold, M.; Nisa, M. U.; Noriega-Papaqui, R.;
Olivera-Nieto, L.; Omodei, N.; Peisker, A.; Pérez Araujo, Y.;
Pérez Pérez, E. G.; Rho, C. D.; Rivière, C.; Rosa-Gonzalez, D.;
Ruiz-Velasco, E.; Salazar, H. I.; Salesa Greus, F.; Sandoval, A.;
Schneider, M.; Schoorlemmer, H.; Serna-Franco, J.; Sinnis, G.; Smith,
A. J.; Springer, W. R.; Surajbali, P.; Taboada, I.; Tanner, M.; Torres,
I.; Torres Escobedo, R.; Turner, R.; Ureña-Mena, F.; Villaseñor,
L.; Wang, X.; Watson, I. J.; Weisgarber, T.; Werner, F.; Willox,
E.; Wood, J.; Yodh, G.; Zepeda, A.; Zhou, H.; Veritas; Capasso, M.;
Ong, R.; Sadeh, I.; Kaaret, P.; Jin, W.; Benbow, W.; Mukherjee, R.;
Prado, R.; Lundy, M.; Patel, S.; Moriarty, P.; Maier, G.; Furniss,
A.; Ragan, K.; Williams, D.; Buckley, J.; Fortson, L.; Quinn, J.;
Holder, J.; Nieto, D.; Adams, C.; O'Brien, S.; Ribeiro, D.; Pfrang,
K.; Gueta, O.; Foote, G.; Weinstein, A.; Kumar, S.; Williamson, T.;
Tak, D.; McGrath, C.; Kleiner, T.; Pohl, M.; Reynolds, P.; Hona, B.;
Hanna, D.; Santander, M.; Sembroski, G.; Patel, S. R.; Errando, M.;
Kertzman, M.; Hervet, O.; Nievas-Rosillo, M.; Lang, M.; Roache, E.;
Humensky, T. B.; Shang, R. Y.; Vassiliev, V.; Chromey, A.; Falcone,
A.; Christiansen, J.; Otte, A.; Gent, A. E.; Brill, A.; Ryan, J.;
Farrell, K.; Gillanders, G.; Feng, Q.; Archer, A.; Kieda, D.
2022icrc.confE.528A Altcode: 2021arXiv210813646A; 2022PoS...395E.528A
Cosmological and astrophysical observations suggest that 85\% of the
total matter of the Universe is made of Dark Matter (DM). However,
its nature remains one of the most challenging and fundamental open
questions of particle physics. Assuming particle DM, this exotic
form of matter cannot consist of Standard Model (SM) particles. Many
models have been developed to attempt unraveling the nature of DM such
as Weakly Interacting Massive Particles (WIMPs), the most favored
particle candidates. WIMP annihilations and decay could produce SM
particles which in turn hadronize and decay to give SM secondaries such
as high energy $\gamma$ rays. In the framework of indirect DM search,
observations of promising targets are used to search for signatures of
DM annihilation. Among these, the dwarf spheroidal galaxies (dSphs)
are commonly favored owing to their expected high DM content and
negligible astrophysical background. In this work, we present the very
first combination of 20 dSph observations, performed by the Fermi-LAT,
HAWC, H.E.S.S., MAGIC, and VERITAS collaborations in order to maximize
the sensitivity of DM searches and improve the current results. We
use a joint maximum likelihood approach combining each experiment's
individual analysis to derive more constraining upper limits on the
WIMP DM self-annihilation cross-section as a function of DM particle
mass. We present new DM constraints over the widest mass range ever
reported, extending from 5 GeV to 100 TeV thanks to the combination
of these five different $\gamma$-ray instruments.
---------------------------------------------------------
Title: The young massive stellar cluster Westerlund 1 in gamma rays
as seen with H.E.S.S.
Authors: Mohrmann, L.; Ohm, S.; Rauth, R.; Specovius, A.; van Eldik,
C.; Abdalla, H.; Aharonian, F.; Ait-Benkhali, F.; Anguener, O.; Arcaro,
C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes, M.; Baghmanyan,
V.; Barbosa Martins, V.; Barnacka, A.; Barnard, M.; Batzofin, R.;
Becherini, Y.; Berge, D.; Bernloehr, K.; Bi, B.; Böttcher, M.;
Boisson, C.; Bolmont, J.; Bony (de), M.; Breuhaus, M.; Brose, R.;
Brun, F.; Bulik, T.; Bylund, T.; Cangemi, F.; Caroff, S.; Casanova,
S.; Catalano, J.; Chambery, P.; Chand, T. B.; Chen, A.; Cotter, G.;
Curlo, M.; Dalgleish, H.; Damascene Mbarubucyeye, J.; Davids, I. D.;
Davies, J.; Devin, J.; Djannati-Ataï, A.; Dmytriiev, A.; Donath,
A.; Doroshenko, V.; Dreyer, L.; Du Plessis, L.; Duffy, C.; Egberts,
K.; Einecke, S.; Ernenwein, J. P.; Fegan, S.; Feijen, K.; Fiasson,
A.; Fichet de Clairfontaine, G.; Fontaine, G.; Frans, L.; Fuessling,
M.; Funk, S.; Gabici, S.; Gallant, Y.; Giavitto, G.; Giunti, L.;
Glawion, D.; Glicenstein, J. F.; Grondin, M. H.; Hattingh, S.; Haupt,
M.; Hermann, G.; Hinton, J.; Hofmann, W.; Hoischen, C.; Holch, T.;
Holler, M.; Horns, D.; Huang, Z.; Huber, D.; Hörbe, M.; Jamrozy,
M.; Jankowsky, F.; Joshi, V.; Jung, I.; Kasai, E.; Katarzynski,
K.; Katz, U.; Khangulyan, D.; Khelifi, B.; Klepser, S.; Kluzniak,
W.; Komin, N.; Konno, R.; Kosack, K.; Kostunin, D.; Kreter, M.;
Kukec Mezek, G.; Kundu, A.; Lamanna, G.; Le Stum, S.; Lemiere, A.;
Lemoine-Goumard, M.; Lenain, J. P.; Leuschner, F.; Levy, C.; Lohse,
T.; Luashvili, A.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev,
D.; Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith, A.;
Mares, A.; Marti'i-Devesa, G.; Marx, R.; Maurin, G.; Meintjes,
P.; Meyer, M.; Mitchell, A.; Moderski, R.; Montanari, A.; Moore,
C.; Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.;
Naurois (de), M.; Nayerhoda, A.; Davids, H.; Niemiec, J.; Noel, A.;
O'Brien, P.; Oberholzer, L. L.; Olivera-Nieto, L.; Ona-Wilhelmi (de),
E.; Ostrowski, M.; Panny, S.; Panter, M.; Parsons, D.; Peron, G.;
Pita, S.; Poireau, V.; Prokhorov, D.; Prokoph, H.; Puehlhofer, G.;
Punch, M.; Quirrenbach, A.; Reichherzer, P.; Reimer, A.; Reimer, O.;
Remy, Q.; Renaud, M.; Reville, B.; Rieger, F.; Romoli, C.; Rowell,
G.; Rudak, B.; Rueda Ricarte, H.; Ruiz Velasco, E.; Sahakian, V.;
Sailer, S.; Salzmann, H.; Sanchez, D.; Santangelo, A.; Sasaki, M.;
Schaefer, J.; Schutte, H.; Schwanke, U.; Schüssler, F.; Senniappan,
M.; Seyffert, A.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.;
Sinha, A.; Sol, H.; Spackman, H.; Spencer, S. T.; Spir-Jacob, M.;
Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steinmassl, S.; Steppa, C.;
Sun, L.; Takahashi, T.; Tanaka, T.; Tavernier, T.; Taylor, A.; Terrier,
R.; Thiersen, H.; Thorpe-Morgan, C.; Tluczykont, M.; Tomankova, L.;
Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, J.;
van Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter,
C.; Vincent, P.; Vink, J.; Völk, H. J.; Wagner, S.; Watson, J. J.;
Werner, F.; White, R.; Wierzcholska, A.; Wong, Y. W.; Yassin, H.;
Yusafzai, A.; Zacharias, M.; Zanin, R.; Zargaryan, D.; Zdziarski,
A.; Zech, A.; Zhu, S.; Zmija, A.; Zouari, S.; Żywucka, N.
2022icrc.confE.789M Altcode: 2021arXiv210803003M; 2022PoS...395E.789M
Massive stellar clusters have recently been hypothesised as
candidates for the acceleration of hadronic cosmic rays up to PeV
energies. Previously, the H.E.S.S. Collaboration has reported about very
extended $\gamma$-ray emission around Westerlund 1, a massive young
stellar cluster in the Milky Way. In this contribution we present an
updated analysis that employs a new analysis technique and is based on
a much larger data set, allowing us to constrain better the morphology
and the energy spectrum of the emission. The analysis technique used
is a three-dimensional likelihood analysis, which is especially well
suited for largely extended sources. The origin of the $\gamma$-ray
emission will be discussed in light of multi-wavelength observations.
---------------------------------------------------------
Title: Search for dark matter annihilation signals from unidentified
Fermi-LAT objects with H.E.S.S.
Authors: Montanari, A.; Moulin, E.; Glawion, D.; Hess; Abdalla, H.;
Aharonian, F.; Ait-Benkhali, F.; Anguener, O.; Arcaro, C.; Armand, C.;
Armstrong, T.; Ashkar, H.; Backes, M.; Baghmanyan, V.; Barbosa Martins,
V.; Barnacka, A.; Barnard, M.; Batzofin, R.; Becherini, Y.; Berge,
D.; Bernloehr, K.; Bi, B.; Böttcher, M.; Boisson, C.; Bolmont, J.;
Bony (de), M.; Breuhaus, M.; Brose, R.; Brun, F.; Bulik, T.; Bylund,
T.; Cangemi, F.; Caroff, S.; Casanova, S.; Catalano, J.; Chambery,
P.; Chand, T. B.; Chen, A.; Cotter, G.; Curlo, M.; Dalgleish, H.;
Damascene Mbarubucyeye, J.; Davids, I. D.; Davies, J.; Devin, J.;
Djannati-Ataï, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.; Dreyer,
L.; Du Plessis, L.; Duffy, C.; Egberts, K.; Einecke, S.; Ernenwein,
J. P.; Fegan, S.; Feijen, K.; Fiasson, A.; Fichet de Clairfontaine,
G.; Fontaine, G.; Frans, L.; Fuessling, M.; Funk, S.; Gabici, S.;
Gallant, Y.; Giavitto, G.; Giunti, L.; Glicenstein, J. F.; Grondin,
M. H.; Hattingh, S.; Haupt, M.; Hermann, G.; Hinton, J.; Hofmann, W.;
Hoischen, C.; Holch, T.; Holler, M.; Horns, D.; Huang, Z.; Huber, D.;
Hörbe, M.; Jamrozy, M.; Jankowsky, F.; Joshi, V.; Jung, I.; Kasai,
E.; Katarzynski, K.; Katz, U.; Khangulyan, D.; Khelifi, B.; Klepser,
S.; Kluzniak, W.; Komin, N.; Konno, R.; Kosack, K.; Kostunin, D.;
Kreter, M.; Kukec Mezek, G.; Kundu, A.; Lamanna, G.; Le Stum, S.;
Lemiere, A.; Lemoine-Goumard, M.; Lenain, J. P.; Leuschner, F.; Levy,
C.; Lohse, T.; Luashvili, A.; Lypova, I.; Mackey, J.; Majumdar, J.;
Malyshev, D.; Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith,
A.; Mares, A.; Marti'i-Devesa, G.; Marx, R.; Maurin, G.; Meintjes,
P.; Meyer, M.; Mitchell, A.; Moderski, R.; Mohrmann, L.; Moore, C.;
Morris, P.; Muller, J.; Murach, T.; Nakashima, K.; Naurois (de),
M.; Nayerhoda, A.; Davids, H.; Niemiec, J.; Noel, A.; O'Brien, P.;
Oberholzer, L. L.; Ohm, S.; Olivera-Nieto, L.; Ona-Wilhelmi (de), E.;
Ostrowski, M.; Panny, S.; Panter, M.; Parsons, D.; Peron, G.; Pita, S.;
Poireau, V.; Prokhorov, D.; Prokoph, H.; Puehlhofer, G.; Punch, M.;
Quirrenbach, A.; Reichherzer, P.; Reimer, A.; Reimer, O.; Remy, Q.;
Renaud, M.; Reville, B.; Rieger, F.; Romoli, C.; Rowell, G.; Rudak,
B.; Rueda Ricarte, H.; Ruiz Velasco, E.; Sahakian, V.; Sailer, S.;
Salzmann, H.; Sanchez, D.; Santangelo, A.; Sasaki, M.; Schaefer, J.;
Schutte, H.; Schwanke, U.; Schüssler, F.; Senniappan, M.; Seyffert,
A.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.; Sinha, A.;
Sol, H.; Spackman, H.; Specovius, A.; Spencer, S. T.; Spir-Jacob, M.;
Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steinmassl, S.; Steppa, C.;
Sun, L.; Takahashi, T.; Tanaka, T.; Tavernier, T.; Taylor, A.; Terrier,
R.; Thiersen, H.; Thorpe-Morgan, C.; Tluczykont, M.; Tomankova, L.;
Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, J.;
van Eldik, C.; van Rensburg, C.; van Soelen, B.; Vasileiadis, G.;
Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Völk, H. J.; Wagner, S.;
Watson, J. J.; Werner, F.; White, R.; Wierzcholska, A.; Wong, Y. W.;
Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin, R.; Zargaryan, D.;
Zdziarski, A.; Zech, A.; Zhu, S.; Zmija, A.; Zouari, S.; Żywucka, N.
2022icrc.confE.538M Altcode: 2021arXiv210901498M; 2022PoS...395E.538M
Cosmological N-body simulations show that Milky-Way-sized galaxies
harbor a population of unmerged dark matter subhalos. These subhalos
could shine in gamma rays and be eventually detected in gamma-ray
surveys as unidentified sources. We search for very-high-energy (VHE,
$E\geq 100$ GeV) gamma-ray emission using H.E.S.S. observations
carried out from a thorough selection of unidentified Fermi-LAT
Objects (UFOs) as dark matter subhalo candidates. Provided that the
dark matter mass is higher than a few hundred GeV, the emission of
the UFOs can be well described by dark matter annihilation models. No
significant VHE gamma-ray emission is detected in any UFO dataset
nor in their combination. We, therefore, derive constraints on the
product of the velocity-weighted annihilation cross-section $\langle
\sigma v\rangle$ by the $J$-factor on dark matter models describing
the UFO emissions. Upper limits at 95% confidence level are derived
on $\langle \sigma v\rangle J$ in $W^+W^-$ and $\tau^+\tau^-$
annihilation channels for the TeV dark matter particles. Focusing
on thermal WIMPs, strong constraints on the $J$-factors are obtained
from H.E.S.S. observations. Adopting model-dependent predictions from
cosmological N-body simulations on the $J$-factor distribution function
for Milky Way (MW)-sized galaxies, only $\lesssim 0.3$ TeV mass dark
matter models marginally allow to explain observed UFO emission.
---------------------------------------------------------
Title: Detection of new Extreme BL Lac objects with H.E.S.S. and
Swift XRT
Authors: Bony (de), M.; Bylund, T.; Meyer, M.; Noel, A. P.; Sanchez,
D.; Abdalla, H.; Aharonian, F.; Ait-Benkhali, F.; Anguener, O.; Arcaro,
C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes, M.; Baghmanyan,
V.; Barbosa Martins, V.; Barnacka, A.; Barnard, M.; Batzofin, R.;
Becherini, Y.; Berge, D.; Bernloehr, K.; Bi, B.; Böttcher, M.;
Boisson, C.; Bolmont, J.; Breuhaus, M.; Brose, R.; Brun, F.; Bulik,
T.; Cangemi, F.; Caroff, S.; Casanova, S.; Catalano, J.; Chambery,
P.; Chand, T. B.; Chen, A.; Cotter, G.; Curlo, M.; Dalgleish, H.;
Damascene Mbarubucyeye, J.; Davids, I. D.; Davies, J.; Devin, J.;
Djannati-Ataï, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.; Dreyer,
L.; Du Plessis, L.; Duffy, C.; Egberts, K.; Einecke, S.; Ernenwein,
J. P.; Fegan, S.; Feijen, K.; Fiasson, A.; Fichet de Clairfontaine, G.;
Fontaine, G.; Frans, L.; Fuessling, M.; Funk, S.; Gabici, S.; Gallant,
Y.; Giavitto, G.; Giunti, L.; Glawion, D.; Glicenstein, J. F.; Grondin,
M. H.; Hattingh, S.; Haupt, M.; Hermann, G.; Hinton, J.; Hofmann, W.;
Hoischen, C.; Holch, T.; Holler, M.; Horns, D.; Huang, Z.; Huber, D.;
Hörbe, M.; Jamrozy, M.; Jankowsky, F.; Joshi, V.; Jung, I.; Kasai,
E.; Katarzynski, K.; Katz, U.; Khangulyan, D.; Khelifi, B.; Klepser,
S.; Kluzniak, W.; Komin, N.; Konno, R.; Kosack, K.; Kostunin, D.;
Kreter, M.; Kukec Mezek, G.; Kundu, A.; Lamanna, G.; Le Stum, S.;
Lemiere, A.; Lemoine-Goumard, M.; Lenain, J. P.; Leuschner, F.; Levy,
C.; Lohse, T.; Luashvili, A.; Lypova, I.; Mackey, J.; Majumdar, J.;
Malyshev, D.; Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith,
A.; Mares, A.; Marti'i-Devesa, G.; Marx, R.; Maurin, G.; Meintjes,
P.; Mitchell, A.; Moderski, R.; Mohrmann, L.; Montanari, A.; Moore,
C.; Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.;
Naurois (de), M.; Nayerhoda, A.; Davids, H.; Niemiec, J.; O'Brien,
P.; Oberholzer, L. L.; Ohm, S.; Olivera-Nieto, L.; Ona-Wilhelmi (de),
E.; Ostrowski, M.; Panny, S.; Panter, M.; Parsons, D.; Peron, G.;
Pita, S.; Poireau, V.; Prokhorov, D.; Prokoph, H.; Puehlhofer, G.;
Punch, M.; Quirrenbach, A.; Reichherzer, P.; Reimer, A.; Reimer, O.;
Remy, Q.; Renaud, M.; Reville, B.; Rieger, F.; Romoli, C.; Rowell,
G.; Rudak, B.; Rueda Ricarte, H.; Ruiz Velasco, E.; Sahakian, V.;
Sailer, S.; Salzmann, H.; Santangelo, A.; Sasaki, M.; Schaefer, J.;
Schutte, H.; Schwanke, U.; Schüssler, F.; Senniappan, M.; Seyffert,
A.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.; Sinha, A.;
Sol, H.; Spackman, H.; Specovius, A.; Spencer, S. T.; Spir-Jacob, M.;
Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steinmassl, S.; Steppa, C.;
Sun, L.; Takahashi, T.; Tanaka, T.; Tavernier, T.; Taylor, A.; Terrier,
R.; Thiersen, H.; Thorpe-Morgan, C.; Tluczykont, M.; Tomankova, L.;
Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, J.;
van Eldik, C.; van Rensburg, C.; van Soelen, B.; Vasileiadis, G.;
Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Völk, H. J.; Wagner, S.;
Watson, J. J.; Werner, F.; White, R.; Wierzcholska, A.; Wong, Y. W.;
Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin, R.; Zargaryan, D.;
Zdziarski, A.; Zech, A.; Zhu, S.; Zmija, A.; Zouari, S.; Żywucka, N.
2022icrc.confE.823B Altcode: 2022PoS...395E.823B; 2021arXiv210802232D
Extreme high synchrotron peaked blazars (EHBLs) are amongst the most
powerful accelerators found in nature. Usually the synchrotron peak
frequency of an EHBL is above $10^{17}\,$Hz, i.e., lies in the range
of medium to hard X-rays making them ideal sources to study particle
acceleration and radiative processes. EHBL objects are commonly observed
at energies beyond several TeV, making them also powerful probes of
gamma-ray absorption in the intergalactic medium. During the last
decade, several attempts have been made to increase the number of EHBL
detected at TeV energies and probe their spectral characteristics. Here
we report new detections of EHBLs in the TeV energy regime, each at
a redshift of less than 0.2, by the High Energy Stereoscopic System
(H.E.S.S.). Also, we report on X-ray observations of these EHBLs
candidates with Swift XRT. In conjunction with the very high energy
observations, this allows us to probe the radiation mechanisms and
the underlying particle acceleration processes.
---------------------------------------------------------
Title: Detection of extended TeV emission around the Geminga pulsar
with H.E.S.S.
Authors: Mitchell, A.; Caroff, S.; Hinton, J.; Mohrmann, L.; Hess;
Abdalla, H.; Aharonian, F.; Ait-Benkhali, F.; Anguener, O.; Arcaro,
C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes, M.; Baghmanyan,
V.; Barbosa Martins, V.; Barnacka, A.; Barnard, M.; Batzofin, R.;
Becherini, Y.; Berge, D.; Bernloehr, K.; Bi, B.; Böttcher, M.;
Boisson, C.; Bolmont, J.; Bony (de), M.; Breuhaus, M.; Brose, R.; Brun,
F.; Bulik, T.; Bylund, T.; Cangemi, F.; Casanova, S.; Catalano, J.;
Chambery, P.; Chand, T. B.; Chen, A.; Cotter, G.; Curlo, M.; Dalgleish,
H.; Damascene Mbarubucyeye, J.; Davids, I. D.; Davies, J.; Devin, J.;
Djannati-Ataï, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.; Dreyer,
L.; Du Plessis, L.; Duffy, C.; Egberts, K.; Einecke, S.; Ernenwein,
J. P.; Fegan, S.; Feijen, K.; Fiasson, A.; Fichet de Clairfontaine,
G.; Fontaine, G.; Frans, L.; Fuessling, M.; Funk, S.; Gabici, S.;
Gallant, Y.; Giavitto, G.; Giunti, L.; Glawion, D.; Glicenstein, J. F.;
Grondin, M. H.; Hattingh, S.; Haupt, M.; Hermann, G.; Hofmann, W.;
Hoischen, C.; Holch, T.; Holler, M.; Horns, D.; Huang, Z.; Huber, D.;
Hörbe, M.; Jamrozy, M.; Jankowsky, F.; Joshi, V.; Jung, I.; Kasai,
E.; Katarzynski, K.; Katz, U.; Khangulyan, D.; Khelifi, B.; Klepser,
S.; Kluzniak, W.; Komin, N.; Konno, R.; Kosack, K.; Kostunin, D.;
Kreter, M.; Kukec Mezek, G.; Kundu, A.; Lamanna, G.; Le Stum, S.;
Lemiere, A.; Lemoine-Goumard, M.; Lenain, J. P.; Leuschner, F.; Levy,
C.; Lohse, T.; Luashvili, A.; Lypova, I.; Mackey, J.; Majumdar, J.;
Malyshev, D.; Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith,
A.; Mares, A.; Marti'i-Devesa, G.; Marx, R.; Maurin, G.; Meintjes,
P.; Meyer, M.; Moderski, R.; Montanari, A.; Moore, C.; Morris, P.;
Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.; Naurois (de),
M.; Nayerhoda, A.; Davids, H.; Niemiec, J.; Noel, A.; O'Brien, P.;
Oberholzer, L. L.; Ohm, S.; Olivera-Nieto, L.; Ona-Wilhelmi (de), E.;
Ostrowski, M.; Panny, S.; Panter, M.; Parsons, D.; Peron, G.; Pita, S.;
Poireau, V.; Prokhorov, D.; Prokoph, H.; Puehlhofer, G.; Punch, M.;
Quirrenbach, A.; Reichherzer, P.; Reimer, A.; Reimer, O.; Remy, Q.;
Renaud, M.; Reville, B.; Rieger, F.; Romoli, C.; Rowell, G.; Rudak,
B.; Rueda Ricarte, H.; Ruiz Velasco, E.; Sahakian, V.; Sailer, S.;
Salzmann, H.; Sanchez, D.; Santangelo, A.; Sasaki, M.; Schaefer, J.;
Schutte, H.; Schwanke, U.; Schüssler, F.; Senniappan, M.; Seyffert,
A.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.; Sinha, A.;
Sol, H.; Spackman, H.; Specovius, A.; Spencer, S. T.; Spir-Jacob, M.;
Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steinmassl, S.; Steppa, C.;
Sun, L.; Takahashi, T.; Tanaka, T.; Tavernier, T.; Taylor, A.; Terrier,
R.; Thiersen, H.; Thorpe-Morgan, C.; Tluczykont, M.; Tomankova, L.;
Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, J.;
van Eldik, C.; van Rensburg, C.; van Soelen, B.; Vasileiadis, G.;
Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Völk, H. J.; Wagner, S.;
Watson, J. J.; Werner, F.; White, R.; Wierzcholska, A.; Wong, Y. W.;
Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin, R.; Zargaryan, D.;
Zdziarski, A.; Zech, A.; Zhu, S.; Zmija, A.; Zouari, S.; Żywucka, N.
2022icrc.confE.780M Altcode: 2022PoS...395E.780M; 2021arXiv210802556M
Highly extended gamma-ray emission around the Geminga pulsar was
discovered by Milagro and verified by HAWC. Despite many observations
with Imaging Atmospheric Cherenkov Telescopes (IACTs), detection of
gamma-ray emission on angular scales exceeding the IACT field-of-view
has proven challenging. Recent developments in analysis techniques
have enabled the detection of significant emission around Geminga
in archival data with H.E.S.S.. In 2019, further data on the Geminga
region were obtained with an adapted observation strategy. Following
the announcement of the detection of significant TeV emission around
Geminga in archival data, in this contribution we present the detection
in an independent dataset. New analysis results will be presented,
and emphasis given to the technical challenges involved in observations
of highly extended gamma-ray emission with IACTs.
---------------------------------------------------------
Title: Search for enhanced TeV gamma ray emission from Giant Molecular
Clouds using H.E.S.S.
Authors: Sinha, A.; Baghmanyan, V.; Peron, G.; Gallant, Y.; Casanova,
S.; Holler, M.; Mitchell, A.; Żywucka, N.; Hess; Abdalla, H.;
Aharonian, F.; Ait-Benkhali, F.; Anguener, O.; Arcaro, C.; Armand, C.;
Armstrong, T.; Ashkar, H.; Backes, M.; Barbosa Martins, V.; Barnacka,
A.; Barnard, M.; Batzofin, R.; Becherini, Y.; Berge, D.; Bernloehr,
K.; Bi, B.; Böttcher, M.; Boisson, C.; Bolmont, J.; Bony (de), M.;
Breuhaus, M.; Brose, R.; Brun, F.; Bulik, T.; Bylund, T.; Cangemi,
F.; Caroff, S.; Catalano, J.; Chambery, P.; Chand, T. B.; Chen, A.;
Cotter, G.; Curlo, M.; Dalgleish, H.; Damascene Mbarubucyeye, J.;
Davids, I. D.; Davies, J.; Devin, J.; Djannati-Ataï, A.; Dmytriiev,
A.; Donath, A.; Doroshenko, V.; Dreyer, L.; Du Plessis, L.; Duffy,
C.; Egberts, K.; Einecke, S.; Ernenwein, J. P.; Fegan, S.; Feijen,
K.; Fiasson, A.; Fichet de Clairfontaine, G.; Fontaine, G.; Frans, L.;
Fuessling, M.; Funk, S.; Gabici, S.; Giavitto, G.; Giunti, L.; Glawion,
D.; Glicenstein, J. F.; Grondin, M. H.; Hattingh, S.; Haupt, M.;
Hermann, G.; Hinton, J.; Hofmann, W.; Hoischen, C.; Holch, T.; Horns,
D.; Huang, Z.; Huber, D.; Hörbe, M.; Jamrozy, M.; Jankowsky, F.;
Joshi, V.; Jung, I.; Kasai, E.; Katarzynski, K.; Katz, U.; Khangulyan,
D.; Khelifi, B.; Klepser, S.; Kluzniak, W.; Komin, N.; Konno, R.;
Kosack, K.; Kostunin, D.; Kreter, M.; Kukec Mezek, G.; Kundu, A.;
Lamanna, G.; Le Stum, S.; Lemiere, A.; Lemoine-Goumard, M.; Lenain,
J. P.; Leuschner, F.; Levy, C.; Lohse, T.; Luashvili, A.; Lypova, I.;
Mackey, J.; Majumdar, J.; Malyshev, D.; Malyshev, D.; Marandon, V.;
Marchegiani, P.; Marcowith, A.; Mares, A.; Marti'i-Devesa, G.; Marx,
R.; Maurin, G.; Meintjes, P.; Meyer, M.; Moderski, R.; Mohrmann,
L.; Montanari, A.; Moore, C.; Morris, P.; Moulin, E.; Muller, J.;
Murach, T.; Nakashima, K.; Naurois (de), M.; Nayerhoda, A.; Davids,
H.; Niemiec, J.; Noel, A.; O'Brien, P.; Oberholzer, L. L.; Ohm,
S.; Olivera-Nieto, L.; Ona-Wilhelmi (de), E.; Ostrowski, M.; Panny,
S.; Panter, M.; Parsons, D.; Pita, S.; Poireau, V.; Prokhorov, D.;
Prokoph, H.; Puehlhofer, G.; Punch, M.; Quirrenbach, A.; Reichherzer,
P.; Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Reville, B.; Rieger,
F.; Romoli, C.; Rowell, G.; Rudak, B.; Rueda Ricarte, H.; Ruiz Velasco,
E.; Sahakian, V.; Sailer, S.; Salzmann, H.; Sanchez, D.; Santangelo,
A.; Sasaki, M.; Schaefer, J.; Schutte, H.; Schwanke, U.; Schüssler,
F.; Senniappan, M.; Seyffert, A.; Shapopi, J. N. S.; Shiningayamwe,
K.; Simoni, R.; Sol, H.; Spackman, H.; Specovius, A.; Spencer, S. T.;
Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steinmassl,
S.; Steppa, C.; Sun, L.; Takahashi, T.; Tanaka, T.; Tavernier, T.;
Taylor, A.; Terrier, R.; Thiersen, H.; Thorpe-Morgan, C.; Tluczykont,
M.; Tomankova, L.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.;
van der Walt, J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.;
Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Völk,
H. J.; Wagner, S.; Watson, J. J.; Werner, F.; White, R.; Wierzcholska,
A.; Wong, Y. W.; Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin, R.;
Zargaryan, D.; Zdziarski, A.; Zech, A.; Zhu, S.; Zmija, A.; Zouari, S.
2022icrc.confE.790S Altcode: 2021arXiv210801738S; 2022PoS...395E.790S
Cosmic Ray (CR) interactions with the dense gas inside Giant Molecular
Clouds (GMCs) produce neutral pions, which in turn decay into gamma
rays. Thus, the gamma ray emission from GMCs is a direct tracer of the
cosmic ray density and the matter density inside the clouds. Detection
of enhanced TeV emission from GMCs, i.e., an emission significantly
larger than what is expected from the average Galactic cosmic rays
illuminating the cloud, can imply a variation in the local cosmic ray
density, due to, for example, the presence of a recent accelerator in
proximity to the cloud. Such gamma-ray observations can be crucial
in probing the cosmic ray distribution across our Galaxy, but are
complicated to perform with present generation Imaging Atmospheric
Cherenkov Telescopes (IACTs). These studies require differentiating
between the strong cosmic-ray induced background, the large scale
diffuse emission, and the emission from the clouds, which is difficult
to the small field of view of present generation IACTs. In this
contribution, we use H.E.S.S. data collected over 16 years to search
for TeV emission from GMCs in the inner molecular galacto-centric
ring of our Galaxy. We implement a 3D FoV likelihood technique, and
simultaneously model the hadronic background, the galactic diffuse
emission and the emission expected from known VHE sources to probe
for excess TeV gamma ray emission from GMCs.
---------------------------------------------------------
Title: Searching for VHE gamma-ray emission associated with IceCube
neutrino alerts using FACT, H.E.S.S., MAGIC, and VERITAS
Authors: The Fact Collaboration; The H. E. S. S. Collaboration;
The Icecube Collaboration; The MAGIC Collaboration; The VERITAS
Collaboration; Acciari, V. A.; Ansoldi, S.; Antonelli, L. A.; Arbet
Engels, A.; Artero, M.; Asano, K.; Baack, D.; Babic, A.; Baquero,
A.; Barres de Almeida, U.; Barrio, J. A.; Batković, I.; Becerra
Gonzalez, J.; Bednarek, W.; Bellizzi, L.; Bernardini, E.; Bernardos,
M. I.; Berti, A.; Besenrieder, J.; Bhattacharyya, W.; Bigongiari,
C.; Biland, A.; Blanch, O.; Bökenkamp, H.; Bonnoli, G.; Bosnjak,
Z.; Busetto, G.; Carosi, R.; Ceribella, G.; Cerruti, M.; Chai, Y.;
Chilingarian, A.; Cikota, S.; Colak, S. M.; Colombo, E.; Contreras,
J. L.; Cortina, J.; Covino, S.; D'Amico, G.; D'Elia, V.; da Vela,
P.; Dazzi, F.; de Angelis, A.; de Lotto, B.; Delfino, M.; Delgado,
J.; Delgado Mendez, C.; Depaoli, D.; di Pierro, F.; di Venere, L.;
Do Souto Espiñeira, E.; Dominis Prester, D.; Donini, A.; Dorner,
D.; Doro, M.; Elsaesser, D.; Fallah Ramazani, V.; Fattorini, A.;
Fonseca, M. V.; Font, L.; Fruck, C.; Fukami, S.; Fukazawa, Y.;
García López, R. J.; Garczarczyk, M.; Gasparyan, S.; Gaug, M.;
Giglietto, N.; Giordano, F.; Gliwny, P.; Godinovic, N.; Green, D.;
Green, J. G.; Hadasch, D.; Hahn, A.; Heckmann, L.; Herrera, J.;
Hoang, J.; Hrupec, D.; Hütten, M.; Inada, T.; Ishio, K.; Iwamura,
Y.; Jiménez Martínez, I.; Jormanainen, J.; Jouvin, L.; Karjalainen,
M.; Kerszberg, D.; Kobayashi, Y.; Kubo, H.; Kushida, J.; Lamastra, A.;
Lelas, D.; Leone, F.; Lindfors, E.; Linhoff, L.; Lombardi, S.; Longo,
F.; Lopez-Coto, R.; López-Moya, M.; López-Oramas, A.; Loporchio,
S.; Machado de Oliveira Fraga, B.; Maggio, C.; Majumdar, P.; Makariev,
M.; Mallamaci, M.; Maneva, G.; Manganaro, M.; Mannheim, K.; Maraschi,
L.; Mariotti, M.; Martinez, M.; Mazin, D.; Menchiari, S.; Mender, S.;
Mićanović, S.; Miceli, D.; Miener, T.; Miranda, J. M.; Mirzoyan,
R.; Molina, E.; Moralejo, A.; Morcuende, D.; Moreno, V.; Moretti,
E.; Nakamori, T.; Nava, L.; Neustroev, V.; Nigro, C.; Nilsson, K.;
Nishijima, K.; Noda, K.; Nozaki, S.; Ohtani, Y.; Oka, T.; Otero-Santos,
J.; Paiano, S.; Palatiello, M.; Paneque, D.; Paoletti, R.; Paredes,
J. M.; Pavletić, L.; Peñil, P.; Persic, M.; Pihet, M.; Prada Moroni,
P. G.; Prandini, E.; Priyadarshi, C.; Puljak, I.; Rhode, W.; Ribó,
M.; Rico, J.; Righi, C.; Rugliancich, A.; Sahakyan, N.; Saito, T.;
Sakurai, S.; Satalecka, K.; Saturni, F. G.; Schleicher, B.; Schmidt,
K.; Schweizer, T.; Sitarek, J.; Šnidarić, I.; Sobczyńska, D.;
Spolon, A.; Stamerra, A.; Strišković, J.; Strom, D.; Strzys, M.;
Suda, Y.; Surić, T.; Takahashi, M.; Takeishi, R.; Tavecchio, F.;
Temnikov, P.; Terzic, T.; Teshima, M.; Tosti, L.; Truzzi, S.; Tutone,
A.; Ubach, S.; van Scherpenberg, J.; Vanzo, G.; Vazquez Acosta, M.;
Ventura, S.; Verguilov, V.; Vigorito, C. F.; Vitale, V.; Vovk, I.;
Will, M.; Wunderlich, C.; Yamamoto, T.; Zarić, D.; Balbo, M.; Bretz,
T.; Buss, J.; Eisenberger, L.; Hildebrand, D.; Iotov, R.; Kalenski, A.;
Neise, D.; Noethe, M.; Paravac, A.; Sliusar, V.; Walter, R.; Abbasi,
R.; Ackermann, M.; Adams, J.; Aguilar, J.; Ahlers, M.; Ahrens, M.;
Alispach, C. M.; Alves Junior, A. A.; Amin, N. M. B.; An, R.; Andeen,
K.; Anderson, T.; Anton, G.; Arguelles, C.; Ashida, Y.; Axani, S.;
Bai, X.; Balagopal v., A.; Barbano, A. M.; Barwick, S. W.; Bastian,
B.; Basu, V.; Baur, S.; Bay, R. C.; Beatty, J. J.; Becker, K. H.;
Becker Tjus, J.; Bellenghi, C.; Benzvi, S.; Berley, D.; Besson,
D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Boddenberg,
M.; Bontempo, F.; Borowka, J.; Boser, S.; Botner, O.; Bottcher, J.;
Bourbeau, E.; Bradascio, F.; Braun, J.; Bron, S.; Brostean-Kaiser,
J.; Browne, S. A.; Burgman, A.; Burley, R.; Busse, R.; Campana, M.;
Carnie-Bronca, E.; Chen, C.; Chirkin, D.; Choi, K.; Clark, B.; Clark,
K.; Classen, L.; Coleman, A.; Collin, G.; Conrad, J. M.; Coppin,
P.; Correa, P.; Cowen, D. F.; Cross, R.; Dappen, C.; Dave, P.; de
Clercq, C.; Delaunay, J.; Dembinski, H.; Deoskar, K.; De Ridder, S.;
Desai, A.; Desiati, P.; de Vries, K.; de Wasseige, G.; de With, M.;
Deyoung, T.; Dharani, S.; Diaz, A.; Diaz-Velez, J. C.; Dittmer, M.;
Dujmovic, H.; Dunkman, M.; Duvernois, M.; Dvorak, E.; Ehrhardt, T.;
Eller, P.; Engel, R.; Erpenbeck, H.; Evans, J.; Evenson, P. A.; Fan,
K. L.; Fazely, A. R.; Fiedlschuster, S.; Fienberg, A.; Filimonov,
K.; Finley, C.; Fischer, L.; Fox, D. B.; Franckowiak, A.; Friedman,
E.; Fritz, A.; Furst, P.; Gaisser, T. K.; Gallagher, J.; Ganster,
E.; Garcia, A.; Garrappa, S.; Gerhardt, L.; Ghadimi, A.; Glaser, C.;
Glauch, T.; Glusenkamp, T.; Goldschmidt, A.; Gonzalez, J.; Goswami,
S.; Grant, D.; Grégoire, T.; Griswold, S.; Gunduz, M.; Günther,
C.; Haack, C.; Hallgren, A.; Halliday, R.; Halve, L.; Halzen, F.;
Minh, M. Ha; Hanson, K.; Hardin, J.; Harnisch, A. A.; Haungs, A.;
Hauser, S.; Hebecker, D.; Helbing, K.; Henningsen, F.; Hettinger,
E. C.; Hickford, S.; Hignight, J.; Hill, C.; Hill, G. C.; Hoffman, K.;
Hoffmann, R.; Hoinka, T.; Hokanson-Fasig, B.; Hoshina, K.; Huang, F.;
Huber, M.; Huber, T.; Hultqvist, K.; Hunnefeld, M.; Hussain, R.; in,
S.; Iovine, N.; Ishihara, A.; Jansson, M.; Japaridze, G.; Jeong, M.;
Jones, B.; Kang, D.; Kang, W.; Kang, X.; Kappes, A.; Kappesser, D.;
Karg, T.; Karl, M.; Karle, A.; Katz, U.; Kauer, M.; Kellermann, M.;
Kelley, J. L.; Kheirandish, A.; Kin, K. I.; Kintscher, T.; Kiryluk,
J.; Klein, S.; Koirala, R.; Kolanoski, H.; Kontrimas, T.; Kopke, L.;
Kopper, C.; Kopper, S.; Koskinen, D. J.; Koundal, P.; Kovacevich, M.;
Kowalski, M.; Kozynets, T.; Kun, E.; Kurahashi, N.; Lad, N.; Lagunas
Gualda, C.; Lanfranchi, J.; Larson, M. J.; Lauber, F. H.; Lazar,
J.; Lee, J.; Leonard, K.; Leszczyńska, A.; Li, Y.; Lincetto, M.;
Liu, Q.; Liubarska, M.; Lohfink, E.; Lozano Mariscal, C. J.; Lu, L.;
Lucarelli, F.; Ludwig, A.; Luszczak, W.; Lyu, Y.; Ma, W. Y.; Madsen,
J.; Mahn, K.; Makino, Y.; Mancina, S.; Maris, I. C.; Maruyama, R. H.;
Mase, K.; McElroy, T.; McNally, F.; Mead, J. V.; Meagher, K.;
Medina, A.; Meier, M.; Meighen-Berger, S.; Micallef, J.; Mockler, D.;
Montaruli, T.; Moore, R.; Morse, R.; Moulai, M.; Naab, R.; Nagai, R.;
Naumann, U.; Necker, J.; Nguyen, L. V.; Niederhausen, H.; Nisa, M.;
Nowicki, S.; Nygren, D.; Obertacke Pollmann, A.; Oehler, M.; Olivas,
A.; O'Sullivan, E.; Pandya, H.; Pankova, D.; Park, N.; Parker, G.;
Paudel, E. N.; Paul, L.; Perez de Los Heros, C.; Peters, L.; Philippen,
S.; Pieloth, D.; Pieper, S.; Pittermann, M.; Pizzuto, A.; Plum, M.;
Popovych, Y.; Porcelli, A.; Prado Rodriguez, M.; Price, P. B.; Pries,
B.; Przybylski, G.; Raab, C.; Raissi, A.; Rameez, M.; Rawlins, K.;
Rea, I. C.; Rehman, A.; Reimann, R.; Renzi, G.; Resconi, E.; Reusch,
S.; Richman, M.; Riedel, B.; Roberts, E.; Robertson, S.; Roellinghoff,
G.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk Cantu, D.;
Safa, I.; Saffer, J.; Sanchez Herrera, S.; Sandrock, A.; Sandroos, J.;
Santander, M.; Sarkar, S.; Sarkar, S.; Scharf, M. K.; Schaufel, M.;
Schieler, H.; Schindler, S.; Schlunder, P.; Schmidt, T.; Schneider,
A.; Schneider, J.; Schröder, F. G.; Schumacher, L. J.; Schwefer,
G.; Sclafani, S.; Seckel, D.; Seunarine, S.; Sharma, A.; Shefali, S.;
Silva, M.; Skrzypek, B.; Smithers, B.; Snihur, R.; Soedingrekso, J.;
Soldin, D.; Spannfellner, C.; Spiczak, G.; Spiering, C.; Stachurska,
J.; Stamatikos, M.; Stanev, T.; Stein, R.; Stettner, J.; Steuer, A.;
Stezelberger, T.; Sturwald, T.; Stuttard, T.; Sullivan, G. W.; Taboada,
I.; Tenholt, F.; Ter-Antonyan, S.; Tilav, S.; Tischbein, F.; Tollefson,
K.; Tönnis, C.; Toscano, S.; Tosi, D.; Trettin, A.; Tselengidou, M.;
Tung, C.; Turcati, A.; Turcotte, R.; Turley, C.; Twagirayezu, J. P.;
Ty, B.; Unland Elorrieta, M.; Valtonen-Mattila, N.; Vandenbroucke,
J.; van Eijndhoven, N.; Vannerom, D.; van Santen, J.; Verpoest, S.;
Vraeghe, M.; Walck, C.; Watson, T.; Weaver, C.; Weigel, P.; Weindl,
A.; Weiss, M.; Weldert, J.; Wendt, C.; Werthebach, J.; Weyrauch, M.;
Whitehorn, N.; Wiebusch, C. H.; Williams, D.; Wolf, M.; Woschnagg,
K.; Wrede, G.; Wulff, J.; Xu, X.; Xu, Y.; Yanez, J. P.; Yoshida, S.;
Yu, S.; Yuan, T.; Zhang, Z.; Jin, W.; Abdalla, H.; Aharonian, F.;
Ait-Benkhali, F.; Anguener, O.; Arcaro, C.; Armand, C.; Armstrong, T.;
Ashkar, H.; Backes, M.; Baghmanyan, V.; Barbosa Martins, V.; Barnacka,
A.; Barnard, M.; Batzofin, R.; Becherini, Y.; Berge, D.; Bernlöhr, K.;
Bi, B.; Böttcher, M.; Boisson, C.; Bolmont, J.; de Bony, M.; Breuhaus,
M.; Brose, R.; Brun, F.; Bulik, T.; Bylund, T.; Cangemi, F.; Caroff,
S.; Casanova, S.; Catalano, J.; Chambery, P.; Chand, T. B.; Chen, A.;
Cotter, G.; Curlo, M.; Damascene Mbarubucyeye, J.; Davids, I. D.;
Davies, J.; Devin, J.; Djannati-Ataï, A.; Dmytriiev, A.; Donath,
A.; Doroshenko, V.; Dreyer, L.; Du Plessis, L.; Duffy, C.; Egberts,
K.; Einecke, S.; Emery, G.; Ernenwein, J. P.; Fegan, S.; Feijen, K.;
Fiasson, A.; Fichet de Clairfontaine, G.; Fontaine, G.; Frans, L.;
Fuessling, M.; Funk, S.; Gabici, S.; Gallant, Y.; Ghafourizade, S.;
Giavitto, G.; Giunti, L.; Glawion, D.; Glicenstein, J. F.; Grondin,
M. H.; Hattingh, S.; Haupt, M.; Hermann, G.; Hinton, J.; Hofmann, W.;
Hoischen, C.; Holch, T.; Holler, M.; Horns, D.; Huang, Z.; Huber, D.;
Hörbe, M.; Jamrozy, M.; Jankowsky, F.; Joshi, V.; Jung, I.; Kasai, E.;
Katarzynski, K.; Katz, U.; Khangulyan, D.; Khelifi, B.; Klepser, S.;
Kluzniak, W.; Komin, N.; Konno, R.; Kosack, K.; Kostunin, D.; Kreter,
M.; Kukec Mezek, G.; Kundu, A.; Lamanna, G.; Le Stum, S.; Lemiere, A.;
Lemoine-Goumard, M.; Lenain, J. P.; Leuschner, F.; Levy, C.; Lohse,
T.; Luashvili, A.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev, D.;
Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares, A.;
Marti'I-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P.; Meyer, M.;
Mitchell, A.; Moderski, R.; Mohrmann, L.; Montanari, A.; Moore, C.;
Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.; Naurois
(de), M.; Nayerhoda, A.; Davids, H.; Niemiec, J.; Noel, A.; O'Brien,
P.; Oberholzer, L. L.; Ohm, S.; Olivera-Nieto, L.; Ona-Wilhelmi (de),
E.; Ostrowski, M.; Panny, S.; Panter, M.; Parsons, D.; Peron, G.;
Pita, S.; Poireau, V.; Prokhorov, D.; Prokoph, H.; Puehlhofer, G.;
Punch, M.; Quirrenbach, A.; Reichherzer, P.; Reimer, A.; Reimer, O.;
Remy, Q.; Renaud, M.; Reville, B.; Rieger, F.; Romoli, C.; Rowell,
G.; Rudak, B.; Rueda Ricarte, H.; Ruiz Velasco, E.; Sahakian, V.;
Sailer, S.; Salzmann, H.; Sanchez, D.; Santangelo, A.; Sasaki, M.;
Schaefer, J.; Schutte, H.; Schwanke, U.; Schüssler, F.; Senniappan,
M.; Seyffert, A.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.;
Sinha, A.; Sol, H.; Spackman, H.; Specovius, A.; Spencer, S. T.;
Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steinmassl,
S.; Steppa, C.; Sun, L.; Takahashi, T.; Tanaka, T.; Tavernier, T.;
Taylor, A.; Terrier, R.; Thiersen, H.; Thorpe-Morgan, C.; Tluczykont,
M.; Tomankova, L.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.;
van der Walt, J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.;
Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Völk,
H. J.; Wagner, S.; Watson, J. J.; Werner, F.; White, R.; Wierzcholska,
A.; Wong, Y. W.; Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin, R.;
Zargaryan, D.; Zdziarski, A.; Zech, A.; Zhu, S.; Zmija, A.; Zouari,
S.; Żywucka, N.
2022icrc.confE.960T Altcode: 2022PoS...395E.960T; 2021arXiv210904350S
The realtime follow-up of neutrino events is a promising approach
to search for astrophysical neutrino sources. It has so far provided
compelling evidence for a neutrino point source: the flaring gamma-ray
blazar TXS 0506+056 observed in coincidence with the high-energy
neutrino IceCube-170922A detected by IceCube. The detection of
very-high-energy gamma rays (VHE, $\mathrm{E} > 100\,\mathrm{GeV}$)
from this source helped establish the coincidence and constrained the
modeling of the blazar emission at the time of the IceCube event. The
four major imaging atmospheric Cherenkov telescope arrays (IACTs)
- FACT, H.E.S.S., MAGIC, and VERITAS - operate an active follow-up
program of target-of-opportunity observations of neutrino alerts sent by
IceCube. This program has two main components. One are the observations
of known gamma-ray sources around which a cluster of candidate neutrino
events has been identified by IceCube (Gamma-ray Follow-Up, GFU). Second
one is the follow-up of single high-energy neutrino candidate events
of potential astrophysical origin such as IceCube-170922A. GFU has been
recently upgraded by IceCube in collaboration with the IACT groups. We
present here recent results from the IACT follow-up programs of IceCube
neutrino alerts and a description of the upgraded IceCube GFU system.
---------------------------------------------------------
Title: Deep observations of Kepler's SNR with H.E.S.S.
Authors: Prokhorov, D.; Vink, J.; Simoni, R.; Komin, N.; Funk, S.;
Malyshev, D.; Mohrmann, L.; Ohm, S.; Puehlhofer, G.; Völk, H. J.;
Hess; Abdalla, H.; Aharonian, F.; Ait-Benkhali, F.; Anguener,
O.; Arcaro, C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes,
M.; Baghmanyan, V.; Barbosa Martins, V.; Barnacka, A.; Barnard,
M.; Batzofin, R.; Becherini, Y.; Berge, D.; Bernloehr, K.; Bi, B.;
Böttcher, M.; Boisson, C.; Bolmont, J.; Bony (de), M.; Breuhaus, M.;
Brose, R.; Brun, F.; Bulik, T.; Bylund, T.; Cangemi, F.; Caroff, S.;
Casanova, S.; Catalano, J.; Chambery, P.; Chand, T. B.; Chen, A.;
Cotter, G.; Curlo, M.; Dalgleish, H.; Damascene Mbarubucyeye, J.;
Davids, I. D.; Davies, J.; Devin, J.; Djannati-Ataï, A.; Dmytriiev,
A.; Donath, A.; Doroshenko, V.; Dreyer, L.; Du Plessis, L.; Duffy,
C.; Egberts, K.; Einecke, S.; Ernenwein, J. P.; Fegan, S.; Feijen,
K.; Fiasson, A.; Fichet de Clairfontaine, G.; Fontaine, G.; Frans,
L.; Fuessling, M.; Gabici, S.; Gallant, Y.; Giavitto, G.; Giunti, L.;
Glawion, D.; Glicenstein, J. F.; Grondin, M. H.; Hattingh, S.; Haupt,
M.; Hermann, G.; Hinton, J.; Hofmann, W.; Hoischen, C.; Holch, T.;
Holler, M.; Horns, D.; Huang, Z.; Huber, D.; Hörbe, M.; Jamrozy, M.;
Jankowsky, F.; Joshi, V.; Jung, I.; Kasai, E.; Katarzynski, K.; Katz,
U.; Khangulyan, D.; Khelifi, B.; Klepser, S.; Kluzniak, W.; Konno,
R.; Kosack, K.; Kostunin, D.; Kreter, M.; Kukec Mezek, G.; Kundu, A.;
Lamanna, G.; Le Stum, S.; Lemiere, A.; Lemoine-Goumard, M.; Lenain,
J. P.; Leuschner, F.; Levy, C.; Lohse, T.; Luashvili, A.; Lypova, I.;
Mackey, J.; Majumdar, J.; Malyshev, D.; Marandon, V.; Marchegiani, P.;
Marcowith, A.; Mares, A.; Marti'i-Devesa, G.; Marx, R.; Maurin, G.;
Meintjes, P.; Meyer, M.; Mitchell, A.; Moderski, R.; Montanari, A.;
Moore, C.; Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima,
K.; Naurois (de), M.; Nayerhoda, A.; Davids, H.; Niemiec, J.; Noel,
A.; O'Brien, P.; Oberholzer, L. L.; Olivera-Nieto, L.; Ona-Wilhelmi
(de), E.; Ostrowski, M.; Panny, S.; Panter, M.; Parsons, D.; Peron,
G.; Pita, S.; Poireau, V.; Prokoph, H.; Punch, M.; Quirrenbach, A.;
Reichherzer, P.; Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Reville,
B.; Rieger, F.; Romoli, C.; Rowell, G.; Rudak, B.; Rueda Ricarte, H.;
Ruiz Velasco, E.; Sahakian, V.; Sailer, S.; Salzmann, H.; Sanchez,
D.; Santangelo, A.; Sasaki, M.; Schaefer, J.; Schutte, H.; Schwanke,
U.; Schüssler, F.; Senniappan, M.; Seyffert, A.; Shapopi, J. N. S.;
Shiningayamwe, K.; Sinha, A.; Sol, H.; Spackman, H.; Specovius, A.;
Spencer, S. T.; Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann,
C.; Steinmassl, S.; Steppa, C.; Sun, L.; Takahashi, T.; Tanaka, T.;
Tavernier, T.; Taylor, A.; Terrier, R.; Thiersen, H.; Thorpe-Morgan,
C.; Tluczykont, M.; Tomankova, L.; Tsirou, M.; Tsuji, N.; Tuffs,
R.; Uchiyama, Y.; van der Walt, J.; van Eldik, C.; van Rensburg,
C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent,
P.; Wagner, S.; Watson, J. J.; Werner, F.; White, R.; Wierzcholska,
A.; Wong, Y. W.; Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin, R.;
Zargaryan, D.; Zdziarski, A.; Zech, A.; Zhu, S.; Zmija, A.; Zouari,
S.; Żywucka, N.
2022icrc.confE.805P Altcode: 2021arXiv210711582P; 2022PoS...395E.805P
Kepler's supernova remnant (SNR) which is produced by the most recent
naked-eye supernova in our Galaxy is one of the best studied SNRs,
but its gamma-ray detection has eluded us so far. Observations with
modern imaging atmospheric Cherenkov telescopes (IACT) have enlarged
the knowledge about nearby SNRs with ages younger than 500 years by
establishing Cassiopeia A and Tycho's SNRs as very high energy (VHE)
gamma-ray sources and setting a lower limit on the distance to Kepler's
SNR. This SNR is significantly more distant than the other two and
expected to be one of the faintest gamma-ray sources within reach of
the IACT arrays of this generation. We report strong evidence for a
VHE signal from Kepler's SNR based on deep observations of the High
Energy Stereoscopic System (H.E.S.S.) with an exposure of 152 hours,
including 122 hours accumulated in 2017-2020. We further discuss
implications of this result for cosmic-ray acceleration in young SNRs.
---------------------------------------------------------
Title: Revisiting the PeVatron candidate MGRO J1908+06 with an
updated H.E.S.S. analysis
Authors: Hess; Abdalla, H.; Aharonian, F.; Ait-Benkhali, F.; Anguener,
O.; Arcaro, C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes,
M.; Baghmanyan, V.; Barbosa Martins, V.; Barnacka, A.; Barnard,
M.; Batzofin, R.; Becherini, Y.; Berge, D.; Bernloehr, K.; Bi, B.;
Böttcher, M.; Boisson, C.; Bolmont, J.; Bony (de), M.; Breuhaus, M.;
Brose, R.; Brun, F.; Bulik, T.; Bylund, T.; Cangemi, F.; Caroff, S.;
Casanova, S.; Catalano, J.; Chambery, P.; Chand, T. B.; Chen, A.;
Cotter, G.; Curlo, M.; Dalgleish, H.; Damascene Mbarubucyeye, J.;
Davids, I. D.; Davies, J.; Devin, J.; Djannati-Ataï, A.; Dmytriiev,
A.; Donath, A.; Doroshenko, V.; Dreyer, L.; Du Plessis, L.; Duffy,
C.; Egberts, K.; Einecke, S.; Ernenwein, J. P.; Fegan, S.; Feijen,
K.; Fiasson, A.; Fichet de Clairfontaine, G.; Fontaine, G.; Frans,
L.; Fuessling, M.; Funk, S.; Gabici, S.; Gallant, Y.; Giavitto, G.;
Giunti, L.; Glawion, D.; Glicenstein, J. F.; Grondin, M. H.; Hattingh,
S.; Haupt, M.; Hermann, G.; Hinton, J.; Hofmann, W.; Hoischen, C.;
Holch, T.; Holler, M.; Horns, D.; Huang, Z.; Huber, D.; Hörbe,
M.; Jamrozy, M.; Jankowsky, F.; Joshi, V.; Jung, I.; Kasai, E.;
Katarzynski, K.; Katz, U.; Khangulyan, D.; Khelifi, B.; Klepser, S.;
Kluzniak, W.; Komin, N.; Konno, R.; Kosack, K.; Kostunin, D.; Kreter,
M.; Kukec Mezek, G.; Kundu, A.; Lamanna, G.; Le Stum, S.; Lemiere, A.;
Lemoine-Goumard, M.; Lenain, J. P.; Leuschner, F.; Levy, C.; Lohse,
T.; Luashvili, A.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev, D.;
Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares, A.;
Marti'i-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P.; Meyer, M.;
Mitchell, A.; Moderski, R.; Mohrmann, L.; Montanari, A.; Moore, C.;
Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.; Naurois
(de), M.; Nayerhoda, A.; Davids, H.; Niemiec, J.; Noel, A.; O'Brien,
P.; Oberholzer, L. L.; Ohm, S.; Olivera-Nieto, L.; Ona-Wilhelmi (de),
E.; Ostrowski, M.; Panny, S.; Panter, M.; Parsons, D.; Peron, G.;
Pita, S.; Poireau, V.; Prokhorov, D.; Prokoph, H.; Puehlhofer, G.;
Punch, M.; Quirrenbach, A.; Reichherzer, P.; Reimer, A.; Reimer, O.;
Remy, Q.; Renaud, M.; Reville, B.; Rieger, F.; Romoli, C.; Rowell,
G.; Rudak, B.; Rueda Ricarte, H.; Ruiz Velasco, E.; Sahakian, V.;
Sailer, S.; Salzmann, H.; Sanchez, D.; Santangelo, A.; Sasaki, M.;
Schaefer, J.; Schutte, H.; Schwanke, U.; Schüssler, F.; Senniappan,
M.; Seyffert, A.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.;
Sinha, A.; Sol, H.; Spackman, H.; Specovius, A.; Spencer, S. T.;
Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steinmassl,
S.; Steppa, C.; Sun, L.; Takahashi, T.; Tanaka, T.; Tavernier, T.;
Taylor, A.; Terrier, R.; Thiersen, H.; Thorpe-Morgan, C.; Tluczykont,
M.; Tomankova, L.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.;
van der Walt, J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.;
Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Völk,
H. J.; Wagner, S.; Watson, J. J.; Werner, F.; White, R.; Wierzcholska,
A.; Wong, Y. W.; Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin, R.;
Zargaryan, D.; Zdziarski, A.; Zech, A.; Zhu, S.; Zmija, A.; Zouari,
S.; Żywucka, N.
2022icrc.confE.779H Altcode: 2021arXiv210803401K; 2022PoS...395E.779H
Detecting and studying galactic gamma-ray sources emitting very-high
energy photons sheds light on the acceleration and propagation of cosmic
rays presumably created in these sources. Currently, there are few
sources emitting photons with energies exceeding 100 TeV. In this work
we revisit the unidentified source MGRO J1908+06, initially detected by
Milagro, using an updated H.E.S.S. dataset and analysis pipeline. The
vicinity of the source contains a supernova remnant and pulsars as
well as molecular clouds. This makes the identification of the primary
source(s) of galactic cosmic rays as well as the nature of the gamma-ray
emission challenging, especially in light of the recent HAWC and LHAASO
detection of the high energy tail of its spectrum. Exploiting the better
angular resolution as compared to particle detectors, we investigate
the morphology of the source as well as its spectral properties.
---------------------------------------------------------
Title: Observation of burst activity from SGR1935+2154 associated
to first galactic FRB with H.E.S.S.
Authors: Hess; Abdalla, H.; Aharonian, F.; Ait-Benkhali, F.; Anguener,
O.; Arcaro, C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes,
M.; Baghmanyan, V.; Barbosa Martins, V.; Barnacka, A.; Barnard,
M.; Batzofin, R.; Becherini, Y.; Berge, D.; Bernloehr, K.; Bi, B.;
Böttcher, M.; Boisson, C.; Bolmont, J.; Bony (de), M.; Breuhaus, M.;
Brose, R.; Brun, F.; Bulik, T.; Bylund, T.; Cangemi, F.; Caroff, S.;
Casanova, S.; Catalano, J.; Chambery, P.; Chand, T. B.; Chen, A.;
Cotter, G.; Curlo, M.; Dalgleish, H.; Damascene Mbarubucyeye, J.;
Davids, I. D.; Davies, J.; Devin, J.; Djannati-Ataï, A.; Dmytriiev,
A.; Donath, A.; Doroshenko, V.; Dreyer, L.; Du Plessis, L.; Duffy,
C.; Egberts, K.; Einecke, S.; Ernenwein, J. P.; Fegan, S.; Feijen,
K.; Fiasson, A.; Fichet de Clairfontaine, G.; Fontaine, G.; Frans,
L.; Fuessling, M.; Funk, S.; Gabici, S.; Gallant, Y.; Giavitto, G.;
Giunti, L.; Glawion, D.; Glicenstein, J. F.; Grondin, M. H.; Hattingh,
S.; Haupt, M.; Hermann, G.; Hinton, J.; Hofmann, W.; Hoischen, C.;
Holch, T.; Holler, M.; Horns, D.; Huang, Z.; Huber, D.; Hörbe,
M.; Jamrozy, M.; Jankowsky, F.; Joshi, V.; Jung, I.; Kasai, E.;
Katarzynski, K.; Katz, U.; Khangulyan, D.; Khelifi, B.; Klepser, S.;
Kluzniak, W.; Komin, N.; Konno, R.; Kosack, K.; Kostunin, D.; Kreter,
M.; Kukec Mezek, G.; Kundu, A.; Lamanna, G.; Le Stum, S.; Lemiere, A.;
Lemoine-Goumard, M.; Lenain, J. P.; Leuschner, F.; Levy, C.; Lohse,
T.; Luashvili, A.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev, D.;
Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares, A.;
Marti'i-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P.; Meyer, M.;
Mitchell, A.; Moderski, R.; Mohrmann, L.; Montanari, A.; Moore, C.;
Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.; Naurois
(de), M.; Nayerhoda, A.; Davids, H.; Niemiec, J.; Noel, A.; O'Brien,
P.; Oberholzer, L. L.; Ohm, S.; Olivera-Nieto, L.; Ona-Wilhelmi (de),
E.; Ostrowski, M.; Panny, S.; Panter, M.; Parsons, D.; Peron, G.;
Pita, S.; Poireau, V.; Prokhorov, D.; Prokoph, H.; Puehlhofer, G.;
Punch, M.; Quirrenbach, A.; Reichherzer, P.; Reimer, A.; Reimer, O.;
Remy, Q.; Renaud, M.; Reville, B.; Rieger, F.; Romoli, C.; Rowell,
G.; Rudak, B.; Rueda Ricarte, H.; Ruiz Velasco, E.; Sahakian, V.;
Sailer, S.; Salzmann, H.; Sanchez, D.; Santangelo, A.; Sasaki, M.;
Schaefer, J.; Schutte, H.; Schwanke, U.; Schüssler, F.; Senniappan,
M.; Seyffert, A.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.;
Sinha, A.; Sol, H.; Spackman, H.; Specovius, A.; Spencer, S. T.;
Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steinmassl,
S.; Steppa, C.; Sun, L.; Takahashi, T.; Tanaka, T.; Tavernier, T.;
Taylor, A.; Terrier, R.; Thiersen, H.; Thorpe-Morgan, C.; Tluczykont,
M.; Tomankova, L.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.;
van der Walt, J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.;
Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Völk,
H. J.; Wagner, S.; Watson, J. J.; Werner, F.; White, R.; Wierzcholska,
A.; Wong, Y. W.; Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin, R.;
Zargaryan, D.; Zdziarski, A.; Zech, A.; Zhu, S.; Zmija, A.; Zouari,
S.; Żywucka, N.
2022icrc.confE.777H Altcode: 2022PoS...395E.777H
No abstract at ADS
---------------------------------------------------------
Title: Search for TeV emission from the Fermi Bubbles at low Galactic
latitudes with H.E.S.S. inner Galaxy survey
Authors: Hess; Abdalla, H.; Aharonian, F.; Ait-Benkhali, F.; Anguener,
O.; Arcaro, C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes,
M.; Baghmanyan, V.; Barbosa Martins, V.; Barnacka, A.; Barnard,
M.; Batzofin, R.; Becherini, Y.; Berge, D.; Bernloehr, K.; Bi, B.;
Böttcher, M.; Boisson, C.; Bolmont, J.; Bony (de), M.; Breuhaus, M.;
Brose, R.; Brun, F.; Bulik, T.; Bylund, T.; Cangemi, F.; Caroff, S.;
Casanova, S.; Catalano, J.; Chambery, P.; Chand, T. B.; Chen, A.;
Cotter, G.; Curlo, M.; Dalgleish, H.; Damascene Mbarubucyeye, J.;
Davids, I. D.; Davies, J.; Devin, J.; Djannati-Ataï, A.; Dmytriiev,
A.; Donath, A.; Doroshenko, V.; Dreyer, L.; Du Plessis, L.; Duffy,
C.; Egberts, K.; Einecke, S.; Ernenwein, J. P.; Fegan, S.; Feijen,
K.; Fiasson, A.; Fichet de Clairfontaine, G.; Fontaine, G.; Frans,
L.; Fuessling, M.; Funk, S.; Gabici, S.; Gallant, Y.; Giavitto,
G.; Giunti, L.; Glawion, D.; Glicenstein, J. F.; Grondin, M. H.;
Hattingh, S.; Haupt, M.; Hermann, G.; Hinton, J.; Hofmann, W.;
Hoischen, C.; Holch, T.; Holler, M.; Horns, D.; Huang, Z.; Huber,
D.; Hörbe, M.; Jamrozy, M.; Jankowsky, F.; Joshi, V.; Jung, I.;
Kasai, E.; Katarzynski, K.; Katz, U.; Khangulyan, D.; Khelifi, B.;
Klepser, S.; Kluzniak, W.; Komin, N.; Konno, R.; Kosack, K.; Kostunin,
D.; Kreter, M.; Kukec Mezek, G.; Kundu, A.; Lamanna, G.; Le Stum,
S.; Lemiere, A.; Lemoine-Goumard, M.; Lenain, J. P.; Leuschner,
F.; Levy, C.; Lohse, T.; Luashvili, A.; Lypova, I.; Mackey, J.;
Majumdar, J.; Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares,
A.; Marti'i-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P.; Meyer,
M.; Mitchell, A.; Moderski, R.; Mohrmann, L.; Moore, C.; Morris,
P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.; Naurois (de),
M.; Nayerhoda, A.; Davids, H.; Niemiec, J.; Noel, A.; O'Brien, P.;
Oberholzer, L. L.; Ohm, S.; Olivera-Nieto, L.; Ona-Wilhelmi (de),
E.; Ostrowski, M.; Panny, S.; Panter, M.; Parsons, D.; Peron, G.;
Pita, S.; Poireau, V.; Prokhorov, D.; Prokoph, H.; Puehlhofer, G.;
Punch, M.; Quirrenbach, A.; Reichherzer, P.; Reimer, A.; Reimer, O.;
Remy, Q.; Renaud, M.; Reville, B.; Rieger, F.; Romoli, C.; Rowell,
G.; Rudak, B.; Rueda Ricarte, H.; Ruiz Velasco, E.; Sahakian, V.;
Sailer, S.; Salzmann, H.; Sanchez, D.; Santangelo, A.; Sasaki, M.;
Schaefer, J.; Schutte, H.; Schwanke, U.; Schüssler, F.; Senniappan,
M.; Seyffert, A.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.;
Sinha, A.; Sol, H.; Spackman, H.; Specovius, A.; Spencer, S. T.;
Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steinmassl,
S.; Steppa, C.; Sun, L.; Takahashi, T.; Tanaka, T.; Tavernier, T.;
Taylor, A.; Terrier, R.; Thiersen, H.; Thorpe-Morgan, C.; Tluczykont,
M.; Tomankova, L.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.;
van der Walt, J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.;
Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Völk,
H. J.; Wagner, S.; Watson, J. J.; Werner, F.; White, R.; Wierzcholska,
A.; Wong, Y. W.; Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin, R.;
Zargaryan, D.; Zdziarski, A.; Zech, A.; Zhu, S.; Zmija, A.; Zouari,
S.; Żywucka, N.; Montanari, A.; Malyshev, D.; Malyshev, D.
2022icrc.confE.791H Altcode: 2022PoS...395E.791H
No abstract at ADS
---------------------------------------------------------
Title: Limits on primordial black hole evaporation from
H.E.S.S. observations.
Authors: Tavernier, T.; Glicenstein, J. F.; Brun, F.; Marandon,
V.; Hess; Abdalla, H.; Aharonian, F.; Ait-Benkhali, F.; Anguener,
O.; Arcaro, C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes,
M.; Baghmanyan, V.; Barbosa Martins, V.; Barnacka, A.; Barnard,
M.; Batzofin, R.; Becherini, Y.; Berge, D.; Bernloehr, K.; Bi, B.;
Böttcher, M.; Boisson, C.; Bolmont, J.; Bony (de), M.; Breuhaus, M.;
Brose, R.; Bulik, T.; Bylund, T.; Cangemi, F.; Caroff, S.; Casanova,
S.; Catalano, J.; Chambery, P.; Chand, T. B.; Chen, A.; Cotter, G.;
Curlo, M.; Dalgleish, H.; Damascene Mbarubucyeye, J.; Davids, I. D.;
Davies, J.; Devin, J.; Djannati-Ataï, A.; Dmytriiev, A.; Donath, A.;
Doroshenko, V.; Dreyer, L.; Du Plessis, L.; Duffy, C.; Egberts, K.;
Einecke, S.; Ernenwein, J. P.; Fegan, S.; Feijen, K.; Fiasson, A.;
Fichet de Clairfontaine, G.; Fontaine, G.; Frans, L.; Fuessling, M.;
Funk, S.; Gabici, S.; Gallant, Y.; Giavitto, G.; Giunti, L.; Glawion,
D.; Grondin, M. H.; Hattingh, S.; Haupt, M.; Hermann, G.; Hinton, J.;
Hofmann, W.; Hoischen, C.; Holch, T.; Holler, M.; Horns, D.; Huang,
Z.; Huber, D.; Hörbe, M.; Jamrozy, M.; Jankowsky, F.; Joshi, V.; Jung,
I.; Kasai, E.; Katarzynski, K.; Katz, U.; Khangulyan, D.; Khelifi, B.;
Klepser, S.; Kluzniak, W.; Komin, N.; Konno, R.; Kosack, K.; Kostunin,
D.; Kreter, M.; Kukec Mezek, G.; Kundu, A.; Lamanna, G.; Le Stum, S.;
Lemiere, A.; Lemoine-Goumard, M.; Lenain, J. P.; Leuschner, F.; Levy,
C.; Lohse, T.; Luashvili, A.; Lypova, I.; Mackey, J.; Majumdar, J.;
Malyshev, D.; Malyshev, D.; Marchegiani, P.; Marcowith, A.; Mares, A.;
Marti'i-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P.; Meyer, M.;
Mitchell, A.; Moderski, R.; Mohrmann, L.; Montanari, A.; Moore, C.;
Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.; Naurois
(de), M.; Nayerhoda, A.; Davids, H.; Niemiec, J.; Noel, A.; O'Brien,
P.; Oberholzer, L. L.; Ohm, S.; Olivera-Nieto, L.; Ona-Wilhelmi (de),
E.; Ostrowski, M.; Panny, S.; Panter, M.; Parsons, D.; Peron, G.;
Pita, S.; Poireau, V.; Prokhorov, D.; Prokoph, H.; Puehlhofer, G.;
Punch, M.; Quirrenbach, A.; Reichherzer, P.; Reimer, A.; Reimer, O.;
Remy, Q.; Renaud, M.; Reville, B.; Rieger, F.; Romoli, C.; Rowell,
G.; Rudak, B.; Rueda Ricarte, H.; Ruiz Velasco, E.; Sahakian, V.;
Sailer, S.; Salzmann, H.; Sanchez, D.; Santangelo, A.; Sasaki, M.;
Schaefer, J.; Schutte, H.; Schwanke, U.; Schüssler, F.; Senniappan,
M.; Seyffert, A.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.;
Sinha, A.; Sol, H.; Spackman, H.; Specovius, A.; Spencer, S. T.;
Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steinmassl,
S.; Steppa, C.; Sun, L.; Takahashi, T.; Tanaka, T.; Tavernier, T.;
Taylor, A.; Terrier, R.; Thiersen, H.; Thorpe-Morgan, C.; Tluczykont,
M.; Tomankova, L.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.;
van der Walt, J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.;
Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Völk,
H. J.; Wagner, S.; Watson, J. J.; Werner, F.; White, R.; Wierzcholska,
A.; Wong, Y. W.; Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin, R.;
Zargaryan, D.; Zdziarski, A.; Zech, A.; Zhu, S.; Zmija, A.; Zouari,
S.; Żywucka, N.
2022icrc.confE.518T Altcode: 2022PoS...395E.518T
No abstract at ADS
---------------------------------------------------------
Title: CTA – the World's largest ground-based gamma-ray observatory
Authors: Zanin, R.; Abdalla, H.; Abe, H.; Abe, S.; Abusleme, A.;
Acero, F.; Acharyya, A.; Acin Portella, V.; Ackley, K.; Adam, R.;
Adams, C.; Adhikari, S. S.; Aguado Ruesga, I.; Agudo, I.; Aguilera,
R.; Aguirre Santaella, A.; Aharonian, F.; Alberdi, A.; Alfaro, R.;
Alfaro, J.; Alispach, C.; Aloisio, R.; Alves Batista, R.; Amans,
J. P.; Amati, L.; Amato, E.; Ambrogi, L.; Ambrosi, G.; Ambrosio, M.;
Ammendola, R.; Anderson, J.; Anduze, M.; Anguner, E. O.; Antonelli,
L. A.; Antonuccio, V.; Antoranz, P.; Anutarawiramkul, R.; Aragunde
Gutierrez, J.; Aramo, C.; Araudo, A.; Araya, M.; Arbet Engels, A.;
Arcaro, C.; Arendt, V.; Armand, C.; Armstrong, T.; Arqueros, F.;
Arrabito, L.; Arsioli, B.; Artero, M.; Asano, K.; Ascasibar, Y.;
Aschersleben, J.; Ashley, M.; Attina, P.; Aubert, P.; Singh, C. B.;
Baack, D.; Babic, A.; Backes, M.; Baena, V.; Bajtlik, S.; Baktash,
A.; Balazs, C.; Balbo, M.; Ballester, O.; Ballet, J.; Balmaverde, B.;
Bamba, A.; Bandiera, R.; Baquero Larriva, A.; Barai, P.; Barbier, C.;
Barbosa Martins, V.; Barcelo, M.; Barkov, M.; Barnard, M.; Baroncelli,
L.; Barres de Almeida, U.; Barrio, J. A.; Bastieri, D.; Batista, P. I.;
Batkovic, I.; Bauer, C.; Bautista González, R.; Baxter, J.; Becciani,
U.; Becerra González, J.; Becherini, Y.; Beck, G.; Becker Tjus, J.;
Bednarek, W.; Belfiore, A.; Bellizzi, L.; Belmont, R.; Benbow, W.;
Berge, D.; Bernardini, E.; Bernardos, M. I.; Bernlöhr, K.; Berti,
A.; Berton, M.; Bertucci, B.; Beshley, V.; Bhatt, N.; Bhattacharyya,
S.; Bhattacharyya, W.; Bhattacharyya, S.; Bi, B. Y.; Bicknell, G.;
Biederbeck, N.; Bigongiari, C.; Biland, A.; Bird, R.; Bissaldi, E.;
Biteau, J.; Bitossi, M.; Blanch, O.; Blank, M.; Blazek, J.; Bobin,
J.; Boccato, C.; Bocchino, F.; Boehm, C.; Bohacova, M.; Boisson, C.;
Boix, J.; Bolle, J. P.; Bolmont, J.; Bonanno, G.; Bonavolontà, C.;
Bonneau Arbeletche, L.; Bonnoli, G.; Bordas, P.; Borkowski, J.; Bose,
R.; Bose, D.; Bosnjak, Z.; Bottacini, E.; Böttcher, M.; Botticella,
M. T.; Boutonnet, C.; Bouyjou, F.; Bozhilov, V.; Bozzo, E.; Brahimi,
L.; Braiding, C.; Brau Nogue, S.; Breen, S.; Bregeon, J.; Breuhaus,
M.; Brill, A.; Brisken, W.; Brocato, E.; Brown, A. M.; Brügge, K.;
Brun, P.; Brun, F.; Brunetti, L.; Brunetti, G.; Bruno, P.; Bruno,
A.; Bruzzese, A.; Bucciantini, N.; Buckley, J. H.; Bühler, R.;
Bulgarelli, A.; Bulik, T.; Bünning, M.; Bunse, M.; Burton, M.;
Burtovoi, A.; Buscemi, M.; Buschjager, S.; Busetto, G.; Buss, J.;
Byrum, K.; Caccianiga, A.; Cadoux, F.; Calanducci, A.; Calderon,
C.; Calvo Tovar, J.; Cameron, R. A.; Campana, P.; Canestrari, R.;
Cangemi, F.; Cantlay, B.; Capalbi, M.; Capasso, M.; Cappi, M.;
Caproni, A.; Capuzzo Dolcetta, R.; Caraveo, P.; Cárdenas, V.;
Cardiel, L.; Cardillo, M.; Carlile, C.; Caroff, S.; Carosi, R.;
Carosi, A.; Carquin, E.; Carrere, M.; Casandjian, J. M.; Casanova,
S.; Cassol, F.; Catalani, F.; Catalano, O.; Cauz, D.; Ceccanti, A.;
Celestino Silva, C.; Cerny, K.; Cerruti, M.; Chabanne, E.; Chadwick,
P.; Chai, Y.; Chambery, P.; Champion, C.; Chaty, S.; Chen, A.; Cheng,
K.; Chernyakova, M.; Chiaro, G.; Chiavassa, A.; Chikawa, M.; Chitnis,
V. R.; Chudoba, J.; Chytka, L.; Cikota, S.; Circiello, A.; Clark,
P.; Colak, M.; Colombo, E.; Colonges, S.; Comastri, A.; Compagnino,
A.; Conforti, V.; Congiu, E.; Coniglione, R.; Conrad, J.; Conte,
F.; Contreras, J. L.; Coppi, P.; Cornat, R.; Coronado Blazquez,
J.; Cortina, J.; Costa, A.; Costantini, H.; Cotter, G.; Courty, B.;
Covino, S.; Crestan, S.; Cristofari, P.; Crocker, R.; Croston, J.;
Cubuk, K.; Cuevas, O.; Cui, X.; Cusumano, G.; Cutini, S.; D'Amico,
G.; D'Ammando, F.; D'Avanzo, P.; Da Vela, P.; Dadina, M.; Dai, S.;
Dalchenko, M.; Dall'Ora, M.; Daniel, M. K.; Dauguet, J.; Davids, I.;
Davies, J.; Dawson, B.; De Angelis, A.; de Araujo Carvalho, A. E.;
de Bony de Lavergne, M.; De Cesare, G.; de Frondat, F.; de la Calle,
I.; de Gouveia Dal Pino, E.; De Lotto, B.; De Luca, A.; De Martino,
D.; de Naurois, M.; de Ona Wilhelmi, E.; De Palma Persio, F.; De
Simone, N.; de Souza Valle, V.; Delagnes, E.; Deleglise Reznicek,
G.; Delgado, C.; Delgado Giler, A. G.; Delgado Mengual Valle, J.;
della Volpe, D.; Depaoli, D.; Devin, J.; Di Girolamo, T.; Di Giulio
Pierro, C.; Di Venere, L.; Díaz, C.; Dib, C.; Diebold, S.; Digel,
S.; Djannati Atai, A.; Djuvsland, J.; Dmytriiev, A.; Docher, K.;
Domínguez, A.; Dominis Prester, D.; Donini, A.; Dorner, D.; Doro,
M.; dos Anjos, R. d. C.; Dournaux, J. L.; Downes, T.; Drake, G.;
Drass, H.; Dravins, D.; Duangchan, C.; Duara, A.; Dubus, G.; Ducci,
L.; Duffy, C.; Dumora, D.; Dundas Mora, K.; Durkalec, A.; Dwarkadas,
V. V.; Ebr, J.; Eckner, C.; Eder, J.; Edy, E.; Egberts, K.; Einecke,
S.; Eleftheriadis, C.; Elsässer, D.; Emery, G.; Emmanoulopoulos, D.;
Ernenwein, J. P.; Errando, M.; Escarate, P.; Escudero, J.; Espinoza,
C.; Ettori, S.; Eungwanichayapant, A.; Evans, P.; Evoli, C.; Fairbairn,
M.; Falceta Goncalves, D.; Falcone, A.; Fallah Ramazanı, V.; Falomo,
R.; Farakos, K.; Fasola, G.; Fattorini, A.; Favre, Y.; Fedora, R.;
Fedorova, E.; Feijen, K.; Feng, Q.; Ferrand, G.; Ferrara, G.; Ferreira,
O.; Fesquet, M.; Fiandrini, E.; Fiasson, A.; Filipovic, M.; Fink, D.;
Finley, J. P.; Fioretti, V.; Fiorillo, D. F. G.; Fiorini, M.; Flis, S.;
Flores, H.; Foffano, L.; Fohr, C.; Fonseca, M. V.; Font, L.; Fontaine,
G.; Fornieri, O.; Fortin, P.; Fortson, L.; Fouque, N.; Fraga, B.;
Franceschini, A.; Franco, F. J.; Freixas Coromina, L.; Fresnillo, L.;
Fugazza, D.; Fujita, Y.; Fukami, S.; Fukazawa, Y.; Fulla, D.; Funk,
S.; Furniss, A.; Gabici, S.; Gaggero, D.; Galanti, G.; Galdemard,
P.; Gallant, Y. A.; Galloway, D.; Gallozzi, S.; Gammaldi, V.; Garcia,
R.; Garcia, E.; Garcia Lopez, E.; Gargano, F.; Gargano, C.; Garozzo,
S.; Gascon, D.; Gasparetto, T.; Gasparrini, D.; Gasparyan, H.; Gaug,
M.; Geffroy, N.; Gent, A.; Germani, S.; Ghalumyan, A.; Ghedina, A.;
Ghirlanda, G.; Gianotti, F.; Giarrusso, S.; Giarrusso, M.; Giavitto,
G.; Giebels, B.; Giglietto, N.; Gika, V.; Gillardo, F.; Gimenes,
R.; Giordano, F.; Giro, E.; Giroletti, M.; Giuliani, A.; Gjaja,
M.; Glicenstein, J. F.; Gliwny, P.; Goksu, H.; Goldoni, P.; Gomez,
J. L.; Gonzalez, M. M.; Gonzalez, J. M.; Gothe, K. S.; Gotz Coelho,
D.; Grabarczyk, T.; Graciani, R.; Grandi, P.; Grasseau, G.; Grasso,
D.; Green, D.; Green, J.; Greenshaw, T.; Grespan, P.; Grillo, A.;
Grondin, M. H.; Grube, J.; Guarino, V.; Guest, B.; Gueta, O.; Günduz,
M.; Gunji, S.; Gyuk, G.; Hackfeld, J.; Hadasch, D.; Hagge, L.; Hahn,
A.; Hajlaoui, J. E.; Halim, A.; Hamal, P.; Hanlon, W.; Harada, Y.;
Hardcastle, M. J.; Collado, M. Harvey; Haubold, T.; Haupt, A.; Havelka,
M.; Hayashi, K.; Hayashi, K.; Hayashida, M.; He, H.; Heckmann, L.;
Heller, M.; Henault, F.; Henri, G.; Hermann, G.; Hernández Cadena, S.;
Herrera Llorente, J.; Hervet, O.; Hinton, J.; Hiramatsu, A.; Hirotani,
K.; Hnatyk, B.; Hnatyk, R.; Hoang, J. K.; Hoffmann, D. H. H.; Hoischen,
C.; Holder, J.; Holler, M.; Hona, B.; Horan, D.; Horns, D.; Horvath,
P.; Houles, J.; Hrabovsky, M.; Hrupec, D.; Huang, Y.; Huet, J. M.;
Hughes, G.; Hull, G.; Humensky, T. B.; Hütten, M.; Iarlori, M.; Illa,
J. M.; Imazawa, R.; Inada, T.; Incardona, F.; Ingallinera, A.; Inoue,
S.; Inoue, T.; Inoue, Y.; Iocco, F.; Ioka, K.; Ionica, M.; Iovenitti,
S.; Iriarte, A.; Ishio, K.; Ishizaki, W.; Iwamura, Y.; Jacquemier, J.;
Jacquemont, M.; Jamrozy, M.; Janecek, P.; Jankowsky, F.; JardinBlicq,
A.; Jarnot, C.; Martínez, P. Jean; Jocou, L.; Jordana, N.; Josselin,
M.; JungRichardt, I.; Junqueira, F. J. P. A.; Juramy Gilles, C.;
Kaaret, P.; Kadowaki, L. H. S.; Kagaya, M.; Kankanyan, R.; Kantzas, D.;
Karas, V.; Karastergiou, A.; Karkar, S.; Kasperek, J.; Katagiri, H.;
Kataoka, J.; Katarzynski, K.; Katsuda, S.; Kawanaka, N.; Kazanas, D.;
Kerszberg, D.; Khélifi, B.; Kherlakian, M. C.; Kian, T. P.; Kieda,
D. B.; Kihm, T.; Kim, S.; Kisaka, S.; Kissmann, R.; Kleijwegt, R.;
Kluge, G.; Kluźniak, W.; Knapp, J.; Kobakhidze, A.; Kobayashi, Y.;
Koch, B.; Kocot, J.; Kohri, K.; Komin, N.; Kong, A.; Kosack, K.; Krack,
F.; Krause, M.; Krennrich, F.; Kubo, H.; Kudryavtsev, V. N.; Kunwar,
S.; Kushida, J.; Kushwaha, P.; Parola, B.; La Rosa, G.; Lahmann, R.;
Lamastra, A.; Landoni, M.; Landriu, D.; Lang, R. G.; Lapington, J.;
Laporte, P.; Lason, P.; Lasuik, J.; Lazendic Galloway, J.; Le Flour,
T.; Le Sidaner, P.; Leach, S.; Lee, S. H.; Lee, W. H.; Oliveira,
S. Lee; Lemiere, A.; Lemoine Goumard, M.; Lenain, J. P.; Leone,
F.; Leray, V.; Leto, G.; Leuschner, F.; Lindemann, R.; Lindfors,
E.; Linhoff, L.; Liodakis, I.; Lipniacka, A.; Lobo, M.; Lohse, T.;
Lombardi, S.; Lopez, A.; Lopez, M.; Lopez Coto, R.; Louis, F.; Louys,
M.; Lucarelli, F.; Boudi, H. Ludwig; Luque Escamilla, P. L.; Maccarone,
M. C.; Mach, E.; Maciejewski, A. J.; Mackey, J.; Maeght, P.; Maggio,
C.; Maier, G.; Majumdar, P.; Makariev, M.; Mallamaci, M.; Malta Nunes
de Almeida, R.; Malyshev, D.; Malyshev, D.; Mandat, D.; Maneva, G.;
Manganaro, M.; Manigot, P.; Mannheim, K.; Maragos, N.; Marano, D.;
Marconi, M.; Marcowith, A.; Marculewicz, M.; Marcun, B.; Marin, J.;
Marinello, N.; Marinos, P.; Markoff, S.; Marquez, P.; Marsella, G.;
Martin, J. M.; Martin, P. G.; Martinez, M.; Martinez, G.; Martinez,
O.; Martinez Huerta, H.; Marty, C.; Marx, R.; Masetti, N.; Massimino,
P.; Matsumoto, H.; Matthews, N.; Maurin, G.; Moerbeck, W. Max; Maxted,
N.; Mazziotta, M. N.; Mazzola, S. M.; Mbarubucyeye, J. D.; Mc Comb,
L.; McHardy, I.; McKeague, S.; McMuldroch, S.; Medina, E.; Medina
Miranda, D.; Melandri, A.; Melioli, C.; Melkumyan, D.; Menchiari,
S.; Mereghetti, S.; Merino Arevalo, G.; Mestre, E.; Meunier, J. L.;
Meures, T.; Micanovic, S.; Miceli, M.; Michailidis, M.; Michalowski,
J.; Miener, T.; Mievre, I.; Miller, J. D.; Mineo, T.; Minev, M.;
Miranda, J. M.; Mitchell, A.; Mizuno, T.; Mode, B. A.; Moderski, R.;
Mohrmann, L.; Molinari, E.; Montaruli, T.; Monteiro, I.; Moore, C.;
Moralejo, A.; Morcuende Parrilla, D.; Moretti, E.; Mori, K.; Moriarty,
P.; Morik, K.; Morris, P.; Morselli, A.; Mosshammer, K.; Mukherjee,
R.; Muller, J.; Mundell, C.; Mundet, J.; Murach, T.; Muraczewski,
A.; Muraishi, H.; Musella, I.; Musumarra, A.; Nagai, A.; Nagataki,
S.; Naito, T.; Nakamori, T.; Nakashima, K.; Nakayama, K.; Nakhjiri,
N.; Naletto, G.; Naumann, D.; Nava, L.; Nawaz, M. A.; Ndiyavala,
H.; Neise, D.; Nellen, L.; Nemmen, R.; Neyroud, N.; Ngernphat, K.;
Nguyen Trung, T.; Nicastro, L.; Nickel, L.; Niemiec, J.; Nieto, D.;
Nigro, C.; Nikołajuk, M.; Ninci, D.; Noda, K.; Nogami, Y.; Nolan,
S.; Norris, R. P.; Nosek, D.; Nöthe, M.; Novotny, V.; Nozaki, S.;
Nunio, F.; O'Brien, P.; Obara, K.; Ohira, Y.; Ohishi, M.; Ohm, S.;
Oka, T.; Okazaki, N.; Okumura, A.; Oliver, C.; Olivera, G.; Olmi, B.;
Orienti, M.; Orito, R.; Orlandini, M.; Orlando, E.; Osborne, J. P.;
Ostrowski, M.; Otte, N.; Ovcharov, E.; Owen, E.; Oya, I.; Ozieblo, A.;
Padovani, M.; Pagliaro, A.; Paizis, A.; Palatiello, M.; Palatka, M.;
Palazzi, E.; Panazol, J. L.; Paneque, D.; Panny, S.; Pantaleo, F. R.;
Panter, M.; Paolillo, M.; Papitto, A.; Paravac, A.; Paredes, J. M.;
Pareschi, G.; Parmiggiani, N.; Parsons, R. D.; Paśko, P.; Patel,
S. R.; Patricelli, B.; Pavletic, L.; Pavy, S.; Peer, A.; Pecimotika,
M.; Pellegriti, M. G.; Peñil Del Campo, P.; Pepato, A.; Perard, S.;
Perennes, C.; Peresano, M.; Perez Aguilera, A.; Perez Romero, J.;
Perez Torres, M. A.; Persic, M.; Petrucci, P. O.; Petruk, O.; Peyaud,
B.; Pfrang, K.; Pian, E.; Piatteli, P.; Pietropaolo, E.; Pillera, R.;
Pimentel, D.; Pintore, F.; Garcia, C. Pio; Pirola, G.; Piron, F.; Pita,
S.; Pohl, M.; Poireau, V.; Pollo, A.; Polo, M.; Pongkitivanichkul, C.;
Porthault, J.; Powell, J.; Pozo, D.; Prado, R. R.; Prandini, E.; Prast,
J.; Pressard, K.; Principe, G.; Produit, N.; Prokhorov, D.; Prokoph,
H.; Przybilski, H.; Pueschel, E.; Pühlhofer, G.; Puljak, I.; Pumo,
M. L.; Punch, M.; Queiroz, F.; Quinn, J.; Quirrenbach, A.; Rajda,
P. J.; Rando, R.; Razzaque, S.; Recchia, S.; Reichherzer, P.; Reimer,
O.; Reisenegger, A.; Remy, Q.; Renaud, M.; Reposeur, T.; Reville,
B.; Reymond, J. M.; Reynolds, J.; Ribeiro, D.; Ribo, M.; Richards,
G.; Rico, J.; Rieger, F.; Riitano, L.; Riquelme, M.; Riquelme, D.;
Rivoire, S.; Rizi, V.; Roache, E.; Roche, M.; Rodriguez, J.; Rodriguez
Fernandez, G.; Rodriguez Ramirez, J. C.; Rodriguez Vazquez, J. J.;
Rojas, G.; Romano, P.; Romeo Lobato, G.; Romoli, C.; Roncadelli,
M.; Rosado, J.; Rosales de Leon, A.; Rowell, G.; Rugliancich, A.;
Ruiz del Mazo, J. E.; Rulten, C.; Russell, C.; Russo Hatlen, F.;
Safi Harb, S.; Saha, L.; Sahakian, V.; Sailer, S.; Saito, T.; Sakaki,
N.; Sakurai, S.; Salina, G.; Salzmann, H.; Sanchez, D.; Sandaker, H.;
Sandoval, A.; Sangiorgi, P.; Sanguillon, M.; Sano, H.; Santander, M.;
Santangelo, A.; Santos Lima, R.; Sanuy, A.; Sapozhnikov, L.; Saric,
T.; Sarkar, S.; Sasaki, H.; Sasaki, N.; Sato, Y.; Saturni, F. G.;
Sawada, M.; Schaefer, J.; Scherer, A.; Scherpenberg, J.; Schipani,
P.; Schleicher, B.; Schmoll, J.; Schneider, M.; Schoorlemmer, H.;
Schovanek, P.; Schussler, F.; Schwab, B.; Schwanke, U.; Schwarz, J.;
Sciacca, E.; Scuderi, S.; Seglar Arroyo, M.; Seitenzahl, I.; Semikoz,
D.; Sergijenko, O.; Serna Franco, J. E.; Seweryn, K.; Sguera, V.;
Shalchi, A.; Shang, R. Y.; Sharma, P.; Sidoli, L.; Sieiro, J.;
Siejkowski, H.; Sillanpaa, A.; Singh, B. B.; Singh, K. K.; Sinha,
A.; Siqueira, C.; Sitarek, J.; Sizun, P.; Sliusar, V.; Sobczynska,
D.; Sobrinho, R. W.; Sol, H.; Sottile, G.; Spackman, H.; Spencer,
S.; Spengler, G.; Spiga, D.; Springer, W.; Stamerra, A.; Stanic, S.;
Starling, R.; Stawarz, Ł.; Stefanik, S.; Stegmann, C.; Steiner, A.;
Steinmassl, S.; Stella, C.; Sternberger, R.; Sterzel, M.; Stevens, C.;
Stevenson, B.; Stolarczyk, T.; Stratta, G.; Straumann, U.; Striskovic,
J.; Strzys, M.; Stuik, R.; Suchenek, M.; Sunada, Y.; Suomijarvi,
T.; Suric, T.; Suzuki, H.; Swierk, P.; Szepieniec, T.; Tachihara,
K.; Tagliaferri, G.; Tajima, H.; Tajima, N.; Tak, D.; Takahashi, H.;
Takahashi, M.; Takata, J.; Takeishi, R.; Tam, T.; Tanaka, M.; Tanaka,
T.; Tanaka, S.; Tavani, M.; Tavecchio, F.; Tavernier, T.; Taylor,
A. R.; Tejedor, L. A.; Temnikov, P.; Terauchi, K.; Terrazas, J. C.;
Terrier, R.; Terzic, T.; Teshima, M.; Thibaut, D.; Thocquenne, F.;
Tian, W.; Tibaldo, L.; Tiengo, A.; Tluczykont, M.; Todero Peixoto,
C. J.; Toma, K.; Tomankova, L.; Tomastik, J.; Tornikoski, M.; Torres,
D. F.; Torresi, E.; Tosti, G.; Tosti, L.; Tothill, N.; Toussenel,
F.; Tovmassian, G.; Trichard, C.; Trifoglio, M.; Trois, A.; Truzzi,
S.; Tsiahina, A.; Turk, B.; Tutone, A.; Uchiyama, Y.; Utayarat,
P.; Vaclavek, L.; Vacula, M.; Vagelli, V.; Vagnetti, F.; Valdivia,
J. A.; Valentino, M.; Valio, A.; Vallage, B.; Vallania Quispe, P.;
van den Berg, A. M.; van Driel, W.; van Eldik, C.; van Rensburg,
C.; van Soelen, B.; Vandenbroucke, J.; Vasileiadis, G.; Vassiliev,
V.; Vazquez Acosta, M.; Vecchi, M.; Vega, A.; Veh, J.; Veitch, P.;
Venter, C.; Ventura, S.; Vercellone, S.; Verguilov, V.; Verna, G.;
Vernetto, S.; Verzi, V.; Vettolani, G. P.; Veyssiere, C.; Viale, I.;
Viana, A.; Viaux, N.; Vignatti, J.; Vigorito, C. F.; Villanueva, J.;
Vitale, V.; Vittorini, V.; Vodeb, V.; Vogel, N.; Voisin, V.; Vorobiov,
S.; Vrastil, M.; Vuillaume, T.; Wagner, S. J.; Wagner, P.; Wakazono,
K.; Wakely, S. P.; Ward, M.; Warren, D.; Watson, J.; Wechakama, M.;
Wegner, P.; Weinstein, A.; Weniger, C.; Werner, F.; Wetteskind, H.;
White, M. L.; Wierzcholska, A.; Wiesand, S.; Wijers, R.; Wilkinson,
M.; Will, M.; Williams, J.; Williamson, T. J.; Wolter, A.; Wong,
Y. W.; Wood, M.; Yamamoto, T.; Yamamoto, H.; Yamane, Y.; Yamazaki,
R.; Yanagita, S.; Yang, L.; Yoo, S.; Yoshida, T.; Yoshikoshi, T.;
Yu, P.; Yusafzai, A.; Zacharias, M.; Zaldivar, B.; Zampieri, L.;
Zanin, R.; Zanmar Sanchez, R.; Zaric, D.; Zavrtanik, M.; Zavrtanik,
D.; Zdziarski, A.; Zech, A.; Zechlin, H.; Zenin, A.; Zerwekh, A.;
Ziętara, K.; Zink, A.; Ziolkowski, J.; Zivec, M.; Zmija, A.
2022icrc.confE...5Z Altcode: 2022PoS...395E...5Z
No abstract at ADS
---------------------------------------------------------
Title: Science verification of the new FlashCam-based camera in the
28m telescope of H.E.S.S.
Authors: Puehlhofer, G.; Bernlöhr, K.; Bi, B.; Hermann, G.; Hinton,
J.; Jung-Richardt, I.; Leuschner, F.; Marandon, V.; Mitchell, A.;
Mohrmann, L.; Parsons, D.; Sailer, S.; Salzmann, H.; Steinmassl, S.;
Werner, F.; Abdalla, H.; Aharonian, F.; Ait-Benkhali, F.; Anguener,
O.; Arcaro, C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes, M.;
Baghmanyan, V.; Barbosa Martins, V.; Barnacka, A.; Barnard, M.;
Batzofin, R.; Becherini, Y.; Berge, D.; Bernloehr, K.; Böttcher,
M.; Boisson, C.; Bolmont, J.; Bony (de), M.; Breuhaus, M.; Brose, R.;
Brun, F.; Bulik, T.; Bylund, T.; Cangemi, F.; Caroff, S.; Casanova,
S.; Catalano, J.; Chambery, P.; Chand, T. B.; Chen, A.; Cotter, G.;
Curlo, M.; Dalgleish, H.; Damascene Mbarubucyeye, J.; Davids, I. D.;
Davies, J.; Devin, J.; Djannati-Ataï, A.; Dmytriiev, A.; Donath,
A.; Doroshenko, V.; Dreyer, L.; Du Plessis, L.; Duffy, C.; Egberts,
K.; Einecke, S.; Ernenwein, J. P.; Fegan, S.; Feijen, K.; Fiasson,
A.; Fichet de Clairfontaine, G.; Fontaine, G.; Frans, L.; Fuessling,
M.; Funk, S.; Gabici, S.; Gallant, Y.; Giavitto, G.; Giunti, L.;
Glawion, D.; Glicenstein, J. F.; Grondin, M. H.; Hattingh, S.; Haupt,
M.; Hörbe, M.; Hofmann, W.; Hoischen, C.; Holch, T.; Holler, M.;
Horns, D.; Huang, Z.; Huber, D.; Jamrozy, M.; Jankowsky, F.; Joshi,
V.; Kasai, E.; Katarzynski, K.; Katz, U.; Khangulyan, D.; Khelifi,
B.; Klepser, S.; Kluzniak, W.; Komin, N.; Konno, R.; Kosack, K.;
Kostunin, D.; Kreter, M.; Kukec Mezek, G.; Kundu, A.; Lamanna, G.;
Le Stum, S.; Lemiere, A.; Lemoine-Goumard, M.; Lenain, J. P.; Levy,
C.; Lohse, T.; Luashvili, A.; Lypova, I.; Mackey, J.; Majumdar, J.;
Malyshev, D.; Malyshev, D.; Marchegiani, P.; Marcowith, A.; Mares,
A.; Marti'i-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P.; Meyer, M.;
Moderski, R.; Montanari, A.; Moore, C.; Morris, P.; Moulin, E.; Muller,
J.; Murach, T.; Nakashima, K.; Naurois (de), M.; Nayerhoda, A.; Davids,
H.; Niemiec, J.; Noel, A.; O'Brien, P.; Oberholzer, L. L.; Ohm, S.;
Olivera-Nieto, L.; Ona-Wilhelmi (de), E.; Ostrowski, M.; Panny, S.;
Panter, M.; Parsons, D.; Peron, G.; Pita, S.; Poireau, V.; Prokhorov,
D.; Prokoph, H.; Punch, M.; Quirrenbach, A.; Reichherzer, P.; Reimer,
A.; Reimer, O.; Remy, Q.; Renaud, M.; Reville, B.; Rieger, F.; Romoli,
C.; Rowell, G.; Rudak, B.; Rueda Ricarte, H.; Ruiz Velasco, E.;
Sahakian, V.; Sanchez, D.; Santangelo, A.; Sasaki, M.; Schaefer, J.;
Schüssler, F.; Schutte, H.; Schwanke, U.; Senniappan, M.; Seyffert,
A.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.; Sinha, A.;
Sol, H.; Spackman, H.; Specovius, A.; Spencer, S. T.; Spir-Jacob,
M.; Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steppa, C.; Sun, L.;
Takahashi, T.; Tanaka, T.; Tavernier, T.; Taylor, A.; Terrier, R.;
Thiersen, H.; Thorpe-Morgan, C.; Tluczykont, M.; Tomankova, L.;
Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, J.;
van Eldik, C.; van Rensburg, C.; van Soelen, B.; Vasileiadis, G.;
Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Völk, H. J.; Wagner,
S.; Watson, J. J.; White, R.; Wierzcholska, A.; Wong, Y. W.; Yassin,
H.; Yusafzai, A.; Zacharias, M.; Zanin, R.; Zargaryan, D.; Zdziarski,
A.; Zech, A.; Zhu, S.; Zmija, A.; Zouari, S.; Żywucka, N.
2022icrc.confE.764P Altcode: 2022PoS...395E.764P; 2021arXiv210802596P
In October 2019 the central 28m telescope of the H.E.S.S. experiment
has been upgraded with a new camera. The camera is based on the
FlashCam design which has been developed in view of a possible
future implementation in the medium-sized telescopes of the Cherenkov
Telescope Array (CTA). We report here on the results of the science
verification program that has been performed after commissioning of
the new camera, to show that the camera and software pipelines are
working up to expectations.
---------------------------------------------------------
Title: Search for dark matter annihilation towards the inner Milky
Way halo with the H.E.S.S. Inner Galaxy Survey
Authors: Hess; Abdalla, H.; Aharonian, F.; Ait-Benkhali, F.; Anguener,
O.; Arcaro, C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes,
M.; Baghmanyan, V.; Barbosa Martins, V.; Barnacka, A.; Barnard,
M.; Batzofin, R.; Becherini, Y.; Berge, D.; Bernloehr, K.; Bi, B.;
Böttcher, M.; Boisson, C.; Bolmont, J.; Bony (de), M.; Breuhaus, M.;
Brose, R.; Brun, F.; Bulik, T.; Bylund, T.; Cangemi, F.; Caroff, S.;
Casanova, S.; Catalano, J.; Chambery, P.; Chand, T. B.; Chen, A.;
Cotter, G.; Curlo, M.; Dalgleish, H.; Damascene Mbarubucyeye, J.;
Davids, I. D.; Davies, J.; Devin, J.; Djannati-Ataï, A.; Dmytriiev,
A.; Donath, A.; Doroshenko, V.; Dreyer, L.; Du Plessis, L.; Duffy,
C.; Egberts, K.; Einecke, S.; Ernenwein, J. P.; Fegan, S.; Feijen,
K.; Fiasson, A.; Fichet de Clairfontaine, G.; Fontaine, G.; Frans,
L.; Fuessling, M.; Funk, S.; Gabici, S.; Gallant, Y.; Giavitto, G.;
Giunti, L.; Glawion, D.; Glicenstein, J. F.; Grondin, M. H.; Hattingh,
S.; Haupt, M.; Hermann, G.; Hinton, J.; Hofmann, W.; Hoischen, C.;
Holch, T.; Holler, M.; Horns, D.; Huang, Z.; Huber, D.; Hörbe,
M.; Jamrozy, M.; Jankowsky, F.; Joshi, V.; Jung, I.; Kasai, E.;
Katarzynski, K.; Katz, U.; Khangulyan, D.; Khelifi, B.; Klepser, S.;
Kluzniak, W.; Komin, N.; Konno, R.; Kosack, K.; Kostunin, D.; Kreter,
M.; Kukec Mezek, G.; Kundu, A.; Lamanna, G.; Le Stum, S.; Lemiere, A.;
Lemoine-Goumard, M.; Lenain, J. P.; Leuschner, F.; Levy, C.; Lohse,
T.; Luashvili, A.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev, D.;
Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares, A.;
Marti'i-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P.; Meyer, M.;
Mitchell, A.; Moderski, R.; Mohrmann, L.; Montanari, A.; Moore, C.;
Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.; Naurois
(de), M.; Nayerhoda, A.; Davids, H.; Niemiec, J.; Noel, A.; O'Brien,
P.; Oberholzer, L. L.; Ohm, S.; Olivera-Nieto, L.; Ona-Wilhelmi (de),
E.; Ostrowski, M.; Panny, S.; Panter, M.; Parsons, D.; Peron, G.;
Pita, S.; Poireau, V.; Prokhorov, D.; Prokoph, H.; Puehlhofer, G.;
Punch, M.; Quirrenbach, A.; Reichherzer, P.; Reimer, A.; Reimer, O.;
Remy, Q.; Renaud, M.; Reville, B.; Rieger, F.; Romoli, C.; Rowell,
G.; Rudak, B.; Rueda Ricarte, H.; Ruiz Velasco, E.; Sahakian, V.;
Sailer, S.; Salzmann, H.; Sanchez, D.; Santangelo, A.; Sasaki, M.;
Schaefer, J.; Schutte, H.; Schwanke, U.; Schüssler, F.; Senniappan,
M.; Seyffert, A.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.;
Sinha, A.; Sol, H.; Spackman, H.; Specovius, A.; Spencer, S. T.;
Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steinmassl,
S.; Steppa, C.; Sun, L.; Takahashi, T.; Tanaka, T.; Tavernier, T.;
Taylor, A.; Terrier, R.; Thiersen, H.; Thorpe-Morgan, C.; Tluczykont,
M.; Tomankova, L.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.;
van der Walt, J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.;
Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Völk,
H. J.; Wagner, S.; Watson, J. J.; Werner, F.; White, R.; Wierzcholska,
A.; Wong, Y. W.; Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin, R.;
Zargaryan, D.; Zdziarski, A.; Zech, A.; Zhu, S.; Zmija, A.; Zouari,
S.; Żywucka, N.
2022icrc.confE.511H Altcode: 2022PoS...395E.511H
No abstract at ADS
---------------------------------------------------------
Title: Evidence of 100 TeV γ-ray emission from HESS J1702-420:
A new PeVatron candidate
Authors: Giunti, L.; Khelifi, B.; Kosack, K.; Terrier, R.;
H. E. S. S. Collaboration; Hess; Abdalla, H.; Aharonian, F.;
Ait-Benkhali, F.; Anguener, O.; Arcaro, C.; Armand, C.; Armstrong,
T.; Ashkar, H.; Backes, M.; Baghmanyan, V.; Barbosa Martins, V.;
Barnacka, A.; Barnard, M.; Batzofin, R.; Becherini, Y.; Berge, D.;
Bernloehr, K.; Bi, B.; Böttcher, M.; Boisson, C.; Bolmont, J.;
Bony (de), M.; Breuhaus, M.; Brose, R.; Brun, F.; Bulik, T.; Bylund,
T.; Cangemi, F.; Caroff, S.; Casanova, S.; Catalano, J.; Chambery,
P.; Chand, T. B.; Chen, A.; Cotter, G.; Curlo, M.; Dalgleish, H.;
Damascene Mbarubucyeye, J.; Davids, I. D.; Davies, J.; Devin, J.;
Djannati-Ataï, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.; Dreyer,
L.; Du Plessis, L.; Duffy, C.; Egberts, K.; Einecke, S.; Ernenwein,
J. P.; Fegan, S.; Feijen, K.; Fiasson, A.; Fichet de Clairfontaine,
G.; Fontaine, G.; Frans, L.; Fuessling, M.; Funk, S.; Gabici, S.;
Gallant, Y.; Giavitto, G.; Glawion, D.; Glicenstein, J. F.; Grondin,
M. H.; Hattingh, S.; Haupt, M.; Hermann, G.; Hinton, J.; Hofmann,
W.; Hoischen, C.; Holch, T.; Holler, M.; Horns, D.; Huang, Z.;
Huber, D.; Hörbe, M.; Jamrozy, M.; Jankowsky, F.; Joshi, V.; Jung,
I.; Kasai, E.; Katarzynski, K.; Katz, U.; Khangulyan, D.; Klepser,
S.; Kluzniak, W.; Komin, N.; Konno, R.; Kostunin, D.; Kreter, M.;
Kukec Mezek, G.; Kundu, A.; Lamanna, G.; Le Stum, S.; Lemiere, A.;
Lemoine-Goumard, M.; Lenain, J. P.; Leuschner, F.; Levy, C.; Lohse,
T.; Luashvili, A.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev, D.;
Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares, A.;
Marti'i-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P.; Meyer, M.;
Mitchell, A.; Moderski, R.; Mohrmann, L.; Montanari, A.; Moore, C.;
Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.; Naurois
(de), M.; Nayerhoda, A.; Davids, H.; Niemiec, J.; Noel, A.; O'Brien,
P.; Oberholzer, L. L.; Ohm, S.; Olivera-Nieto, L.; Ona-Wilhelmi (de),
E.; Ostrowski, M.; Panny, S.; Panter, M.; Parsons, D.; Peron, G.; Pita,
S.; Poireau, V.; Prokhorov, D.; Prokoph, H.; Puehlhofer, G.; Punch, M.;
Quirrenbach, A.; Reichherzer, P.; Reimer, A.; Reimer, O.; Remy, Q.;
Renaud, M.; Reville, B.; Rieger, F.; Romoli, C.; Rowell, G.; Rudak,
B.; Rueda Ricarte, H.; Ruiz Velasco, E.; Sahakian, V.; Sailer, S.;
Salzmann, H.; Sanchez, D.; Santangelo, A.; Sasaki, M.; Schaefer, J.;
Schutte, H.; Schwanke, U.; Schüssler, F.; Senniappan, M.; Seyffert,
A.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol,
H.; Spackman, H.; Specovius, A.; Spencer, S. T.; Spir-Jacob, M.;
Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steinmassl, S.; Steppa,
C.; Sun, L.; Takahashi, T.; Tanaka, T.; Tavernier, T.; Taylor, A.;
Thiersen, H.; Thorpe-Morgan, C.; Tluczykont, M.; Tomankova, L.;
Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, J.;
van Eldik, C.; van Rensburg, C.; van Soelen, B.; Vasileiadis, G.;
Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Völk, H. J.; Wagner, S.;
Watson, J. J.; Werner, F.; White, R.; Wierzcholska, A.; Wong, Y. W.;
Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin, R.; Zargaryan, D.;
Zdziarski, A.; Zech, A.; Zhu, S.; Zmija, A.; Zouari, S.; Żywucka, N.
2022icrc.confE.793G Altcode: 2022PoS...395E.793G; 2021arXiv210802989G
The identification of active PeVatrons, hadronic particle accelerators
reaching the knee of the cosmic-ray spectrum (at the energy of few PeV),
is crucial to understand the origin of cosmic rays in the Galaxy. In
this context, we report on new H.E.S.S. observations of the PeVatron
candidate HESS J1702-420, which reveal the presence of gamma-rays up
to 100 TeV. This is the first time in the history of H.E.S.S. that
photons with such high energy are clearly detected. Remarkably, the
new deep observations allowed the discovery of a new gamma-ray source
component, called HESS J1702-420A, that was previously hidden under
the bulk emission traditionally associated with HESSJ1702-420. This
new object has a power-law spectral slope < 2 and a gamma-ray
spectrum that, extending with no sign of curvature up to 100 TeV,
makes it an excellent candidate site for the presence of PeV-energy
cosmic rays. This discovery brings new information to the ongoing
debate on the nature of the unidentified source HESSJ1702-420, one of
the most compelling PeVatron candidates in the gamma-ray sky, and on
the origin of Galactic cosmic rays.
---------------------------------------------------------
Title: Is PKS 0625-354 another variable TeV active galactic nucleus?
Authors: H. E. S. S. Collaboration; Hess; Abdalla, H.; Aharonian, F.;
Ait-Benkhali, F.; Anguener, O.; Arcaro, C.; Armand, C.; Armstrong,
T.; Ashkar, H.; Backes, M.; Baghmanyan, V.; Barbosa Martins, V.;
Barnacka, A.; Barnard, M.; Batzofin, R.; Becherini, Y.; Berge, D.;
Bernloehr, K.; Bi, B.; Böttcher, M.; Boisson, C.; Bolmont, J.;
Bony (de), M.; Breuhaus, M.; Brose, R.; Brun, F.; Bulik, T.; Bylund,
T.; Cangemi, F.; Caroff, S.; Casanova, S.; Catalano, J.; Chambery,
P.; Chand, T. B.; Chen, A.; Cotter, G.; Curlo, M.; Dalgleish, H.;
Damascene Mbarubucyeye, J.; Davids, I. D.; Davies, J.; Devin, J.;
Djannati-Ataï, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.; Dreyer,
L.; Du Plessis, L.; Duffy, C.; Egberts, K.; Einecke, S.; Ernenwein,
J. P.; Fegan, S.; Feijen, K.; Fiasson, A.; Fichet de Clairfontaine, G.;
Fontaine, G.; Frans, L.; Fuessling, M.; Funk, S.; Gabici, S.; Gallant,
Y.; Giavitto, G.; Giunti, L.; Glawion, D.; Glicenstein, J. F.; Grondin,
M. H.; Hattingh, S.; Haupt, M.; Hermann, G.; Hinton, J.; Hofmann, W.;
Hoischen, C.; Holch, T.; Holler, M.; Horns, D.; Huang, Z.; Huber, D.;
Hörbe, M.; Jamrozy, M.; Jankowsky, F.; Joshi, V.; Jung, I.; Kasai, E.;
Katarzynski, K.; Katz, U.; Khangulyan, D.; Khelifi, B.; Klepser, S.;
Kluzniak, W.; Komin, N.; Konno, R.; Kosack, K.; Kostunin, D.; Kreter,
M.; Kukec Mezek, G.; Kundu, A.; Lamanna, G.; Le Stum, S.; Lemiere, A.;
Lemoine-Goumard, M.; Lenain, J. P.; Leuschner, F.; Levy, C.; Lohse,
T.; Luashvili, A.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev, D.;
Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares, A.;
Marti'i-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P.; Meyer, M.;
Mitchell, A.; Moderski, R.; Mohrmann, L.; Montanari, A.; Moore, C.;
Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.; Naurois
(de), M.; Nayerhoda, A.; Davids, H.; Niemiec, J.; Noel, A.; O'Brien,
P.; Oberholzer, L. L.; Ohm, S.; Olivera-Nieto, L.; Ona-Wilhelmi (de),
E.; Ostrowski, M.; Panny, S.; Panter, M.; Parsons, D.; Peron, G.;
Pita, S.; Poireau, V.; Prokhorov, D.; Prokoph, H.; Puehlhofer, G.;
Punch, M.; Quirrenbach, A.; Reichherzer, P.; Reimer, A.; Reimer, O.;
Remy, Q.; Renaud, M.; Reville, B.; Rieger, F.; Romoli, C.; Rowell,
G.; Rudak, B.; Rueda Ricarte, H.; Ruiz Velasco, E.; Sahakian, V.;
Sailer, S.; Salzmann, H.; Sanchez, D.; Santangelo, A.; Sasaki, M.;
Schaefer, J.; Schutte, H.; Schwanke, U.; Schüssler, F.; Senniappan,
M.; Seyffert, A.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.;
Sinha, A.; Sol, H.; Spackman, H.; Specovius, A.; Spencer, S. T.;
Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steinmassl,
S.; Steppa, C.; Sun, L.; Takahashi, T.; Tanaka, T.; Tavernier, T.;
Taylor, A.; Terrier, R.; Thiersen, H.; Thorpe-Morgan, C.; Tluczykont,
M.; Tomankova, L.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.;
van der Walt, J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.;
Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Völk,
H. J.; Wagner, S.; Watson, J. J.; Werner, F.; White, R.; Wierzcholska,
A.; Wong, Y. W.; Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin, R.;
Zargaryan, D.; Zdziarski, A.; Zech, A.; Zhu, S.; Zmija, A.; Zouari,
S.; Żywucka, N.
2022icrc.confE.814H Altcode: 2022PoS...395E.814H
No abstract at ADS
---------------------------------------------------------
Title: H.E.S.S. follow-up of BBH merger events
Authors: Seglar Arroyo, M.; Hess; Abdalla, H.; Aharonian, F.;
Ait-Benkhali, F.; Anguener, O.; Arcaro, C.; Armand, C.; Armstrong,
T.; Ashkar, H.; Backes, M.; Baghmanyan, V.; Barbosa Martins, V.;
Barnacka, A.; Barnard, M.; Batzofin, R.; Becherini, Y.; Berge, D.;
Bernloehr, K.; Bi, B.; Böttcher, M.; Boisson, C.; Bolmont, J.;
Bony (de), M.; Breuhaus, M.; Brose, R.; Brun, F.; Bulik, T.; Bylund,
T.; Cangemi, F.; Caroff, S.; Casanova, S.; Catalano, J.; Chambery,
P.; Chand, T. B.; Chen, A.; Cotter, G.; Curlo, M.; Dalgleish, H.;
Damascene Mbarubucyeye, J.; Davids, I. D.; Davies, J.; Devin, J.;
Djannati-Ataï, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.; Dreyer,
L.; Du Plessis, L.; Duffy, C.; Egberts, K.; Einecke, S.; Ernenwein,
J. P.; Fegan, S.; Feijen, K.; Fiasson, A.; Fichet de Clairfontaine, G.;
Fontaine, G.; Frans, L.; Fuessling, M.; Funk, S.; Gabici, S.; Gallant,
Y.; Giavitto, G.; Giunti, L.; Glawion, D.; Glicenstein, J. F.; Grondin,
M. H.; Hattingh, S.; Haupt, M.; Hermann, G.; Hinton, J.; Hofmann, W.;
Hoischen, C.; Holch, T.; Holler, M.; Horns, D.; Huang, Z.; Huber, D.;
Hörbe, M.; Jamrozy, M.; Jankowsky, F.; Joshi, V.; Jung, I.; Kasai, E.;
Katarzynski, K.; Katz, U.; Khangulyan, D.; Khelifi, B.; Klepser, S.;
Kluzniak, W.; Komin, N.; Konno, R.; Kosack, K.; Kostunin, D.; Kreter,
M.; Kukec Mezek, G.; Kundu, A.; Lamanna, G.; Le Stum, S.; Lemiere, A.;
Lemoine-Goumard, M.; Lenain, J. P.; Leuschner, F.; Levy, C.; Lohse,
T.; Luashvili, A.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev, D.;
Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares, A.;
Marti'i-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P.; Meyer, M.;
Mitchell, A.; Moderski, R.; Mohrmann, L.; Montanari, A.; Moore, C.;
Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.; Naurois
(de), M.; Nayerhoda, A.; Davids, H.; Niemiec, J.; Noel, A.; O'Brien,
P.; Oberholzer, L. L.; Ohm, S.; Olivera-Nieto, L.; Ona-Wilhelmi (de),
E.; Ostrowski, M.; Panny, S.; Panter, M.; Parsons, D.; Peron, G.; Pita,
S.; Poireau, V.; Prokhorov, D.; Prokoph, H.; Puehlhofer, G.; Punch, M.;
Quirrenbach, A.; Reichherzer, P.; Reimer, A.; Reimer, O.; Remy, Q.;
Renaud, M.; Reville, B.; Rieger, F.; Romoli, C.; Rowell, G.; Rudak,
B.; Rueda Ricarte, H.; Ruiz Velasco, E.; Sahakian, V.; Sailer, S.;
Salzmann, H.; Sanchez, D.; Santangelo, A.; Sasaki, M.; Schaefer, J.;
Schutte, H.; Schwanke, U.; Schüssler, F.; Senniappan, M.; Seyffert,
A.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.; Sinha, A.;
Sol, H.; Spackman, H.; Specovius, A.; Spencer, S. T.; Spir-Jacob, M.;
Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steinmassl, S.; Steppa, C.;
Sun, L.; Takahashi, T.; Tanaka, T.; Tavernier, T.; Taylor, A.; Terrier,
R.; Thiersen, H.; Thorpe-Morgan, C.; Tluczykont, M.; Tomankova, L.;
Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, J.;
van Eldik, C.; van Rensburg, C.; van Soelen, B.; Vasileiadis, G.;
Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Völk, H. J.; Wagner, S.;
Watson, J. J.; Werner, F.; White, R.; Wierzcholska, A.; Wong, Y. W.;
Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin, R.; Zargaryan, D.;
Zdziarski, A.; Zech, A.; Zmija, A.; Zouari, S.; Żywucka, N.; Zhu, S.
2022icrc.confE.943S Altcode: 2022PoS...395E.943S
No abstract at ADS
---------------------------------------------------------
Title: LMC N132D: A mature supernova remnant with a power-law
gamma-ray spectrum extending beyond 8 TeV
Authors: H. E. S. S. Collaboration; Abdalla, H.; Aharonian, F.; Ait
Benkhali, F.; Angüner, E. O.; Arcaro, C.; Armand, C.; Armstrong,
T.; Ashkar, H.; Backes, M.; Baghmanyan, V.; Barbosa Martins, V.;
Barnacka, A.; Barnard, M.; Batzofin, R.; Becherini, Y.; Berge, D.;
Bernlöhr, K.; Bi, B.; Böttcher, M.; Boisson, C.; Bolmont, J.;
de Bony de Lavergne, M.; Breuhaus, M.; Brose, R.; Brun, F.; Bulik,
T.; Bylund, T.; Cangemi, F.; Caroff, S.; Casanova, S.; Catalano, J.;
Chambery, P.; Chand, T.; Chen, A.; Cotter, G.; Curyło, M.; Damascene
Mbarubucyeye, J.; Davids, I. D.; Davies, J.; Devin, J.; Djannati-Ataï,
A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.; Dreyer, L.; Du Plessis,
L.; Duffy, C.; Egberts, K.; Einecke, S.; Ernenwein, J. -P.; Fegan,
S.; Feijen, K.; Fiasson, A.; Fichet de Clairfontaine, G.; Fontaine,
G.; Lott, F.; Füßling, M.; Funk, S.; Gabici, S.; Gallant, Y. A.;
Giavitto, G.; Giunti, L.; Glawion, D.; Glicenstein, J. F.; Grondin,
M. -H.; Hattingh, S.; Haupt, M.; Hermann, G.; Hinton, J. A.; Hofmann,
W.; Hoischen, C.; Holch, T. L.; Holler, M.; Hörbe, M.; Horns, D.;
Huang, Zhiqiu; Huber, D.; Jamrozy, M.; Jankowsky, F.; Joshi, V.;
Jung-Richardt, I.; Kasai, E.; Katarzyński, K.; Katz, U.; Khangulyan,
D.; Khélifi, B.; Klepser, S.; Kluźniak, W.; Komin, Nu.; Konno, R.;
Kosack, K.; Kostunin, D.; Kreter, M.; Kukec Mezek, G.; Kundu, A.;
Lamanna, G.; Le Stum, S.; Lemière, A.; Lemoine-Goumard, M.; Lenain,
J. -P.; Leuschner, F.; Levy, C.; Lohse, T.; Luashvili, A.; Lypova, I.;
Mackey, J.; Majumdar, J.; Malyshev, D.; Malyshev, D.; Marandon, V.;
Marchegiani, P.; Marcowith, A.; Mares, A.; Martí-Devesa, G.; Marx,
R.; Maurin, G.; Meintjes, P. J.; Meyer, M.; Mitchell, A.; Moderski,
R.; Mohrmann, L.; Montanari, A.; Moore, C.; Moulin, E.; Muller, J.;
Murach, T.; Nakashima, K.; de Naurois, M.; Nayerhoda, A.; Ndiyavala,
H.; Niemiec, J.; Priyana Noel, A.; O'Brien, P.; Oberholzer, L.; Odaka,
H.; Ohm, S.; Olivera-Nieto, L.; de Ona Wilhelmi, E.; Ostrowski,
M.; Panny, S.; Panter, M.; Parsons, R. D.; Peron, G.; Pita, S.;
Poireau, V.; Prokhorov, D. A.; Prokoph, H.; Pühlhofer, G.; Punch, M.;
Quirrenbach, A.; Reichherzer, P.; Reimer, A.; Reimer, O.; Remy, Q.;
Renaud, M.; Reville, B.; Rieger, F.; Romoli, C.; Rowell, G.; Rudak,
B.; Rueda Ricarte, H.; Ruiz-Velasco, E.; Sahakian, V.; Sailer, S.;
Salzmann, H.; Sanchez, D. A.; Santangelo, A.; Sasaki, M.; Schäfer,
J.; Schüssler, F.; Schutte, H. M.; Schwanke, U.; Senniappan, M.;
Seyffert, A. S.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.;
Sinha, A.; Sol, H.; Specovius, A.; Spencer, S.; Spir-Jacob, M.;
Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Steinmassl, S.; Steppa,
C.; Sun, L.; Takahashi, T.; Tanaka, T.; Tavernier, T.; Taylor, A. M.;
Terrier, R.; Thiersen, J. H. E.; Thorpe-Morgan, C.; Tluczykont, M.;
Tomankova, L.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van
der Walt, D. J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.;
Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Völk,
H. J.; Wagner, S. J.; Watson, J.; Werner, F.; White, R.; Wierzcholska,
A.; Wong, Yu Wun; Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin,
R.; Zargaryan, D.; Zdziarski, A. A.; Zech, A.; Zhu, S. J.; Zmija,
A.; Zouari, S.; Żywucka, N.
2021A&A...655A...7H Altcode: 2021arXiv210802015H
Context. Supernova remnants (SNRs) are commonly thought to be the
dominant sources of Galactic cosmic rays up to the knee of the
cosmic-ray spectrum at a few PeV. Imaging Atmospheric Cherenkov
Telescopes have revealed young SNRs as very-high-energy (VHE, >100
GeV) gamma-ray sources, but for only a few SNRs the hadronic cosmic-ray
origin of their gamma-ray emission is indisputably established. In all
these cases, the gamma-ray spectra exhibit a spectral cutoff at energies
much below 100 TeV and thus do not reach the PeVatron regime. <BR />
Aims: The aim of this work was to achieve a firm detection for the
oxygen-rich SNR LMC N132D in the VHE gamma-ray domain with an extended
set of data, and to clarify the spectral characteristics and the
localization of the gamma-ray emission from this exceptionally powerful
gamma-ray-emitting SNR. <BR /> Methods: We analyzed 252 h of High Energy
Stereoscopic System (H.E.S.S.) observations towards SNR N132D that
were accumulated between December 2004 and March 2016 during a deep
survey of the Large Magellanic Cloud, adding 104 h of observations to
the previously published data set to ensure a > 5σ detection. To
broaden the gamma-ray spectral coverage required for modeling the
spectral energy distribution, an analysis of Fermi-LAT Pass 8 data was
also included. <BR /> Results: We unambiguously detect N132D at VHE with
a significance of 5.7σ. We report the results of a detailed analysis
of its spectrum and localization based on the extended H.E.S.S. data
set. The joint analysis of the extended H.E.S.S and Fermi-LAT data
results in a spectral energy distribution in the energy range from
1.7 GeV to 14.8 TeV, which suggests a high luminosity of N132D at GeV
and TeV energies. We set a lower limit on a gamma-ray cutoff energy
of 8 TeV with a confidence level of 95%. The new gamma-ray spectrum as
well as multiwavelength observations of N132D when compared to physical
models suggests a hadronic origin of the VHE gamma-ray emission. <BR />
Conclusions: SNR N132D is a VHE gamma-ray source that shows a spectrum
extending to the VHE domain without a spectral cutoff at a few TeV,
unlike the younger oxygen-rich SNR Cassiopeia A. The gamma-ray emission
is best explained by a dominant hadronic component formed by diffusive
shock acceleration. The gamma-ray properties of N132D may be affected
by an interaction with a nearby molecular cloud that partially lies
inside the 95% confidence region of the source position.
---------------------------------------------------------
Title: Searching for TeV Gamma-Ray Emission from SGR 1935+2154 during
Its 2020 X-Ray and Radio Bursting Phase
Authors: Abdalla, H.; Aharonian, F.; Ait Benkhali, F.; Angüner,
E. O.; Arcaro, C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes,
M.; Baghmanyan, V.; Barbosa Martins, V.; Barnacka, A.; Barnard,
M.; Becherini, Y.; Berge, D.; Bernlöhr, K.; Bi, B.; Böttcher,
M.; Boisson, C.; Bolmont, J.; de Bony de Lavergne, M.; Breuhaus,
M.; Brose, R.; Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik,
T.; Bylund, T.; Cangemi, F.; Caroff, S.; Carosi, A.; Casanova, S.;
Chambery, P.; Chand, T.; Chandra, S.; Chen, A.; Cotter, G.; Curyło,
M.; Damascene Mbarubucyeye, J.; Davids, I. D.; Davies, J.; Deil, C.;
Devin, J.; Dirson, L.; Djannati-Ataï, A.; Dmytriiev, A.; Donath,
A.; Doroshenko, V.; Dreyer, L.; Duffy, C.; Du Plessis, L.; Dyks,
J.; Egberts, K.; Eichhorn, F.; Einecke, S.; Emery, G.; Ernenwein,
J. -P.; Feijen, K.; Fegan, S.; Fiasson, A.; Fichet de Clairfontaine,
G.; Fontaine, G.; Funk, S.; Füßling, M.; Gabici, S.; Gallant, Y. A.;
Ghafourizade, S.; Giavitto, G.; Giunti, L.; Glawion, D.; Glicenstein,
J. F.; Grondin, M. -H.; Hahn, J.; Haupt, M.; Hattingh, S.; Hermann, G.;
Hinton, J. A.; Hofmann, W.; Hoischen, C.; Holch, T. L.; Holler, M.;
Hörbe, M.; Horns, D.; Huang, Z.; Huber, D.; Jamrozy, M.; Jankowsky,
D.; Jankowsky, F.; Jardin-Blicq, A.; Joshi, V.; Jung-Richardt, I.;
Kasai, E.; Kastendieck, M. A.; Katarzyński, K.; Katz, U.; Khangulyan,
D.; Khélifi, B.; Klepser, S.; Kluźniak, W.; Komin, Nu.; Konno, R.;
Kosack, K.; Kostunin, D.; Kreter, M.; Kukec Mezek, G.; Kundu, A.;
Lamanna, G.; Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Le
Stum, S.; Leuschner, F.; Levy, C.; Lohse, T.; Luashvili, A.; Lypova,
I.; Mackey, J.; Majumdar, J.; Malyshev, D.; Malyshev, D.; Marandon, V.;
Marchegiani, P.; Marcowith, A.; Mares, A.; Martí-Devesa, G.; Marx,
R.; Maurin, G.; Meintjes, P. J.; Meyer, M.; Mitchell, A.; Moderski,
R.; Mohrmann, L.; Montanari, A.; Moore, C.; Morris, P.; Moulin, E.;
Muller, J.; Murach, T.; Nakashima, K.; Nayerhoda, A.; de Naurois, M.;
Ndiyavala, H.; Niemiec, J.; Oakes, L.; O'Brien, P.; Odaka, H.; Ohm,
S.; Olivera-Nieto, L.; de Ona Wilhelmi, E.; Ostrowski, M.; Panny,
S.; Panter, M.; Parsons, R. D.; Peron, G.; Peyaud, B.; Piel, Q.;
Pita, S.; Poireau, V.; Priyana Noel, A.; Prokhorov, D. A.; Prokoph,
H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Rauth,
R.; Reichherzer, P.; Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.;
Reville, B.; Rieger, F.; Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak,
B.; Rueda Ricarte, H.; Ruiz-Velasco, E.; Sahakian, V.; Sailer, S.;
Salzmann, H.; Sanchez, D. A.; Santangelo, A.; Sasaki, M.; Schäfer,
J.; Schüssler, F.; Schutte, H. M.; Schwanke, U.; Seglar-Arroyo,
M.; Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shapopi, J. N. S.;
Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol, H.; Spackman, H.;
Specovius, A.; Spencer, S.; Spir-Jacob, M.; Stawarz, Ł.; Sun, L.;
Steenkamp, R.; Stegmann, C.; Steinmassl, S.; Steppa, C.; Takahashi,
T.; Tanaka, T.; Tavernier, T.; Taylor, A. M.; Terrier, R.; Thiersen,
J. H. E.; Thorpe-Morgan, C.; Tiziani, D.; Tluczykont, M.; Tomankova,
L.; Trichard, C.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.;
van der Walt, D. J.; van Eldik, C.; van Rensburg, C.; van Soelen,
B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.;
Völk, H. J.; Wadiasingh, Z.; Wagner, S. J.; Watson, J.; Werner, F.;
White, R.; Wierzcholska, A.; deWilt, P.; Wong, Yu Wun; Yassin, H.;
Yusafzai, A.; Zacharias, M.; Zanin, R.; Zargaryan, D.; Zdziarski,
A. A.; Zech, A.; Zhu, S. J.; Zorn, J.; Zouari, S.; Żywucka, N.;
H. E. S. S. Collaboration
2021ApJ...919..106A Altcode: 2021arXiv211000636H
Magnetar hyperflares are the most plausible explanation for fast
radio bursts (FRBs)-enigmatic powerful radio pulses with durations
of several milliseconds and high brightness temperatures. The first
observational evidence for this scenario was obtained in 2020 April
when an FRB was detected from the direction of the Galactic magnetar
and soft gamma-ray repeater SGR 1935+2154. The FRB was preceded by
two gamma-ray outburst alerts by the BAT instrument aboard the Swift
satellite, which triggered follow-up observations by the High Energy
Stereoscopic System (H.E.S.S.). H.E.S.S. observed SGR 1935+2154 for 2
hr on 2020 April 28. The observations are coincident with X-ray bursts
from the magnetar detected by INTEGRAL and Fermi-GBM, thus providing
the first very high energy gamma-ray observations of a magnetar in
a flaring state. High-quality data acquired during these follow-up
observations allow us to perform a search for short-time transients. No
significant signal at energies E > 0.6 TeV is found, and upper
limits on the persistent and transient emission are derived. We here
present the analysis of these observations and discuss the obtained
results and prospects of the H.E.S.S. follow-up program for soft
gamma-ray repeaters.
---------------------------------------------------------
Title: Search for Dark Matter Annihilation Signals from Unidentified
Fermi-LAT Objects with H.E.S.S.
Authors: Abdalla, H.; Aharonian, F.; Ait Benkhali, F.; Angüner,
E. O.; Arcaro, C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes,
M.; Baghmanyan, V.; Barbosa-Martins, V.; Barnacka, A.; Barnard, M.;
Becherini, Y.; Berge, D.; Bernlöhr, K.; Bi, B.; Böttcher, M.;
Boisson, C.; Bolmont, J.; de Bony de Lavergne, M.; Breuhaus, M.;
Brose, R.; Brun, F.; Bulik, T.; Bylund, T.; Cangemi, F.; Caroff,
S.; Casanova, S.; Chambery, P.; Catalano, J.; Chand, T.; Chen, A.;
Cotter, G.; Curyło, M.; Dalgleish, H.; Mbarubucyeye, J. Damascene;
Davids, I. D.; Davies, J.; Devin, J.; Djannati-Ataï, A.; Dmytriiev,
A.; Donath, A.; Doroshenko, V.; Dreyer, L.; du Plessis, L.; Duffy,
C.; Egberts, K.; Einecke, S.; Emery, G.; Ernenwein, J. -P.; Feijen,
K.; Fegan, S.; Fiasson, A.; de Clairfontaine, G. Fichet; Fontaine, G.;
Funk, S.; Füssling, M.; Gabici, S.; Gallant, Y. A.; Ghafourizade, S.;
Giavitto, G.; Giunti, L.; Glawion, D.; Glicenstein, J. F.; Grondin,
M. -H.; Hattingh, S.; Haupt, M.; Hermann, G.; Hinton, J. A.; Hofmann,
W.; Hoischen, C.; Holch, T. L.; Holler, M.; Hörbe, M.; Horns, D.;
Huang, Z.; Huber, D.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.;
Joshi, V.; Jung-Richardt, I.; Kasai, E.; Katarzyński, K.; Katz, U.;
Khangulyan, D.; Khélifi, B.; Klepser, S.; Kluźniak, W.; Komin, Nu.;
Konno, R.; Kosack, K.; Kostunin, D.; Kreter, M.; Kukec Mezek, G.;
Kundu, A.; Lamanna, G.; Le Stum, S.; Lemière, A.; Lemoine-Goumard,
M.; Lenain, J. -P.; Leuschner, F.; Levy, C.; Luashvili, A.; Lohse,
T.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev, D.; Malyshev, D.;
Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares, A.; Martí-Devesa,
G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Meyer, M.; Mitchell, A.;
Moderski, R.; Mohrmann, L.; Montanari, A.; Moore, C.; Morris, P.;
Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.; Nayerhoda, A.;
de Naurois, M.; Ndiyavala, H.; Niemiec, J.; Noel, A.; Oberholzer,
L.; O'Brien, P.; Ohm, S.; Olivera-Nieto, L.; de Ona Wilhelmi, E.;
Ostrowski, M.; Panter, M.; Panny, S.; Parsons, R. D.; Peron, G.;
Pita, S.; Poireau, V.; Prokhorov, D. A.; Prokoph, H.; Pühlhofer,
G.; Punch, M.; Quirrenbach, A.; Reichherzer, P.; Reimer, A.; Reimer,
O.; Remy, Q.; Renaud, M.; Rieger, F.; Romoli, C.; Rowell, G.; Rudak,
B.; Rueda Ricarte, H.; Ruiz-Velasco, E.; Sahakian, V.; Sailer, S.;
Salzmann, H.; Sanchez, D. A.; Santangelo, A.; Sasaki, M.; Schäfer, J.;
Schüssler, F.; Schutte, H. M.; Schwanke, U.; Senniappan, M.; Seyffert,
A. S.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.; Sinha, A.;
Spackman, H.; Sol, H.; Specovius, A.; Spencer, S.; Spir-Jacob, M.;
Stawarz, Ł.; Sun, L.; Steenkamp, R.; Stegmann, C.; Steinmassl, S.;
Steppa, C.; Takahashi, T.; Tanaka, T.; Tavernier, T.; Taylor, A. M.;
Terrier, R.; Thorpe-Morgan, C.; Thiersen, J. H. E.; Tluczykont, M.;
Tomankova, L.; Tsirou, M.; Tsuji, M.; Tuffs, R.; Uchiyama, Y.; van
der Walt, D. J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.;
Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Viana, A.; Vink,
J.; Völk, H. J.; Wagner, S. J.; Werner, F.; White, R.; Wierzcholska,
A.; Wong, Yu Wun; Yassin, H.; Yusafzai, A.; Zacharias, M.; Zanin,
R.; Zargaryan, D.; Zdziarski, A. A.; Zech, A.; Zhu, S. J.; Zmija,
A.; Zorn, J.; Zouari, S.; Żywucka, N.; H. E. S. S. Collaboration
2021ApJ...918...17A Altcode: 2021arXiv210600551H
Cosmological N-body simulations show that Milky Way-sized galaxies
harbor a population of unmerged dark matter (DM) subhalos. These
subhalos could shine in gamma-rays and eventually be detected in
gamma-ray surveys as unidentified sources. We performed a thorough
selection among unidentified Fermi-Large Area Telescope Objects
(UFOs) to identify them as possible tera-electron-volt-scale DM
subhalo candidates. We search for very-high-energy (E ≳ 100 GeV)
gamma-ray emissions using H.E.S.S. observations toward four selected
UFOs. Since no significant very-high-energy gamma-ray emission is
detected in any data set of the four observed UFOs or in the combined
UFO data set, strong constraints are derived on the product of the
velocity-weighted annihilation cross section ⟨σv⟩ by the J
factor for the DM models. The 95% confidence level observed upper
limits derived from combined H.E.S.S. observations reach ⟨σv⟩J
values of 3.7 × 10<SUP>-5</SUP> and 8.1 × 10<SUP>-6</SUP> GeV<SUP>2
</SUP>cm<SUP>-2 </SUP>s<SUP>-1</SUP> in the W<SUP>+</SUP>W<SUP>-</SUP>
and τ<SUP>+</SUP>τ<SUP>-</SUP> channels, respectively, for a
1 TeV DM mass. Focusing on thermal weakly interacting massive
particles, the H.E.S.S. constraints restrict the J factors to lie
in the range 6.1 × 10<SUP>19</SUP>-2.0 × 10<SUP>21</SUP> GeV<SUP>2
</SUP>cm<SUP>-5</SUP> and the masses to lie between 0.2 and 6 TeV in the
W<SUP>+</SUP>W<SUP>-</SUP> channel. For the τ<SUP>+</SUP>τ<SUP>-</SUP>
channel, the J factors lie in the range 7.0 × 10<SUP>19</SUP>-7.1 ×
10<SUP>20</SUP> GeV<SUP>2 </SUP>cm<SUP>-5</SUP> and the masses lie
between 0.2 and 0.5 TeV. Assuming model-dependent predictions from
cosmological N-body simulations on the J-factor distribution for Milky
Way-sized galaxies, the DM models with masses >0.3 TeV for the UFO
emissions can be ruled out at high confidence level.
---------------------------------------------------------
Title: Evidence of 100 TeV γ-ray emission from HESS J1702-420:
A new PeVatron candidate
Authors: Abdalla, H.; Aharonian, F.; Ait Benkhali, F.; Angüner,
E. O.; Arcaro, C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes,
M.; Baghmanyan, V.; Barbosa Martins, V.; Barnacka, A.; Barnard, M.;
Becherini, Y.; Berge, D.; Bernlöhr, K.; Bi, B.; Böttcher, M.;
Boisson, C.; Bolmont, J.; de Bony de Lavergne, M.; Breuhaus, M.;
Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.; Bylund, T.;
Caroff, S.; Carosi, A.; Casanova, S.; Chand, T.; Chandra, S.; Chen,
A.; Cotter, G.; Curyło, M.; Damascene Mbarubucyeye, J.; Davids,
I. D.; Davies, J.; Deil, C.; Devin, J.; Dirson, L.; Djannati-Ataï,
A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.; Dreyer, L.; Duffy, C.;
Dyks, J.; Egberts, K.; Eichhorn, F.; Einecke, S.; Emery, G.; Ernenwein,
J. -P.; Feijen, K.; Fegan, S.; Fiasson, A.; Fichet de Clairfontaine,
G.; Fontaine, G.; Funk, S.; Füßling, M.; Gabici, S.; Gallant, Y. A.;
Giavitto, G.; Giunti, L.; Glawion, D.; Glicenstein, J. F.; Grondin,
M. -H.; Hahn, J.; Haupt, M.; Hermann, G.; Hinton, J. A.; Hofmann, W.;
Hoischen, C.; Holch, T. L.; Holler, M.; Hörbe, M.; Horns, D.; Huber,
D.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.; Jardin-Blicq, A.; Joshi,
V.; Jung-Richardt, I.; Kasai, E.; Kastendieck, M. A.; Katarzyński,
K.; Katz, U.; Khangulyan, D.; Khélifi, B.; Klepser, S.; Kluźniak, W.;
Komin, Nu.; Konno, R.; Kosack, K.; Kostunin, D.; Kreter, M.; Lamanna,
G.; Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leuschner, F.;
Levy, C.; Lohse, T.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev,
D.; Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares,
A.; Martí-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Meyer,
M.; Mitchell, A.; Moderski, R.; Mohrmann, L.; Montanari, A.; Moore,
C.; Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.;
Nayerhoda, A.; de Naurois, M.; Ndiyavala, H.; Niemiec, J.; Oakes, L.;
O'Brien, P.; Odaka, H.; Ohm, S.; Olivera-Nieto, L.; de Ona Wilhelmi,
E.; Ostrowski, M.; Panny, S.; Panter, M.; Parsons, R. D.; Peron,
G.; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V.; Priyana Noel, A.;
Prokhorov, D. A.; Prokoph, H.; Pühlhofer, G.; Punch, M.; Quirrenbach,
A.; Raab, S.; Rauth, R.; Reichherzer, P.; Reimer, A.; Reimer, O.; Remy,
Q.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli, C.; Rowell, G.;
Rudak, B.; Ruiz-Velasco, E.; Sahakian, V.; Sailer, S.; Salzmann, H.;
Sanchez, D. A.; Santangelo, A.; Sasaki, M.; Scalici, M.; Schäfer,
J.; Schüssler, F.; Schutte, H. M.; Schwanke, U.; Seglar-Arroyo,
M.; Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shapopi, J. N. S.;
Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol, H.; Specovius, A.;
Spencer, S.; Spir-Jacob, M.; Stawarz, Ł.; Sun, L.; Steenkamp, R.;
Stegmann, C.; Steinmassl, S.; Steppa, C.; Takahashi, T.; Tavernier,
T.; Taylor, A. M.; Terrier, R.; Thiersen, J. H. E.; Tiziani, D.;
Tluczykont, M.; Tomankova, L.; Trichard, C.; Tsirou, M.; Tuffs, R.;
Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.; van Rensburg, C.;
van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.;
Vink, J.; Völk, H. J.; Wadiasingh, Z.; Wagner, S. J.; Watson, J.;
Werner, F.; White, R.; Wierzcholska, A.; Wun Wong, Yu; Yusafzai, A.;
Zacharias, M.; Zanin, R.; Zargaryan, D.; Zdziarski, A. A.; Zech, A.;
Zhu, S. J.; Zorn, J.; Zouari, S.; Żywucka, N.
2021A&A...653A.152A Altcode: 2021arXiv210606405G; 2021arXiv210606405A
<BR /> Aims: The identification of PeVatrons, hadronic particle
accelerators reaching the knee of the cosmic ray spectrum (few ×
10<SUP>15</SUP> eV), is crucial to understand the origin of cosmic
rays in the Galaxy. We provide an update on the unidentified source
HESS J1702-420, a promising PeVatron candidate. <BR /> Methods:
We present new observations of HESS J1702-420 made with the High
Energy Stereoscopic System (H.E.S.S.), and processed using improved
analysis techniques. The analysis configuration was optimized to
enhance the collection area at the highest energies. We applied a
three-dimensional likelihood analysis to model the source region and
adjust non thermal radiative spectral models to the γ-ray data. We
also analyzed archival Fermi Large Area Telescope data to constrain
the source spectrum at γ-ray energies > 10 GeV. <BR /> Results: We
report the detection of γ-rays up to 100 TeV from a specific region
of HESS J1702-420, which is well described by a new source component
called HESS J1702-420A that was separated from the bulk of TeV emission
at a 5.4σ confidence level. The power law γ-ray spectrum of HESS
J1702-420A extends with an index of Γ = 1.53 ± 0.19<SUB>stat</SUB>
± 0.20<SUB>sys</SUB> and without curvature up to the energy
band 64−113 TeV, in which it was detected by H.E.S.S. at a 4.0σ
confidence level. This makes HESS J1702-420A a compelling candidate
site for the presence of extremely high energy cosmic rays. With a flux
above 2 TeV of (2.08 ± 0.49<SUB>stat</SUB> ± 0.62<SUB>sys</SUB>)
× 10<SUP>−13</SUP> cm<SUP>−2</SUP> s<SUP>−1</SUP> and a
radius of (0.06 ± 0.02<SUB>stat</SUB> ± 0.03<SUB>sys</SUB>)°, HESS
J1702-420A is outshone - below a few tens of TeV - by the companion
HESS J1702-420B. The latter has a steep spectral index of Γ = 2.62
± 0.10<SUB>stat</SUB> ± 0.20<SUB>sys</SUB> and an elongated shape,
and it accounts for most of the low-energy HESS J1702-420 flux. Simple
hadronic and leptonic emission models can be well adjusted to the
spectra of both components. Remarkably, in a hadronic scenario, the
cut-off energy of the particle distribution powering HESS J1702-420A
is found to be higher than 0.5 PeV at a 95% confidence level. <BR />
Conclusions: For the first time, H.E.S.S. resolved two components
with significantly different morphologies and spectral indices,
both detected at > 5σ confidence level, whose combined emissions
result in the source HESS J1702-420. We detected HESS J1702-420A at a
4.0σ confidence level in the energy band 64−113 TeV, which brings
evidence for the source emission up to 100 TeV. In a hadronic emission
scenario, the hard γ-ray spectrum of HESS J1702-420A implies that
the source likely harbors PeV protons, thus becoming one of the most
solid PeVatron candidates detected so far in H.E.S.S. data. However, a
leptonic origin of the observed TeV emission cannot be ruled out either.
---------------------------------------------------------
Title: TeV Emission of Galactic Plane Sources with HAWC and H.E.S.S.
Authors: Abdalla, H.; Aharonian, F.; Ait Benkhali, F.; Angüner,
E. O.; Arcaro, C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes,
M.; Baghmanyan, V.; Barbosa Martins, V.; Barnacka, A.; Barnard,
M.; Becherini, Y.; Berge, D.; Bernlöhr, K.; Bi, B.; Böttcher, M.;
Boisson, C.; Bolmont, J.; de Bonyde Lavergne, M.; Breuhaus, M.; Brose,
R.; Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.; Bylund, T.;
Caroff, S.; Carosi, A.; Chand, T.; Chandra, S.; Chen, A.; Cotter, G.;
Curyło, M.; Damascene Mbarubucyeye, J.; Davids, I. D.; Davies, J.;
Deil, C.; Devin, J.; Dirson, L.; Djannati-Ataï, A.; Dmytriiev, A.;
Donath, A.; Doroshenko, V.; Dreyer, L.; Duffy, C.; Dyks, J.; Egberts,
K.; Eichhorn, F.; Einecke, S.; Emery, G.; Ernenwein, J. -P.; Feijen,
K.; Fegan, S.; Fiasson, A.; Fichet de Clairfontaine, G.; Fontaine,
G.; Funk, S.; Füßling, M.; Gabici, S.; Gallant, Y. A.; Giavitto,
G.; Giunti, L.; Glawion, D.; Glicenstein, J. F.; Gottschall, D.;
Grondin, M. -H.; Hahn, J.; Haupt, M.; Hermann, G.; Hinton, J. A.;
Hofmann, W.; Hoischen, C.; Holch, T. L.; Holler, M.; Hörbe, M.;
Horns, D.; Huber, D.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.;
Jung-Richardt, I.; Kasai, E.; Kastendieck, M. A.; Katarzyński, K.;
Katz, U.; Khangulyan, D.; Khélifi, B.; Klepser, S.; Kluźniak, W.;
Komin, Nu.; Konno, R.; Kosack, K.; Kostunin, D.; Kreter, M.; Lamanna,
G.; Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leuschner, F.;
Levy, C.; Lohse, T.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev,
D.; Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares,
A.; Martí-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Meyer,
M.; Mitchell, A. M. W.; Moderski, R.; Mohrmann, L.; Montanari, A.;
Moore, C.; Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima,
K.; Nayerhoda, A.; de Naurois, M.; Ndiyavala, H.; Niemiec, J.;
Oakes, L.; O'Brien, P.; Odaka, H.; Ohm, S.; Olivera-Nieto, L.; de
Ona Wilhelmi, E.; Ostrowski, M.; Panter, M.; Panny, S.; Parsons,
R. D.; Peron, G.; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V.;
Priyana Noel, A.; Prokhorov, D. A.; Prokoph, H.; Pühlhofer, G.;
Punch, M.; Quirrenbach, A.; Raab, S.; Rauth, R.; Reichherzer, P.;
Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Rieger, F.; Rinchiuso,
L.; Romoli, C.; Rowell, G.; Rudak, B.; Sahakian, V.; Sailer, S.;
Salzmann, H.; Sanchez, D. A.; Santangelo, A.; Sasaki, M.; Schäfer,
J.; Schüssler, F.; Schutte, H. M.; Schwanke, U.; Seglar-Arroyo,
M.; Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shapopi, J. N. S.;
Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol, H.; Specovius, A.;
Spencer, S.; Spir-Jacob, M.; Stawarz, Ł.; Sun, L.; Steenkamp, R.;
Stegmann, C.; Steinmassl, S.; Steppa, C.; Takahashi, T.; Tavernier,
T.; Taylor, A. M.; Terrier, R.; Thiersen, J. H. E.; Tiziani, D.;
Tluczykont, M.; Tomankova, L.; Trichard, C.; Tsirou, M.; Tuffs, R.;
Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.; van Rensburg, C.;
van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.;
Vink, J.; Völk, H. J.; Wadiasingh, Z.; Wagner, S. J.; Watson, J.;
Werner, F.; White, R.; Wierzcholska, A.; Wong, Yu Wun; Yusafzai, A.;
Zacharias, M.; Zanin, R.; Zargaryan, D.; Zdziarski, A. A.; Zech, A.;
Zhu, S. J.; Zmija, A.; Zorn, J.; Zouari, S.; Żywucka, N.; Albert,
A.; Alfaro, R.; Alvarez, C.; Arteaga-Velézquez, J. C.; Arunbabu,
K. P.; Avila Rojas, D.; Belmont-Moreno, E.; BenZvi, S. Y.; Brisbois,
C.; Caballero-Mora, K. S.; Capistrán, T.; Carramiñana, A.; Casanova,
S.; Cotti, U.; Cotzomi, J.; Coutiño de León, S.; De la Fuente, E.;
de León, C.; Diaz Hernandez, R.; Díaz-Vélez, J. C.; Dingus, B. L.;
DuVernois, M. A.; Durocher, M.; Ellsworth, R. W.; Engel, K.; Espinoza,
C.; Fan, K. L.; Fernández Alonso, M.; Fraija, N.; Galván-Gámez,
A.; Garcia, D.; García-González, J. A.; Garfias, F.; Giacinti, G.;
González, M. M.; Goodman, J. A.; Harding, J. P.; Hernandez, S.; Hona,
B.; Huang, D.; Hueyotl-Zahuantitla, F.; Hüntemeyer, P.; Iriarte, A.;
Jardin-Blicq, A.; Joshi, V.; Kieda, D.; Lee, W. H.; León Vargas, H.;
Linnemann, J. T.; Longinotti, A. L.; Luis-Raya, G.; López-Coto, R.;
Malone, K.; Martinez, O.; Martinez-Castellanos, I.; Martínez-Castro,
J.; Matthews, J. A.; Miranda-Romagnoli, P.; Morales-Soto, J. A.;
Moreno, E.; Mostafá, M.; Nayerhoda, A.; Nellen, L.; Newbold, M.;
Nisa, M. U.; Noriega-Papaqui, R.; Omodei, N.; Peisker, A.; Pérez
Araujo, Y.; Pérez-Pérez, E. G.; Rho, C. D.; Rosa-González, D.;
Ruiz-Velasco, E.; Salesa Greus, F.; Sandoval, A.; Schneider, M.;
Schoorlemmer, H.; Serna-Franco, J.; Smith, A. J.; Springer, R. W.;
Surajbali, P.; Tollefson, K.; Torres, I.; Torres-Escobedo, R.; Turner,
R.; Ureña-Mena, F.; Villaseñor, L.; Weisgarber, T.; Willox, E.;
Zhou, H.; HAWC Collaboration
2021ApJ...917....6A Altcode: 2021arXiv210701425A
The High Altitude Water Cherenkov (HAWC) observatory and the High
Energy Stereoscopic System (H.E.S.S.) are two leading instruments
in the ground-based very-high-energy γ-ray domain. HAWC employs
the water Cherenkov detection (WCD) technique, while H.E.S.S. is
an array of Imaging Atmospheric Cherenkov Telescopes (IACTs). The
two facilities therefore differ in multiple aspects, including their
observation strategy, the size of their field of view, and their angular
resolution, leading to different analysis approaches. Until now, it has
been unclear if the results of observations by both types of instruments
are consistent: several of the recently discovered HAWC sources have
been followed up by IACTs, resulting in a confirmed detection only in
a minority of cases. With this paper, we go further and try to resolve
the tensions between previous results by performing a new analysis of
the H.E.S.S. Galactic plane survey data, applying an analysis technique
comparable between H.E.S.S. and HAWC. Events above 1 TeV are selected
for both data sets, the point-spread function of H.E.S.S. is broadened
to approach that of HAWC, and a similar background estimation method
is used. This is the first detailed comparison of the Galactic plane
observed by both instruments. H.E.S.S. can confirm the γ-ray emission
of four HAWC sources among seven previously undetected by IACTs,
while the three others have measured fluxes below the sensitivity of
the H.E.S.S. data set. Remaining differences in the overall γ-ray flux
can be explained by the systematic uncertainties. Therefore, we confirm
a consistent view of the γ-ray sky between WCD and IACT techniques.
---------------------------------------------------------
Title: Revealing x-ray and gamma ray temporal and spectral
similarities in the GRB 190829A afterglow
Authors: H. E. S. S. Collaboration; Abdalla, H.; Aharonian, F.; Ait
Benkhali, F.; Angüner, E. O.; Arcaro, C.; Armand, C.; Armstrong,
T.; Ashkar, H.; Backes, M.; Baghmanyan, V.; Barbosa Martins, V.;
Barnacka, A.; Barnard, M.; Becherini, Y.; Berge, D.; Bernlöhr,
K.; Bi, B.; Bissaldi, E.; Böttcher, M.; Boisson, C.; Bolmont, J.;
de Bony de Lavergne, M.; Breuhaus, M.; Brun, F.; Brun, P.; Bryan,
M.; Büchele, M.; Bulik, T.; Bylund, T.; Caroff, S.; Carosi, A.;
Casanova, S.; Chand, T.; Chandra, S.; Chen, A.; Cotter, G.; Curyło,
M.; Damascene Mbarubucyeye, J.; Davids, I. D.; Davies, J.; Deil, C.;
Devin, J.; Dirson, L.; Djannati-Ataï, A.; Dmytriiev, A.; Donath,
A.; Doroshenko, V.; Dreyer, L.; Duffy, C.; Dyks, J.; Egberts, K.;
Eichhorn, F.; Einecke, S.; Emery, G.; Ernenwein, J. -P.; Feijen, K.;
Fegan, S.; Fiasson, A.; Fichet de Clairfontaine, G.; Fontaine, G.;
Funk, S.; Füßling, M.; Gabici, S.; Gallant, Y. A.; Giavitto, G.;
Giunti, L.; Glawion, D.; Glicenstein, J. F.; Grondin, M. -H.; Hahn,
J.; Haupt, M.; Hermann, G.; Hinton, J. A.; Hofmann, W.; Hoischen,
C.; Holch, T. L.; Holler, M.; Hörbe, M.; Horns, D.; Huber, D.;
Jamrozy, M.; Jankowsky, D.; Jankowsky, F.; Jardin-Blicq, A.; Joshi,
V.; Jung-Richardt, I.; Kasai, E.; Kastendieck, M. A.; Katarzyński,
K.; Katz, U.; Khangulyan, D.; Khélifi, B.; Klepser, S.; Kluźniak, W.;
Komin, Nu.; Konno, R.; Kosack, K.; Kostunin, D.; Kreter, M.; Lamanna,
G.; Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leuschner, F.;
Levy, C.; Lohse, T.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev,
D.; Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares,
A.; Martí-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Meyer,
M.; Mitchell, A.; Moderski, R.; Mohrmann, L.; Montanari, A.; Moore,
C.; Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.;
Nayerhoda, A.; de Naurois, M.; Ndiyavala, H.; Niemiec, J.; Oakes, L.;
O'Brien, P.; Odaka, H.; Ohm, S.; Olivera-Nieto, L.; de Ona Wilhelmi,
E.; Ostrowski, M.; Panny, S.; Panter, M.; Parsons, R. D.; Peron,
G.; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V.; Priyana Noel, A.;
Prokhorov, D. A.; Prokoph, H.; Pühlhofer, G.; Punch, M.; Quirrenbach,
A.; Raab, S.; Rauth, R.; Reichherzer, P.; Reimer, A.; Reimer, O.; Remy,
Q.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli, C.; Rowell, G.;
Rudak, B.; Ruiz-Velasco, E.; Sahakian, V.; Sailer, S.; Salzmann, H.;
Sanchez, D. A.; Santangelo, A.; Sasaki, M.; Scalici, M.; Schäfer,
J.; Schüssler, F.; Schutte, H. M.; Schwanke, U.; Seglar-Arroyo,
M.; Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shapopi, J. N. S.;
Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol, H.; Specovius, A.;
Spencer, S.; Spir-Jacob, M.; Stawarz, Ł.; Sun, L.; Steenkamp,
R.; Stegmann, C.; Steinmassl, S.; Steppa, C.; Takahashi, T.; Tam,
T.; Tavernier, T.; Taylor, A. M.; Terrier, R.; Thiersen, J. H. E.;
Tiziani, D.; Tluczykont, M.; Tomankova, L.; Tsirou, M.; Tuffs, R.;
Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.; van Rensburg, C.;
van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.;
Vink, J.; Völk, H. J.; Wadiasingh, Z.; Wagner, S. J.; Watson, J.;
Werner, F.; White, R.; Wierzcholska, A.; Wong, Yu Wun; Yusafzai, A.;
Zacharias, M.; Zanin, R.; Zargaryan, D.; Zdziarski, A. A.; Zech, A.;
Zhu, S. J.; Zorn, J.; Zouari, S.; Żywucka, N.; Evans, P.; Page, K.
2021Sci...372.1081H Altcode: 2021arXiv210602510H
Gamma-ray bursts (GRBs), which are bright flashes of gamma rays
from extragalactic sources followed by fading afterglow emission,
are associated with stellar core collapse events. We report the
detection of very-high-energy (VHE) gamma rays from the afterglow of
GRB 190829A, between 4 and 56 hours after the trigger, using the High
Energy Stereoscopic System (H.E.S.S.). The low luminosity and redshift
of GRB 190829A reduce both internal and external absorption, allowing
determination of its intrinsic energy spectrum. Between energies
of 0.18 and 3.3 tera-electron volts, this spectrum is described by
a power law with photon index of 2.07 ± 0.09, similar to the x-ray
spectrum. The x-ray and VHE gamma-ray light curves also show similar
decay profiles. These similar characteristics in the x-ray and gamma-ray
bands challenge GRB afterglow emission scenarios.
---------------------------------------------------------
Title: Search for dark matter annihilation in the
Wolf-Lundmark-Melotte dwarf irregular galaxy with H.E.S.S.
Authors: Abdallah, H.; Adam, R.; Aharonian, F.; Benkhali, F. Ait;
Angüner, E. O.; Arcaro, C.; Armand, C.; Armstrong, T.; Ashkar, H.;
Backes, M.; Baghmanyan, V.; Martins, V. Barbosa; Barnacka, A.; Barnard,
M.; Becherini, Y.; Berge, D.; Bernlöhr, K.; Bi, B.; Böttcher, M.;
Boisson, C.; Bolmont, J.; de Lavergne, M. de Bony; Breuhaus, M.; Brun,
F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.; Bylund, T.; Caroff,
S.; Carosi, A.; Casanova, S.; Chand, T.; Chandra, S.; Chen, A.; Cotter,
G.; Curyło, M.; Mbarubucyeye, J. Damascene; Davids, I. D.; Davies,
J.; Deil, C.; Devin, J.; deWilt, P.; Dirson, L.; Djannati-Ataï,
A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.; Duffy, C.; Dyks, J.;
Egberts, K.; Eichhorn, F.; Einecke, S.; Emery, G.; Ernenwein, J. -P.;
Feijen, K.; Fegan, S.; Fiasson, A.; de Clairfontaine, G. Fichet;
Fontaine, G.; Funk, S.; Füßling, M.; Gabici, S.; Gallant, Y. A.;
Giavitto, G.; Giunti, L.; Glawion, D.; Glicenstein, J. F.; Gottschall,
D.; Grondin, M. -H.; Hahn, J.; Haupt, M.; Hermann, G.; Hinton, J. A.;
Hofmann, W.; Hoischen, C.; Holch, T. L.; Holler, M.; Hörbe, M.; Horns,
D.; Huber, D.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.; Jardin-Blicq,
A.; Joshi, V.; Jung-Richardt, I.; Kasai, E.; Kastendieck, M. A.;
Katarzyński, K.; Katz, U.; Khangulyan, D.; Khélifi, B.; Klepser, S.;
Kluźniak, W.; Komin, Nu.; Konno, R.; Kosack, K.; Kostunin, D.; Kreter,
M.; Lamanna, G.; Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.;
Levy, C.; Lohse, T.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev,
D.; Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith, A.;
Mares, A.; Martı-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.;
Meyer, M.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Montanari, A.;
Moore, C.; Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima,
K.; Nayerhoda, A.; de Naurois, M.; Ndiyavala, H.; Niederwanger, F.;
Niemiec, J.; Oakes, L.; O'Brien, P.; Odaka, H.; Ohm, S.; Olivera-Nieto,
L.; Wilhelmi, E. de Ona; Ostrowski, M.; Panter, M.; Panny, S.; Parsons,
R. D.; Peron, G.; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V.; Noel,
A. Priyana; Prokhorov, D. A.; Prokoph, H.; Pühlhofer, G.; Punch, M.;
Quirrenbach, A.; Raab, S.; Rauth, R.; Reichherzer, P.; Reimer, A.;
Reimer, O.; Remy, Q.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli,
C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.; Sahakian, V.; Sailer, S.;
Sanchez, D. A.; Santangelo, A.; Sasaki, M.; Scalici, M.; Schüssler,
F.; Schutte, H. M.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.;
Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shiningayamwe, K.; Simoni,
R.; Sinha, A.; Sol, H.; Specovius, A.; Spencer, S.; Spir-Jacob, M.;
Stawarz, Ł.; Sun, L.; Steenkamp, R.; Stegmann, C.; Steinmassl, S.;
Steppa, C.; Takahashi, T.; Tavernier, T.; Taylor, A. M.; Terrier,
R.; Tiziani, D.; Tluczykont, M.; Tomankova, L.; Trichard, C.; Tsirou,
M.; Tuffs, R.; Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.; van
Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.;
Vincent, P.; Vink, J.; Völk, H. J.; Vuillaume, T.; Wadiasingh, Z.;
Wagner, S. J.; Watson, J.; Werner, F.; White, R.; Wierzcholska, A.;
Wong, Yu Wun; Yusafzai, A.; Zacharias, M.; Zanin, R.; Zargaryan, D.;
Zdziarski, A. A.; Zech, A.; Zhu, S.; Zorn, J.; Zouari, S.; Zaywucka,
N.; H. E. S. S. Collaboration
2021PhRvD.103j2002A Altcode: 2021arXiv210504325H
We search for an indirect signal of dark matter through very
high-energy γ rays from the Wolf-Lundmark-Melotte (WLM) dwarf
irregular galaxy. The pair annihilation of dark matter particles would
produce Standard Model particles in the final state such as γ rays,
which might be detected by ground-based Cherenkov telescopes. Dwarf
irregular galaxies represent promising targets as they are dark
matter dominated objects with well-measured kinematics and small
uncertainties on their dark matter distribution profiles. In 2018,
the five-telescopes of the high energy stereoscopic system observed
the dwarf irregular galaxy WLM for 18 hours. We present the first
analysis based on data obtained from an imaging atmospheric Cherenkov
telescope for this subclass of dwarf galaxy. As we do not observe any
significant excess in the direction of WLM, we interpret the result
in terms of constraints on the velocity-weighted cross section for
dark matter pair annihilation ⟨σ v ⟩ as a function of the dark
matter particle mass for various continuum channels, as well as the
prompt γ γ emission. For the τ<SUP>+</SUP>τ<SUP>-</SUP> channel,
the limits reach a ⟨σ v ⟩ value of about 4 ×10<SUP>-22</SUP>
cm<SUP>3</SUP> s<SUP>-1</SUP> for a dark matter particle mass of 1
TeV. For the prompt γ γ channel, the upper limit reaches a ⟨σ v
⟩ value of about 5 ×10<SUP>-24</SUP> cm<SUP>3</SUP> s<SUP>-1</SUP>
for a mass of 370 GeV. These limits represent an improvement of up to
a factor 200, with respect to previous results for the dwarf irregular
galaxies for TeV dark matter search.
---------------------------------------------------------
Title: Broadband Multi-wavelength Properties of M87 during the 2017
Event Horizon Telescope Campaign
Authors: EHT MWL Science Working Group; Algaba, J. C.; Anczarski,
J.; Asada, K.; Baloković, M.; Chandra, S.; Cui, Y. -Z.; Falcone,
A. D.; Giroletti, M.; Goddi, C.; Hada, K.; Haggard, D.; Jorstad,
S.; Kaur, A.; Kawashima, T.; Keating, G.; Kim, J. -Y.; Kino, M.;
Komossa, S.; Kravchenko, E. V.; Krichbaum, T. P.; Lee, S. -S.;
Lu, R. -S.; Lucchini, M.; Markoff, S.; Neilsen, J.; Nowak, M. A.;
Park, J.; Principe, G.; Ramakrishnan, V.; Reynolds, M. T.; Sasada,
M.; Savchenko, S. S.; Williamson, K. E.; Event Horizon Telescope
Collaboration; Akiyama, Kazunori; Alberdi, Antxon; Alef, Walter;
Anantua, Richard; Azulay, Rebecca; Baczko, Anne-Kathrin; Ball, David;
Barrett, John; Bintley, Dan; Benson, Bradford A.; Blackburn, Lindy;
Blundell, Raymond; Boland, Wilfred; Bouman, Katherine L.; Bower,
Geoffrey C.; Boyce, Hope; Bremer, Michael; Brinkerink, Christiaan D.;
Brissenden, Roger; Britzen, Silke; Broderick, Avery E.; Broguiere,
Dominique; Bronzwaer, Thomas; Byun, Do-Young; Carlstrom, John E.;
Chael, Andrew; Chan, Chi-Kwan; Chatterjee, Shami; Chatterjee, Koushik;
Chen, Ming-Tang; Chen, Yongjun; Chesler, Paul M.; Cho, Ilje; Christian,
Pierre; Conway, John E.; Cordes, James M.; Crawford, Thomas M.; Crew,
Geoffrey B.; Cruz-Osorio, Alejandro; Davelaar, Jordy; de Laurentis,
Mariafelicia; Deane, Roger; Dempsey, Jessica; Desvignes, Gregory;
Dexter, Jason; Doeleman, Sheperd S.; Eatough, Ralph P.; Falcke, Heino;
Farah, Joseph; Fish, Vincent L.; Fomalont, Ed; Ford, H. Alyson;
Fraga-Encinas, Raquel; Friberg, Per; Fromm, Christian M.; Fuentes,
Antonio; Galison, Peter; Gammie, Charles F.; García, Roberto; Gentaz,
Olivier; Georgiev, Boris; Gold, Roman; Gómez, José L.; Gómez-Ruiz,
Arturo I.; Gu, Minfeng; Gurwell, Mark; Hecht, Michael H.; Hesper,
Ronald; Ho, Luis C.; Ho, Paul; Honma, Mareki; Huang, Chih-Wei L.;
Huang, Lei; Hughes, David H.; Ikeda, Shiro; Inoue, Makoto; Issaoun,
Sara; James, David J.; Jannuzi, Buell T.; Janssen, Michael; Jeter,
Britton; Jiang, Wu; Jiménez-Rosales, Alejandra; Johnson, Michael D.;
Jung, Taehyun; Karami, Mansour; Karuppusamy, Ramesh; Kettenis, Mark;
Kim, Dong-Jin; Kim, Jongsoo; Kim, Junhan; Koay, Jun Yi; Kofuji,
Yutaro; Koch, Patrick M.; Koyama, Shoko; Kramer, Michael; Kramer,
Carsten; Kuo, Cheng-Yu; Lauer, Tod R.; Levis, Aviad; Li, Yan-Rong;
Li, Zhiyuan; Lindqvist, Michael; Lico, Rocco; Lindahl, Greg; Liu,
Jun; Liu, Kuo; Liuzzo, Elisabetta; Lo, Wen-Ping; Lobanov, Andrei P.;
Loinard, Laurent; Lonsdale, Colin; MacDonald, Nicholas R.; Mao,
Jirong; Marchili, Nicola; Marrone, Daniel P.; Marscher, Alan P.;
Martí-Vidal, Iván; Matsushita, Satoki; Matthews, Lynn D.; Medeiros,
Lia; Menten, Karl M.; Mizuno, Izumi; Mizuno, Yosuke; Moran, James M.;
Moriyama, Kotaro; Moscibrodzka, Monika; Müller, Cornelia; Musoke,
Gibwa; Mejías, Alejandro Mus; Nagai, Hiroshi; Nagar, Neil M.;
Nakamura, Masanori; Narayan, Ramesh; Narayanan, Gopal; Natarajan,
Iniyan; Nathanail, Antonios; Neri, Roberto; Ni, Chunchong; Noutsos,
Aristeidis; Okino, Hiroki; Olivares, Héctor; Ortiz-León, Gisela N.;
Oyama, Tomoaki; Özel, Feryal; Palumbo, Daniel C. M.; Patel, Nimesh;
Pen, Ue-Li; Pesce, Dominic W.; Piétu, Vincent; Plambeck, Richard;
Popstefanija, Aleksandar; Porth, Oliver; Pötzl, Felix M.; Prather,
Ben; Preciado-López, Jorge A.; Psaltis, Dimitrios; Pu, Hung-Yi;
Rao, Ramprasad; Rawlings, Mark G.; Raymond, Alexander W.; Rezzolla,
Luciano; Ricarte, Angelo; Ripperda, Bart; Roelofs, Freek; Rogers,
Alan; Ros, Eduardo; Rose, Mel; Roshanineshat, Arash; Rottmann, Helge;
Roy, Alan L.; Ruszczyk, Chet; Rygl, Kazi L. J.; Sánchez, Salvador;
Sánchez-Arguelles, David; Savolainen, Tuomas; Schloerb, F. Peter;
Schuster, Karl-Friedrich; Shao, Lijing; Shen, Zhiqiang; Small, Des;
Sohn, Bong Won; Soohoo, Jason; Sun, He; Tazaki, Fumie; Tetarenko,
Alexandra J.; Tiede, Paul; Tilanus, Remo P. J.; Titus, Michael; Toma,
Kenji; Torne, Pablo; Trent, Tyler; Traianou, Efthalia; Trippe, Sascha;
van Bemmel, Ilse; van Langevelde, Huib Jan; van Rossum, Daniel R.;
Wagner, Jan; Ward-Thompson, Derek; Wardle, John; Weintroub, Jonathan;
Wex, Norbert; Wharton, Robert; Wielgus, Maciek; Wong, George N.;
Wu, Qingwen; Yoon, Doosoo; Young, André; Young, Ken; Younsi, Ziri;
Yuan, Feng; Yuan, Ye-Fei; Zensus, J. Anton; Zhao, Guang-Yao; Zhao,
Shan-Shan; Fermi Large Area Telescope Collaboration; Principe, G.;
Giroletti, M.; D'Ammando, F.; Orienti, M.; H. E. S. S. Collaboration;
Abdalla, H.; Adam, R.; Aharonian, F.; Benkhali, F. Ait; Angüner,
E. O.; Arcaro, C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes,
M.; Baghmanyan, V.; Barbosa Martins, V.; Barnacka, A.; Barnard,
M.; Becherini, Y.; Berge, D.; Bernlöhr, K.; Bi, B.; Böttcher, M.;
Boisson, C.; Bolmont, J.; de Lavergne, M. De Bony; Breuhaus, M.; Brun,
F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.; Bylund, T.; Caroff,
S.; Carosi, A.; Casanova, S.; Chand, T.; Chen, A.; Cotter, G.; Curyło,
M.; Damascene Mbarubucyeye, J.; Davids, I. D.; Davies, J.; Deil, C.;
Devin, J.; Dewilt, P.; Dirson, L.; Djannati-Ataï, A.; Dmytriiev,
A.; Donath, A.; Doroshenko, V.; Duffy, C.; Dyks, J.; Egberts, K.;
Eichhorn, F.; Einecke, S.; Emery, G.; Ernenwein, J. -P.; Feijen, K.;
Fegan, S.; Fiasson, A.; de Clairfontaine, G. Fichet; Fontaine, G.;
Funk, S.; Füßling, M.; Gabici, S.; Gallant, Y. A.; Giavitto, G.;
Giunti, L.; Glawion, D.; Glicenstein, J. F.; Gottschall, D.; Grondin,
M. -H.; Hahn, J.; Haupt, M.; Hermann, G.; Hinton, J. A.; Hofmann,
W.; Hoischen, C.; Holch, T. L.; Holler, M.; Hörbe, M.; Horns, D.;
Huber, D.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.; Jardin-Blicq,
A.; Joshi, V.; Jung-Richardt, I.; Kasai, E.; Kastendieck, M. A.;
Katarzyński, K.; Katz, U.; Khangulyan, D.; Khélifi, B.; Klepser,
S.; Kluźniak, W.; Komin, Nu.; Konno, R.; Kosack, K.; Kostunin, D.;
Kreter, M.; Lamanna, G.; Lemière, A.; Lemoine-Goumard, M.; Lenain,
J. -P.; Levy, C.; Lohse, T.; Lypova, I.; Mackey, J.; Majumdar,
J.; Malyshev, D.; Malyshev, D.; Marandon, V.; Marchegiani, P.;
Marcowith, A.; Mares, A.; Martí-Devesa, G.; Marx, R.; Maurin, G.;
Meintjes, P. J.; Meyer, M.; Moderski, R.; Mohamed, M.; Mohrmann,
L.; Montanari, A.; Moore, C.; Morris, P.; Moulin, E.; Muller, J.;
Murach, T.; Nakashima, K.; Nayerhoda, A.; de Naurois, M.; Ndiyavala,
H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; O'Brien, P.; Odaka,
H.; Ohm, S.; Olivera-Nieto, L.; de Ona Wilhelmi, E.; Ostrowski, M.;
Panter, M.; Panny, S.; Parsons, R. D.; Peron, G.; Peyaud, B.; Piel, Q.;
Pita, S.; Poireau, V.; Noel, A. Priyana; Prokhorov, D. A.; Prokoph, H.;
Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Rauth, R.; Reichherzer, P.;
Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Rieger, F.; Rinchiuso,
L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.; Sahakian,
V.; Sailer, S.; Sanchez, D. A.; Santangelo, A.; Sasaki, M.; Scalici,
M.; Schutte, H. M.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.;
Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shiningayamwe, K.; Simoni,
R.; Sinha, A.; Sol, H.; Specovius, A.; Spencer, S.; Spir-Jacob, M.;
Stawarz, Ł.; Sun, L.; Steenkamp, R.; Stegmann, C.; Steinmassl, S.;
Steppa, C.; Takahashi, T.; Tavernier, T.; Taylor, A. M.; Terrier, R.;
Tiziani, D.; Tluczykont, M.; Tomankova, L.; Trichard, C.; Tsirou,
M.; Tuffs, R.; Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.;
van Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter,
C.; Vincent, P.; Vink, J.; Völk, H. J.; Vuillaume, T.; Wadiasingh,
Z.; Wagner, S. J.; Watson, J.; Werner, F.; White, R.; Wierzcholska,
A.; Wong, Yu Wun; Yusafzai, A.; Zacharias, M.; Zanin, R.; Zargaryan,
D.; Zdziarski, A. A.; Zech, A.; Zhu, S. J.; Zorn, J.; Zouari, S.;
Żywucka, N.; MAGIC Collaboration; Acciari, V. A.; Ansoldi, S.;
Antonelli, L. A.; Engels, A. Arbet; Artero, M.; Asano, K.; Baack, D.;
Babić, A.; Baquero, A.; de Almeida, U. Barres; Barrio, J. A.; Becerra
González, J.; Bednarek, W.; Bellizzi, L.; Bernardini, E.; Bernardos,
M.; Berti, A.; Besenrieder, J.; Bhattacharyya, W.; Bigongiari, C.;
Biland, A.; Blanch, O.; Bonnoli, G.; Bošnjak, Ž.; Busetto, G.;
Carosi, R.; Ceribella, G.; Cerruti, M.; Chai, Y.; Chilingarian, A.;
Cikota, S.; Colak, S. M.; Colombo, E.; Contreras, J. L.; Cortina,
J.; Covino, S.; D'Amico, G.; D'Elia, V.; da Vela, P.; Dazzi, F.; de
Angelis, A.; de Lotto, B.; Delfino, M.; Delgado, J.; Delgado Mendez,
C.; Depaoli, D.; di Pierro, F.; di Venere, L.; Do Souto Espiñeira,
E.; Dominis Prester, D.; Donini, A.; Dorner, D.; Doro, M.; Elsaesser,
D.; Ramazani, V. Fallah; Fattorini, A.; Ferrara, G.; Fonseca, M. V.;
Font, L.; Fruck, C.; Fukami, S.; García López, R. J.; Garczarczyk,
M.; Gasparyan, S.; Gaug, M.; Giglietto, N.; Giordano, F.; Gliwny,
P.; Godinović, N.; Green, J. G.; Green, D.; Hadasch, D.; Hahn, A.;
Heckmann, L.; Herrera, J.; Hoang, J.; Hrupec, D.; Hütten, M.; Inada,
T.; Inoue, S.; Ishio, K.; Iwamura, Y.; Jiménez, I.; Jormanainen, J.;
Jouvin, L.; Kajiwara, Y.; Karjalainen, M.; Kerszberg, D.; Kobayashi,
Y.; Kubo, H.; Kushida, J.; Lamastra, A.; Lelas, D.; Leone, F.;
Lindfors, E.; Lombardi, S.; Longo, F.; López-Coto, R.; López-Moya,
M.; López-Oramas, A.; Loporchio, S.; Machado de Oliveira Fraga, B.;
Maggio, C.; Majumdar, P.; Makariev, M.; Mallamaci, M.; Maneva, G.;
Manganaro, M.; Mannheim, K.; Maraschi, L.; Mariotti, M.; Martínez,
M.; Mazin, D.; Menchiari, S.; Mender, S.; Mićanović, S.; Miceli,
D.; Miener, T.; Minev, M.; Miranda, J. M.; Mirzoyan, R.; Molina, E.;
Moralejo, A.; Morcuende, D.; Moreno, V.; Moretti, E.; Neustroev, V.;
Nigro, C.; Nilsson, K.; Nishijima, K.; Noda, K.; Nozaki, S.; Ohtani,
Y.; Oka, T.; Otero-Santos, J.; Paiano, S.; Palatiello, M.; Paneque,
D.; Paoletti, R.; Paredes, J. M.; Pavletić, L.; Peñil, P.; Perennes,
C.; Persic, M.; Moroni, P. G. Prada; Prandini, E.; Priyadarshi, C.;
Puljak, I.; Rhode, W.; Ribó, M.; Rico, J.; Righi, C.; Rugliancich,
A.; Saha, L.; Sahakyan, N.; Saito, T.; Sakurai, S.; Satalecka, K.;
Saturni, F. G.; Schleicher, B.; Schmidt, K.; Schweizer, T.; Sitarek,
J.; Šnidarić, I.; Sobczynska, D.; Spolon, A.; Stamerra, A.; Strom,
D.; Strzys, M.; Suda, Y.; Surić, T.; Takahashi, M.; Tavecchio, F.;
Temnikov, P.; Terzić, T.; Teshima, M.; Tosti, L.; Truzzi, S.; Tutone,
A.; Ubach, S.; van Scherpenberg, J.; Vanzo, G.; Vazquez Acosta, M.;
Ventura, S.; Verguilov, V.; Vigorito, C. F.; Vitale, V.; Vovk, I.;
Will, M.; Wunderlich, C.; Zarić, D.; VERITAS Collaboration; Adams,
C. B.; Benbow, W.; Brill, A.; Capasso, M.; Christiansen, J. L.;
Chromey, A. J.; Daniel, M. K.; Errando, M.; Farrell, K. A.; Feng, Q.;
Finley, J. P.; Fortson, L.; Furniss, A.; Gent, A.; Giuri, C.; Hassan,
T.; Hervet, O.; Holder, J.; Hughes, G.; Humensky, T. B.; Jin, W.;
Kaaret, P.; Kertzman, M.; Kieda, D.; Kumar, S.; Lang, M. J.; Lundy,
M.; Maier, G.; Moriarty, P.; Mukherjee, R.; Nieto, D.; Nievas-Rosillo,
M.; O'Brien, S.; Ong, R. A.; Otte, A. N.; Patel, S.; Pfrang, K.; Pohl,
M.; Prado, R. R.; Pueschel, E.; Quinn, J.; Ragan, K.; Reynolds, P. T.;
Ribeiro, D.; Richards, G. T.; Roache, E.; Rulten, C.; Ryan, J. L.;
Santander, M.; Sembroski, G. H.; Shang, R.; Weinstein, A.; Williams,
D. A.; Williamson, T. J.; Eavn Collaboration; Hirota, Tomoya; Cui,
Lang; Niinuma, Kotaro; Ro, Hyunwook; Sakai, Nobuyuki; Sawada-Satoh,
Satoko; Wajima, Kiyoaki; Wang, Na; Liu, Xiang; Yonekura, Yoshinori
2021ApJ...911L..11E Altcode: 2021arXiv210406855A
In 2017, the Event Horizon Telescope (EHT) Collaboration succeeded in
capturing the first direct image of the center of the M87 galaxy. The
asymmetric ring morphology and size are consistent with theoretical
expectations for a weakly accreting supermassive black hole of mass
∼6.5 × 10<SUP>9</SUP>M<SUB>⊙</SUB>. The EHTC also partnered
with several international facilities in space and on the ground, to
arrange an extensive, quasi-simultaneous multi-wavelength campaign. This
Letter presents the results and analysis of this campaign, as well as
the multi-wavelength data as a legacy data repository. We captured M87
in a historically low state, and the core flux dominates over HST-1 at
high energies, making it possible to combine core flux constraints with
the more spatially precise very long baseline interferometry data. We
present the most complete simultaneous multi-wavelength spectrum of
the active nucleus to date, and discuss the complexity and caveats
of combining data from different spatial scales into one broadband
spectrum. We apply two heuristic, isotropic leptonic single-zone models
to provide insight into the basic source properties, but conclude
that a structured jet is necessary to explain M87's spectrum. We can
exclude that the simultaneous γ-ray emission is produced via inverse
Compton emission in the same region producing the EHT mm-band emission,
and further conclude that the γ-rays can only be produced in the
inner jets (inward of HST-1) if there are strongly particle-dominated
regions. Direct synchrotron emission from accelerated protons and
secondaries cannot yet be excluded.
---------------------------------------------------------
Title: H.E.S.S. and MAGIC observations of a sudden cessation of a
very-high-energy γ-ray flare in PKS 1510−089 in May 2016
Authors: H. E. S. S. Collaboration; Abdalla, H.; Adam, R.; Aharonian,
F.; Ait Benkhali, F.; Angüner, E. O.; Arcaro, C.; Armand, C.;
Armstrong, T.; Ashkar, H.; Backes, M.; Baghmanyan, V.; Barbosa Martins,
V.; Barnacka, A.; Barnard, M.; Becherini, Y.; Berge, D.; Bernlöhr,
K.; Bi, B.; Böttcher, M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.; de
Bony de Lavergne, M.; Bregeon, J.; Breuhaus, M.; Brun, F.; Brun, P.;
Bryan, M.; Büchele, M.; Bulik, T.; Bylund, T.; Caroff, S.; Carosi, A.;
Casanova, S.; Chand, T.; Chandra, S.; Chen, A.; Cotter, G.; Curyło,
M.; Damascene Mbarubucyeye, J.; Davids, I. D.; Davies, J.; Deil, C.;
Devin, J.; Dewilt, P.; Dirson, L.; Djannati-Ataï, A.; Dmytriiev,
A.; Donath, A.; Doroshenko, V.; Dyks, J.; Egberts, K.; Eichhorn, F.;
Einecke, S.; Emery, G.; Ernenwein, J. -P.; Feijen, K.; Fegan, S.;
Fiasson, A.; Fichet de Clairfontaine, G.; Filipovic, M.; Fontaine,
G.; Funk, S.; Füßling, M.; Gabici, S.; Gallant, Y. A.; Giavitto, G.;
Giunti, L.; Glawion, D.; Glicenstein, J. F.; Gottschall, D.; Grondin,
M. -H.; Hahn, J.; Haupt, M.; Hermann, G.; Hinton, J. A.; Hofmann, W.;
Hoischen, C.; Holch, T. L.; Holler, M.; Hörbe, M.; Horns, D.; Huber,
D.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.; Jardin-Blicq, A.; Joshi,
V.; Jung-Richardt, I.; Kastendieck, M. A.; Katarzyński, K.; Katz,
U.; Khangulyan, D.; Khélifi, B.; Klepser, S.; Kluźniak, W.; Komin,
Nu.; Konno, R.; Kosack, K.; Kostunin, D.; Kreter, M.; Lamanna, G.;
Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Levy, C.; Lohse,
T.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev, D.; Malyshev, D.;
Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares, A.; Martí-Devesa,
G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Meyer, M.; Mitchell,
A. M. W.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Montanari, A.;
Moore, C.; Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima,
K.; Nayerhoda, A.; de Naurois, M.; Ndiyavala, H.; Niederwanger, F.;
Niemiec, J.; Oakes, L.; O'Brien, P.; Odaka, H.; Ohm, S.; Olivera-Nieto,
L.; de Ona Wilhelmi, E.; Ostrowski, M.; Panter, M.; Panny, S.; Parsons,
R. D.; Peron, G.; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V.; Priyana
Noel, A.; Prokhorov, D. A.; Prokoph, H.; Pühlhofer, G.; Punch, M.;
Quirrenbach, A.; Raab, S.; Rauth, R.; Reichherzer, P.; Reimer, A.;
Reimer, O.; Remy, Q.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli,
C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.; Sahakian, V.; Sailer, S.;
Sanchez, D. A.; Santangelo, A.; Sasaki, M.; Scalici, M.; Schüssler,
F.; Schutte, H. M.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.;
Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shiningayamwe, K.; Simoni,
R.; Sinha, A.; Sol, H.; Specovius, A.; Spencer, S.; Spir-Jacob, M.;
Stawarz, Ł.; Sun, L.; Steenkamp, R.; Stegmann, C.; Steinmassl, S.;
Steppa, C.; Takahashi, T.; Tavernier, T.; Taylor, A. M.; Terrier, R.;
Tiziani, D.; Tluczykont, M.; Tomankova, L.; Trichard, C.; Tsirou,
M.; Tuffs, R.; Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.;
van Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter,
C.; Vincent, P.; Vink, J.; Völk, H. J.; Vuillaume, T.; Wadiasingh,
Z.; Wagner, S. J.; Watson, J.; Werner, F.; White, R.; Wierzcholska,
A.; Wong, Yu. W.; Yusafzai, A.; Zacharias, M.; Zanin, R.; Zargaryan,
D.; Zdziarski, A. A.; Zech, A.; Zhu, S. J.; Zorn, J.; Zouari, S.;
Żywucka, N.; MAGIC Collaboration; Acciari, V. A.; Ansoldi, S.;
Antonelli, L. A.; Arbet Engels, A.; Asano, K.; Baack, D.; Babić, A.;
Baquero, A.; Barres de Almeida, U.; Barrio, J. A.; Becerra González,
J.; Bednarek, W.; Bellizzi, L.; Bernardini, E.; Berti, A.; Besenrieder,
J.; Bhattacharyya, W.; Bigongiari, C.; Biland, A.; Blanch, O.; Bonnoli,
G.; Bošnjak, Ž.; Busetto, G.; Carosi, R.; Ceribella, G.; Cerruti,
M.; Chai, Y.; Chilingarian, A.; Cikota, S.; Colak, S. M.; Colin, U.;
Colombo, E.; Contreras, J. L.; Cortina, J.; Covino, S.; D'Amico, G.;
D'Elia, V.; da Vela, P.; Dazzi, F.; de Angelis, A.; de Lotto, B.;
Delfino, M.; Delgado, J.; Depaoli, D.; di Pierro, F.; di Venere, L.;
Do Souto Espiñeira, E.; Dominis Prester, D.; Donini, A.; Dorner, D.;
Doro, M.; Elsaesser, D.; Fallah Ramazani, V.; Fattorini, A.; Ferrara,
G.; Foffano, L.; Fonseca, M. V.; Font, L.; Fruck, C.; Fukami, S.;
García López, R. J.; Garczarczyk, M.; Gasparyan, S.; Gaug, M.;
Giglietto, N.; Giordano, F.; Gliwny, P.; Godinović, N.; Green, D.;
Hadasch, D.; Hahn, A.; Heckmann, L.; Herrera, J.; Hoang, J.; Hrupec,
D.; Hütten, M.; Inada, T.; Inoue, S.; Ishio, K.; Iwamura, Y.; Jouvin,
L.; Kajiwara, Y.; Karjalainen, M.; Kerszberg, D.; Kobayashi, Y.; Kubo,
H.; Kushida, J.; Lamastra, A.; Lelas, D.; Leone, F.; Lindfors, E.;
Lombardi, S.; Longo, F.; López, M.; López-Coto, R.; López-Oramas,
A.; Loporchio, S.; Machado de Oliveira Fraga, B.; Maggio, C.; Majumdar,
P.; Makariev, M.; Mallamaci, M.; Maneva, G.; Manganaro, M.; Mannheim,
K.; Maraschi, L.; Mariotti, M.; Martínez, M.; Mazin, D.; Mender, S.;
Mićanović, S.; Miceli, D.; Miener, T.; Minev, M.; Miranda, J. M.;
Mirzoyan, R.; Molina, E.; Moralejo, A.; Morcuende, D.; Moreno, V.;
Moretti, E.; Munar-Adrover, P.; Neustroev, V.; Nigro, C.; Nilsson,
K.; Ninci, D.; Nishijima, K.; Noda, K.; Nozaki, S.; Ohtani, Y.;
Oka, T.; Otero-Santos, J.; Palatiello, M.; Paneque, D.; Paoletti,
R.; Paredes, J. M.; Pavletić, L.; Peñil, P.; Perennes, C.; Persic,
M.; Prada Moroni, P. G.; Prandini, E.; Priyadarshi, C.; Puljak, I.;
Rhode, W.; Ribó, M.; Rico, J.; Righi, C.; Rugliancich, A.; Saha, L.;
Sahakyan, N.; Saito, T.; Sakurai, S.; Satalecka, K.; Schleicher, B.;
Schmidt, K.; Schweizer, T.; Sitarek, J.; Šnidarić, I.; Sobczynska,
D.; Spolon, A.; Stamerra, A.; Strom, D.; Strzys, M.; Suda, Y.; Surić,
T.; Takahashi, M.; Tavecchio, F.; Temnikov, P.; Terzić, T.; Teshima,
M.; Torres-Albà, N.; Tosti, L.; Truzzi, S.; van Scherpenberg, J.;
Vanzo, G.; Vazquez Acosta, M.; Ventura, S.; Verguilov, V.; Vigorito,
C. F.; Vitale, V.; Vovk, I.; Will, M.; Zarić, D.; Jorstad, S. G.;
Marscher, A. P.; Boccardi, B.; Casadio, C.; Hodgson, J.; Kim, J. -Y.;
Krichbaum, T. P.; Lähteenmäki, A.; Tornikoski, M.; Traianou, E.;
Weaver, Z. R.
2021A&A...648A..23H Altcode: 2020arXiv201210254H
The flat spectrum radio quasar (FSRQ) PKS 1510−089 is known for its
complex multiwavelength behaviour and it is one of only a few FSRQs
detected in very-high-energy (VHE, E > 100 GeV) γ rays. The VHE
γ-ray observations with H.E.S.S. and MAGIC in late May and early
June 2016 resulted in the detection of an unprecedented flare, which
revealed, for the first time, VHE γ-ray intranight variability for
this source. While a common variability timescale of 1.5 h has been
found, there is a significant deviation near the end of the flare, with
a timescale of ∼20 min marking the cessation of the event. The peak
flux is nearly two orders of magnitude above the low-level emission. For
the first time, a curvature was detected in the VHE γ-ray spectrum
of PKS 1510-089, which can be fully explained by the absorption
on the part of the extragalactic background light. Optical R-band
observations with ATOM revealed a counterpart of the γ-ray flare,
even though the detailed flux evolution differs from the VHE γ-ray
light curve. Interestingly, a steep flux decrease was observed at the
same time as the cessation of the VHE γ-ray flare. In the high-energy
(HE, E > 100 MeV) γ-ray band, only a moderate flux increase was
observed with Fermi-LAT, while the HE γ-ray spectrum significantly
hardens up to a photon index of 1.6. A search for broad-line region
(BLR) absorption features in the γ-ray spectrum indicates that the
emission region is located outside of the BLR. Radio very-long-baseline
interferometry observations reveal a fast-moving knot interacting with
a standing jet feature around the time of the flare. As the standing
feature is located ∼50 pc from the black hole, the emission region
of the flare may have been located at a significant distance from the
black hole. If this is indeed a true correlation, the VHE γ rays must
have been produced far down in the jet, where turbulent plasma crosses
a standing shock.
---------------------------------------------------------
Title: A SmallSat to Study the Structure and Evolution of ExoJupiter
Atmospheres (SEEJ)
Authors: Wolk, S.; Moore, C.; Hong, J.; Romaine, S.; Moorhead, A.;
Kaltenegger, L.; Wargelin, B.; Kashyap, V.
2021BAAS...53c1214W Altcode:
The most important effects on an exoplanet atmosphere are driven by
high-energy photons and particles from the host star, which heat and
ionize the planetary atmosphere, potentially leading to its loss. The
rarest, largest flares are disproportionately important. SEEJ will
study the Structure and Evolution of ExoJupiter atmospheres with long
observations, with cumulative exposures well beyond those conducted by
any other mission. SEEJ will measure how often high energy flares of
a given size occur, and establish, for the first time the statistics
of these crucial events on exoplanet hosts. Observing transits SEEJ
will measure the thermospheric scale height, and so the inflation or
damage to the exoJupiter atmosphere. SEEJ will provide the data for
theory to tie the rare flares and their effects together via improved
models of exoplanet thermospheres.The X-rays emitted by an exoplanet
host star is critical to the atmosphere of the planet. Specifically,
X-rays can induce both life-enabling and life-threatening photochemistry
in planetary atmospheres. Similarly, observed X-ray flares may be
harbingers of coronal mass ejections which can aid the development of
life by removing primary, hydrogen-dominated atmospheres or threaten
its existence by depleting secondary atmospheres and specific
critical species such as ozone. An understanding of the behavior
of stellar coronae at all phases of stellar/planetary evolution is
fundamental to our ability to gauge the cumulative impact of stellar
X-rays on planetary atmospheres. <P />The First Objective of SEEJ is
to characterize the X-ray emission for a diversity of planet hosting
stars through long term monitoring, and use this as input to exo-planet
atmospheric models to determine effect on planetary atmospheres,
and possible feedback between the planet and star. <P />The Second
Objective of SEEJ is to detect and measure planetary exospheric
structure through the shape and extent of the upper atmosphere for a
variety of exoplanets. <P />SEEJ will provide detailed X-ray transit
light curve profiles of suitable targets accumulating them by observing
multiple exoplanet transits. SEEJ will monitor roughly 40 transits of
as many as 7 X-ray bright exoplanet hosts in a single year.
---------------------------------------------------------
Title: A Search for Blue Lurkers in the Open Cluster NGC 6791 Applying
an Image-Subtraction Reduction Pipeline to the Kepler Superstamp
Authors: McClure, R. L.; Soares, M.; Mathieu, R.; Moore, C.
2021AAS...23714006M Altcode:
The original Kepler mission observations included a super-stamp of
the open cluster NGC 6791, a cluster of particular interest as one
of the oldest and most metal rich open clusters in the Milky Way. We
present initial results of a forthcoming catalog of 100 ppm or better
photometric-precision light-curves of stars in the NGC 6791 super-stamp,
along with the surrounding field Kepler Objects of Interest postage
stamps. We apply an image subtraction reduction pipeline useful for
crowded fields of the core of open clusters, as used for K2 super-stamps
by Soares-Furtado et al. 2017. This work will provide light curves and
analyses of all identified variable stars in the cluster. In particular,
we intend to use these data to search for only the second population
of blue lurkers. We also anticipate unforeseen discoveries in this
benchmark open cluster due to the precision of the light curves and
quantity of resolved objects. We have underway a WIYN Open Cluster
Study radial-velocity survey of the cluster to support analyses of
these discovered objects to V = 18. We intend to apply this pipeline
for similar analyses on the other three open cluster super-stamps
in the Kepler field. The authors acknowledge funding support from
NSF AST-1714506, the Office of the Vice Chancellor for Research
and Graduate Education at the University of Wisconsin-Madison, the
J.D. Fluno Family Distinguished Graduate Fellowship, and the Wisconsin
Alumni Research Foundation.
---------------------------------------------------------
Title: An extreme particle accelerator in the Galactic plane:
HESS J1826-130
Authors: H. E. S. S. Collaboration; Abdalla, H.; Adam, R.; Aharonian,
F.; Ait Benkhali, F.; Angüner, E. O.; Arcaro, C.; Armand, C.;
Armstrong, T.; Ashkar, H.; Backes, M.; Baghmanyan, V.; Barbosa Martins,
V.; Barnacka, A.; Barnard, M.; Becherini, Y.; Berge, D.; Bernlöhr,
K.; Bi, B.; Böttcher, M.; Boisson, C.; Bolmont, J.; de Bony de
Lavergne, M.; Bordas, P.; Breuhaus, M.; Brun, F.; Brun, P.; Bryan,
M.; Büchele, M.; Bulik, T.; Bylund, T.; Caroff, S.; Carosi, A.;
Casanova, S.; Chand, T.; Chandra, S.; Chen, A.; Cotter, G.; Curyło,
M.; Damascene Mbarubucyeye, J.; Davids, I. D.; Davies, J.; Deil, C.;
Devin, J.; deWilt, P.; Dirson, L.; Djannati-Ataï, A.; Dmytriiev,
A.; Donath, A.; Doroshenko, V.; Duffy, C.; Dyks, J.; Egberts, K.;
Eichhorn, F.; Einecke, S.; Emery, G.; Ernenwein, J. -P.; Feijen, K.;
Fegan, S.; Fiasson, A.; Fichet de Clairfontaine, G.; Fontaine, G.;
Funk, S.; Füßling, M.; Gabici, S.; Gallant, Y. A.; Giavitto, G.;
Giunti, L.; Glawion, D.; Glicenstein, J. F.; Gottschall, D.; Grondin,
M. -H.; Hahn, J.; Haupt, M.; Hermann, G.; Hinton, J. A.; Hofmann,
W.; Hoischen, C.; Holch, T. L.; Holler, M.; Hörbe, M.; Horns, D.;
Huber, D.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.; Jardin-Blicq,
A.; Joshi, V.; Jung-Richardt, I.; Kasai, E.; Kastendieck, M. A.;
Katarzyński, K.; Katz, U.; Khangulyan, D.; Khélifi, B.; Klepser,
S.; Kluźniak, W.; Komin, Nu.; Konno, R.; Kosack, K.; Kostunin, D.;
Kreter, M.; Lamanna, G.; Lemière, A.; Lemoine-Goumard, M.; Lenain,
J. -P.; Levy, C.; Lohse, T.; Lypova, I.; Mackey, J.; Majumdar, J.;
Malyshev, D.; Malyshev, D.; Marandon, V.; Marchegiani, ¶.; Marcowith,
A.; Mares, A.; Martí-Devesa, G.; Marx, R.; Maurin, G.; Meintjes,
P. J.; Meyer, M.; Mitchell, A.; Moderski, R.; Mohamed, M.; Mohrmann,
L.; Montanari, A.; Moore, C.; Morris, P.; Moulin, E.; Muller, J.;
Murach, T.; Nakashima, K.; Nayerhoda, A.; de Naurois, M.; Ndiyavala,
H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; O'Brien, P.; Odaka,
H.; Ohm, S.; Olivera-Nieto, L.; de Ona Wilhelmi, E.; Ostrowski, M.;
Oya, I.; Panter, M.; Panny, S.; Parsons, R. D.; Peron, G.; Peyaud,
B.; Piel, Q.; Pita, S.; Poireau, V.; Priyana Noel, A.; Prokhorov,
D. A.; Prokoph, H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.;
Raab, S.; Rauth, R.; Reichherzer, P.; Reimer, A.; Reimer, O.; Remy,
Q.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli, C.; Rowell, G.;
Rudak, B.; Ruiz-Velasco, E.; Sahakian, V.; Sailer, S.; Sanchez, D. A.;
Santangelo, A.; Sasaki, M.; Scalici, M.; Schüssler, F.; Schutte,
H. M.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.; Senniappan, M.;
Seyffert, A. S.; Shafi, N.; Shiningayamwe, K.; Simoni, R.; Sinha, A.;
Sol, H.; Specovius, A.; Spencer, S.; Spir-Jacob, M.; Stawarz, Ł.; Sun,
L.; Steenkamp, R.; Stegmann, C.; Steinmassl, S.; Steppa, C.; Takahashi,
T.; Tavernier, T.; Taylor, A. M.; Terrier, R.; Tiziani, D.; Tluczykont,
M.; Tomankova, L.; Trichard, C.; Tsirou, M.; Tuffs, R.; Uchiyama, Y.;
van der Walt, D. J.; van Eldik, C.; van Rensburg, C.; van Soelen,
B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.;
Völk, H. J.; Vuillaume, T.; Wadiasingh, Z.; Wagner, S. J.; Watson,
J.; Werner, F.; White, R.; Wierzcholska, A.; Wong, Yu Wun; Yusafzai,
A.; Zacharias, M.; Zanin, R.; Zargaryan, D.; Zdziarski, A. A.; Zech,
A.; Zhu, S. J.; Ziegler, A.; Zorn, J.; Zouari, S.; Żywucka, N.
2020A&A...644A.112H Altcode: 2020arXiv201013101H
The unidentified very-high-energy (VHE; E > 0.1 TeV) γ-ray source,
HESS J1826-130, was discovered with the High Energy Stereoscopic
System (HESS) in the Galactic plane. The analysis of 215 h of HESS
data has revealed a steady γ-ray flux from HESS J1826-130, which
appears extended with a half-width of 0.21° ± 0.02<SUB>stat</SUB>°
± 0.05<SUB>sys</SUB>°. The source spectrum is best fit with
either a power-law function with a spectral index Γ = 1.78 ±
0.10<SUB>stat</SUB> ± 0.20<SUB>sys</SUB> and an exponential cut-off
at 15.2<SUB>-3.2</SUB><SUP>+5.5</SUP> TeV, or a broken power-law with
Γ<SUB>1</SUB> = 1.96 ± 0.06<SUB>stat</SUB> ± 0.20<SUB>sys</SUB>,
Γ<SUB>2</SUB> = 3.59 ± 0.69<SUB>stat</SUB> ± 0.20<SUB>sys</SUB>
for energies below and above E<SUB>br</SUB> = 11.2 ± 2.7 TeV,
respectively. The VHE flux from HESS J1826-130 is contaminated by
the extended emission of the bright, nearby pulsar wind nebula, HESS
J1825-137, particularly at the low end of the energy spectrum. Leptonic
scenarios for the origin of HESS J1826-130 VHE emission related to PSR
J1826-1256 are confronted by our spectral and morphological analysis. In
a hadronic framework, taking into account the properties of dense gas
regions surrounding HESS J1826-130, the source spectrum would imply
an astrophysical object capable of accelerating the parent particle
population up to ≳200 TeV. Our results are also discussed in a
multiwavelength context, accounting for both the presence of nearby
supernova remnants, molecular clouds, and counterparts detected in
radio, X-rays, and TeV energies.
---------------------------------------------------------
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
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 C<SUB>3</SUB>F<SUB>8</SUB> 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 σ<SUB>SD</SUB>≲3 ×10<SUP>-39</SUP>cm<SUP>2</SUP> (6
×10<SUP>-38</SUP>cm<SUP>2</SUP> ) at ≳90 % C.L. for a DM particle
of mass 1 TeV annihilating into τ<SUP>+</SUP>τ<SUP>-</SUP> (b b ¯ )
with a local density of ρ<SUB>DM</SUB>=0.3 GeV<SUP>/cm 3</SUP> . The
constraints scale inversely with ρ<SUB>DM</SUB> and are independent
of the DM velocity distribution.
---------------------------------------------------------
Title: Search for dark matter signals towards a selection of recently
detected DES dwarf galaxy satellites of the Milky Way with H.E.S.S.
Authors: Abdallah, H.; Adam, R.; Aharonian, F.; Ait Benkhali, F.;
Angüner, E. O.; Arakawa, M.; Arcaro, C.; Armand, C.; Armstrong, T.;
Ashkar, H.; Backes, M.; Baghmanyan, V.; Barbosa Martins, V.; Barnacka,
A.; Barnard, M.; Becherini, Y.; Berge, D.; Bernlöhr, K.; Böttcher,
M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.; Breuhaus, M.; Bregeon, J.;
Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.; Bylund, T.;
Caroff, S.; Carosi, A.; Casanova, S.; Chand, T.; Chandra, S.; Chen,
A.; Cotter, G.; Curyło, M.; Davids, I. D.; Davies, J.; Deil, C.;
Devin, J.; deWilt, P.; Dirson, L.; Djannati-Ataï, A.; Dmytriiev,
A.; Donath, A.; Doroshenko, V.; Dyks, J.; Egberts, K.; Eichhorn,
F.; Emery, G.; Ernenwein, J. -P.; Eschbach, S.; Feijen, K.; Fegan,
S.; Fiasson, A.; Fontaine, G.; Funk, S.; Füßling, M.; Gabici, S.;
Gallant, Y. A.; Giavitto, G.; Giunti, L.; Glawion, D.; Glicenstein,
J. F.; Gottschall, D.; Grondin, M. -H.; Hahn, J.; Haupt, M.; Hermann,
G.; Hinton, J. A.; Hofmann, W.; Hoischen, C.; Holch, T. L.; Holler, M.;
Hörbe, M.; Horns, D.; Huber, D.; Iwasaki, H.; Jamrozy, M.; Jankowsky,
D.; Jankowsky, F.; Jardin-Blicq, A.; Joshi, V.; Jung-Richardt, I.;
Kastendieck, M. A.; Katarzyński, K.; Katsuragawa, M.; Katz, U.;
Khangulyan, D.; Khélifi, B.; Klepser, S.; Kluźniak, W.; Komin,
Nu.; Konno, R.; Kosack, K.; Kostunin, D.; Kreter, M.; Lamanna, G.;
Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leser, E.; Levy,
C.; Lohse, T.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev, D.;
Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares, A.;
Martı-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Moderski,
R.; Mohamed, M.; Mohrmann, L.; Moore, C.; Morris, P.; Moulin, E.;
Muller, J.; Murach, T.; Nakashima, K.; Nakashima, S.; de Naurois, M.;
Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; O'Brien, P.;
Odaka, H.; Ohm, S.; de Ona Wilhelmi, E.; Ostrowski, M.; Panter, M.;
Parsons, R. D.; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V.; Priyana
Noel, A.; Prokhorov, D. A.; Prokoph, H.; Pühlhofer, G.; Punch, M.;
Quirrenbach, A.; Raab, S.; Rauth, R.; Reimer, A.; Reimer, O.; Remy,
Q.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli, C.; Rowell, G.;
Rudak, B.; Ruiz-Velasco, E.; Sahakian, V.; Sailer, S.; Saito, S.;
Sanchez, D. A.; Santangelo, A.; Sasaki, M.; Scalici, M.; Schüssler,
F.; Schutter, H. M.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.;
Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shiningayamwe, K.; Simoni,
R.; Sinha, A.; Sol, H.; Specovius, A.; Spencer, S.; Spir-Jacob, M.;
Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Steppa, C.; Takahashi, T.;
Tavernier, T.; Taylor, A. M.; Terrier, R.; Tiziani, D.; Tluczykont,
M.; Tomankova, L.; Trichard, C.; Tsirou, M.; Tsuji, N.; Tuffs, R.;
Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.; van Rensburg, C.; van
Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Viana, A.; Vincent,
P.; Vink, J.; Völk, H. J.; Vuillaume, T.; Wadiasingh, Z.; Wagner,
S. J.; Watson, J.; Werner, F.; White, R.; Wierzcholska, A.; Yang, R.;
Yoneda, H.; Zacharias, M.; Zanin, R.; Zargaryan, D.; Zdziarski, A. A.;
Zech, A.; Zhu, S.; Zorn, J.; Żywucka, N.; H. E. S. S. Collaboration
2020PhRvD.102f2001A Altcode: 2020arXiv200800688H
Dwarf spheroidal galaxy satellites of the Milky Way are prime targets
for indirect detection of dark matter with gamma rays due to their
proximity, high dark matter content, and absence of nonthermal
emission processes. Recently, the Dark Energy Survey (DES) revealed
the existence of new ultrafaint dwarf spheroidal galaxies in the
southern-hemisphere sky, therefore ideally located for ground-based
observations with the imaging atmospheric Cherenkov telescope array
H.E.S.S. We present a search for very-high-energy (E ≳100 GeV )
gamma-ray emission using H.E.S.S. observations carried out recently
towards Reticulum II, Tucana II, Tucana III, Tucana IV, and Grus II
satellites. No significant very-high-energy gamma-ray excess is found
from the observations on any individual object nor in the combined
analysis of all the datasets. Using the most recent modeling of the
dark matter distribution in the dwarf galaxy halo, we compute for
the first time on DES satellites individual and combined constraints
from Cherenkov telescope observations on the annihilation cross
section of dark matter particles in the form of Weakly Interacting
Massive Particles. The combined 95% C.L. observed upper limits reach
⟨σ v ⟩≃1 ×10<SUP>-23</SUP> cm<SUP>3</SUP> s<SUP>-1</SUP>
in the W<SUP>+</SUP>W<SUP>-</SUP> channel and 4 ×10<SUP>-26</SUP>
cm<SUP>3</SUP> s<SUP>-1</SUP> in the γ γ channels for a dark matter
mass of 1.5 TeV. The H.E.S.S. constraints well complement the results
from Fermi-LAT, HAWC, MAGIC, and VERITAS and are currently the most
stringent in the γ γ channels in the multi-GeV/multi-TeV mass range.
---------------------------------------------------------
Title: Simultaneous observations of the blazar PKS 2155-304 from
ultra-violet to TeV energies
Authors: Abdalla, H.; Adam, R.; Aharonian, F.; Ait Benkhali, F.;
Angüner, E. O.; Arakawa, M.; Arcaro, C.; Armand, C.; Ashkar, H.;
Backes, M.; Barbosa Martins, V.; Barnard, M.; Becherini, Y.; Berge, D.;
Bernlöhr, K.; Blackwell, R.; Böttcher, M.; Boisson, C.; Bolmont, J.;
Bonnefoy, S.; Bregeon, J.; Breuhaus, M.; Brun, F.; Brun, P.; Bryan, M.;
Büchele, M.; Bulik, T.; Bylund, T.; Caroff, S.; Carosi, A.; Casanova,
S.; Cerruti, M.; Chand, T.; Chandra, S.; Chen, A.; Colafrancesco, S.;
Curyło, M.; Davids, I. D.; Deil, C.; Devin, J.; deWilt, P.; Dirson,
L.; Djannati-Ataï, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.;
Dyks, J.; Egberts, K.; Emery, G.; Ernenwein, J. -P.; Eschbach, S.;
Feijen, K.; Fegan, S.; Fiasson, A.; Fontaine, G.; Funk, S.; Füßling,
M.; Gabici, S.; Gallant, Y. A.; Gaté, F.; Giavitto, G.; Giunti, L.;
Glawion, D.; Glicenstein, J. F.; Gottschall, D.; Grondin, M. -H.;
Hahn, J.; Haupt, M.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton,
J. A.; Hofmann, W.; Hoischen, C.; Holch, T. L.; Holler, M.; Horns,
D.; Huber, D.; Iwasaki, H.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.;
Jardin-Blicq, A.; Jung-Richardt, I.; Kastendieck, M. A.; Katarzyński,
K.; Katsuragawa, M.; Katz, U.; Khangulyan, D.; Khélifi, B.; King,
J.; Klepser, S.; Kluźniak, W.; Komin, Nu.; Kosack, K.; Kostunin, D.;
Kreter, M.; Lamanna, G.; Lemière, A.; Lemoine-Goumard, M.; Lenain,
J. -P.; Leser, E.; Levy, C.; Lohse, T.; Lypova, I.; Mackey, J.;
Majumdar, J.; Malyshev, D.; Marandon, V.; Marcowith, A.; Mares, A.;
Mariaud, C.; Martí-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.;
Mitchell, A. M. W.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Moore,
C.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, S.; de Naurois,
M.; Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; O'Brien,
P.; Odaka, H.; Ohm, S.; de Ona Wilhelmi, E.; Ostrowski, M.; Oya, I.;
Panter, M.; Parsons, R. D.; Perennes, C.; Petrucci, P. -O.; Peyaud,
B.; Piel, Q.; Pita, S.; Poireau, V.; Priyana Noel, A.; Prokhorov,
D. A.; Prokoph, H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab,
S.; Rauth, R.; Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Rieger,
F.; Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco,
E.; Sahakian, V.; Sailer, S.; Saito, S.; Sanchez, D. A.; Santangelo,
A.; Sasaki, M.; Schlickeiser, R.; Schüssler, F.; Schulz, A.; Schutte,
H. M.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.; Senniappan, M.;
Seyffert, A. S.; Shafi, N.; Shiningayamwe, K.; Simoni, R.; Sinha, A.;
Sol, H.; Specovius, A.; Spir-Jacob, M.; Stawarz, Ł.; Steenkamp, R.;
Stegmann, C.; Steppa, C.; Takahashi, T.; Tavernier, T.; Taylor, A. M.;
Terrier, R.; Tiziani, D.; Tluczykont, M.; Trichard, C.; Tsirou, M.;
Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.;
van Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter,
C.; Vincent, P.; Vink, J.; Völk, H. J.; Vuillaume, T.; Wadiasingh,
Z.; Wagner, S. J.; White, R.; Wierzcholska, A.; Yang, R.; Yoneda,
H.; Zacharias, M.; Zanin, R.; Zdziarski, A. A.; Zech, A.; Zorn, J.;
Żywucka, N.; Madejski, G. M.; Nalewajko, K.; Madsen, K. K.; Chiang,
J.; Baloković, M.; Paneque, D.; Furniss, A. K.; Hayashida, M.; Urry,
C. M.; Ajello, M.; Harrison, F. A.; Giebels, B.; Stern, D.; Forster,
K.; Giommi, P.; Perri, M.; Puccetti, S.; Zoglauer, A.; Tagliaferri, G.
2020A&A...639A..42A Altcode: 2019arXiv191207273H
Here we report the results of the first ever contemporaneous
multi-wavelength observation campaign on the BL Lac object PKS 2155-304
involving Swift, NuSTAR, Fermi-LAT, and H.E.S.S. The use of these
instruments allows us to cover a broad energy range, which is important
for disentangling the different radiative mechanisms. The source,
observed from June 2013 to October 2013, was found in a low flux state
with respect to previous observations but exhibited highly significant
flux variability in the X-rays. The high-energy end of the synchrotron
spectrum can be traced up to 40 keV without significant contamination
by high-energy emission. A one-zone synchrotron self-Compton model
was used to reproduce the broadband flux of the source for all the
observations presented here but failed for previous observations made
in April 2013. A lepto-hadronic solution was then explored to explain
these earlier observational results.
---------------------------------------------------------
Title: Very high energy γ-ray emission from two blazars of unknown
redshift and upper limits on their distance
Authors: Abdalla, H.; Adam, R.; Aharonian, F.; Ait Benkhali, F.;
Angüner, E. O.; Arakawa, M.; Arcaro, C.; Armand, C.; Armstrong, T.;
Ashkar, H.; Backes, M.; Baghmanyan, V.; Barbosa Martins, V.; Barnacka,
A.; Barnard, M.; Becherini, Y.; Berge, D.; Bernlöhr, K.; Böttcher,
M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bregeon, J.; Breuhaus, M.;
Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.; Bylund, T.;
Caroff, S.; Carosi, A.; Casanova, S.; Chand, T.; Chandra, S.; Chen,
A.; Cotter, G.; Curyło, M.; Davids, I. D.; Davies, J.; Deil, C.;
Devin, J.; deWilt, P.; Dirson, L.; Djannati-Ataï, A.; Dmytriiev,
A.; Donath, A.; Doroshenko, V.; Dyks, J.; Egberts, K.; Eichhorn,
F.; Emery, G.; Ernenwein, J. -P.; Feijen, K.; Fegan, S.; Fiasson,
A.; Fontaine, G.; Funk, S.; Füßling, M.; Gabici, S.; Gallant,
Y. A.; Giavitto, G.; Giunti, L.; Glawion, D.; Glicenstein, J. F.;
Gottschall, D.; Grondin, M. -H.; Hahn, J.; Haupt, M.; Hermann, G.;
Hinton, J. A.; Hofmann, W.; Hoischen, C.; Holch, T. L.; Holler, M.;
Hörbe, M.; Horns, D.; Huber, D.; Iwasaki, H.; Jamrozy, M.; Jankowsky,
D.; Jankowsky, F.; Jardin-Blicq, A.; Joshi, V.; Jung-Richardt, I.;
Kastendieck, M. A.; Katarzyński, K.; Katsuragawa, M.; Katz, U.;
Khangulyan, D.; Khélifi, B.; Klepser, S.; Kluźniak, W.; Komin,
Nu; Konno, R.; Kosack, K.; Kostunin, D.; Kreter, M.; Lamanna, G.;
Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leser, E.; Levy,
C.; Lohse, T.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev, D.;
Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares, A.;
Martí-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Moderski,
R.; Mohamed, M.; Mohrmann, L.; Moore, C.; Morris, P.; Moulin, E.;
Muller, J.; Murach, T.; Nakashima, S.; Nakashima, K.; de Naurois, M.;
Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; O'Brien, P.;
Odaka, H.; Ohm, S.; de Oña Wilhelmi, E.; Ostrowski, M.; Panter, M.;
Parsons, R. D.; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V.; Noel,
A. P.; Prokhorov, D. A.; Prokoph, H.; Pühlhofer, G.; Punch, M.;
Quirrenbach, A.; Raab, S.; Rauth, R.; Reimer, A.; Reimer, O.; Remy,
Q.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli, C.; Rowell, G.;
Rudak, B.; Ruiz-Velasco, E.; Sahakian, V.; Sailer, S.; Saito, S.;
Sanchez, D. A.; Santangelo, A.; Sasaki, M.; Scalici, M.; Schüssler,
F.; Schutte, H. M.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.;
Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shiningayamwe, K.; Simoni,
R.; Sinha, A.; Sol, H.; Specovius, A.; Spencer, S.; Spir-Jacob, M.;
Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Steppa, C.; Takahashi, T.;
Tavernier, T.; Taylor, A. M.; Terrier, R.; Tiziani, D.; Tluczykont,
M.; Tomankova, L.; Trichard, C.; Tsirou, M.; Tsuji, N.; Tuffs, R.;
Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.; van Rensburg, C.;
van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.;
Vink, J.; Völk, H. J.; Vuillaume, T.; Wadiasingh, Z.; Wagner, S. J.;
Watson, J.; Werner, F.; White, R.; Wierzcholska, A.; Yang, R.; Yoneda,
H.; Zacharias, M.; Zanin, R.; Zargaryan, D.; Zdziarski, A. A.; Zech,
A.; Zhu, S. J.; Zorn, J.; Żywucka, N.; Cerruti, M.
2020MNRAS.494.5590A Altcode: 2020arXiv200403306H; 2020MNRAS.tmp.1233H
We report on the detection of very high energy (VHE; E >
100 GeV) γ-ray emission from the BL Lac objects KUV 00311-1938
and PKS 1440-389 with the High Energy Stereoscopic System
(H.E.S.S.). H.E.S.S. observations were accompanied or preceded by
multiwavelength observations with Fermi/LAT, XRT and UVOT onboard the
Swift satellite, and ATOM. Based on an extrapolation of the Fermi/LAT
spectrum towards the VHE γ-ray regime, we deduce a 95 per cent
confidence level upper limit on the unknown redshift of KUV 00311-1938
of $z$ < 0.98 and of PKS 1440-389 of $z$ < 0.53. When combined
with previous spectroscopy results, the redshift of KUV 00311-1938 is
constrained to 0.51 ≤ $z$ < 0.98 and of PKS 1440-389 to 0.14 ⪅
$z$ < 0.53.
---------------------------------------------------------
Title: Resolving acceleration to very high energies along the jet
of Centaurus A
Authors: H. E. S. S. Collaboration; Abdalla, H.; Adam, R.; Aharonian,
F.; Ait Benkhali, F.; Angüner, E. O.; Arakawa, M.; Arcaro, C.;
Armand, C.; Ashkar, H.; Backes, M.; Barbosa Martins, V.; Barnard, M.;
Becherini, Y.; Berge, D.; Bernlöhr, K.; Blackwell, R.; Böttcher, M.;
Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bregeon, J.; Breuhaus, M.;
Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.; Bylund, T.;
Capasso, M.; Caroff, S.; Carosi, A.; Casanova, S.; Cerruti, M.; Chand,
T.; Chandra, S.; Chen, A.; Colafrancesco, S.; Curyło, M.; Davids,
I. D.; Deil, C.; Devin, J.; deWilt, P.; Dirson, L.; Djannati-Ataï,
A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.; Drury, L. O'C.; Dyks,
J.; Egberts, K.; Emery, G.; Ernenwein, J. -P.; Eschbach, S.; Feijen,
K.; Fegan, S.; Fiasson, A.; Fontaine, G.; Funk, S.; Füßling,
M.; Gabici, S.; Gallant, Y. A.; Gaté, F.; Giavitto, G.; Glawion,
D.; Glicenstein, J. F.; Gottschall, D.; Grondin, M. -H.; Hahn, J.;
Haupt, M.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.;
Hofmann, W.; Hoischen, C.; Holch, T. L.; Holler, M.; Horns, D.;
Huber, D.; Iwasaki, H.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.;
Jardin-Blicq, A.; Jung-Richardt, I.; Kastendieck, M. A.; Katarzyński,
K.; Katsuragawa, M.; Katz, U.; Khangulyan, D.; Khélifi, B.; King,
J.; Klepser, S.; Kluźniak, W.; Komin, N.; Kosack, K.; Kostunin, D.;
Kraus, M.; Lamanna, G.; Lau, J.; Lemière, A.; Lemoine-Goumard, M.;
Lenain, J. -P.; Leser, E.; Levy, C.; Lohse, T.; Lypova, I.; Mackey,
J.; Majumdar, J.; Malyshev, D.; Marandon, V.; Marcowith, A.; Mares, A.;
Mariaud, C.; Martí-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.;
Mitchell, A. M. W.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Moore,
C.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, S.; de Naurois,
M.; Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; O'Brien,
P.; Odaka, H.; Ohm, S.; de Ona Wilhelmi, E.; Ostrowski, M.; Oya, I.;
Panter, M.; Parsons, R. D.; Perennes, C.; Petrucci, P. -O.; Peyaud,
B.; Piel, Q.; Pita, S.; Poireau, V.; Priyana Noel, A.; Prokhorov,
D. A.; Prokoph, H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab,
S.; Rauth, R.; Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Rieger,
F.; Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco,
E.; Sahakian, V.; Saito, S.; Sanchez, D. A.; Santangelo, A.; Sasaki,
M.; Schlickeiser, R.; Schüssler, F.; Schulz, A.; Schutte, H. M.;
Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.; Senniappan, M.;
Seyffert, A. S.; Shafi, N.; Shiningayamwe, K.; Simoni, R.; Sinha, A.;
Sol, H.; Specovius, A.; Spir-Jacob, M.; Stawarz, Ł.; Steenkamp, R.;
Stegmann, C.; Steppa, C.; Takahashi, T.; Tavernier, T.; Taylor, A. M.;
Terrier, R.; Tiziani, D.; Tluczykont, M.; Trichard, C.; Tsirou, M.;
Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.;
van Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter,
C.; Vincent, P.; Vink, J.; Voisin, F.; Völk, H. J.; Vuillaume, T.;
Wadiasingh, Z.; Wagner, S. J.; White, R.; Wierzcholska, A.; Yang,
R.; Yoneda, H.; Zacharias, M.; Zanin, R.; Zdziarski, A. A.; Zech,
A.; Ziegler, A.; Zorn, J.; Żywucka, N.
2020Natur.582..356H Altcode: 2020arXiv200704823T
The nearby radio galaxy Centaurus A belongs to a class of active
galaxies that are luminous at radio wavelengths. Most show collimated
relativistic outflows known as jets, which extend over hundreds
of thousands of parsecs for the most powerful sources. Accretion
of matter onto the central supermassive black hole is believed to
fuel these jets and power their emission<SUP>1</SUP>. Synchrotron
radiation from relativistic electrons causes the radio emission, and
it has been suggested that the X-ray emission from Centaurus A also
originates in electron synchrotron processes<SUP>2-4</SUP>. Another
possible explanation is inverse Compton scattering with cosmic microwave
background (CMB) soft photons<SUP>5-7</SUP>. Synchrotron radiation needs
ultrarelativistic electrons (about 50 teraelectronvolts) and, given
their short cooling times, requires some continuous re-acceleration
mechanism<SUP>8</SUP>. Inverse Compton scattering, on the other hand,
does not require very energetic electrons, but the jets must stay
highly relativistic on large scales (exceeding 1 megaparsec). Some
recent evidence disfavours inverse Compton-CMB models<SUP>9-12</SUP>,
although other work seems to be compatible with them<SUP>13,14</SUP>. In
principle, the detection of extended γ-ray emission, which directly
probes the presence of ultrarelativistic electrons, could distinguish
between these options. At gigaelectronvolt energies there is also an
unusual spectral hardening<SUP>15,16</SUP> in Centaurus A that has
not yet been explained. Here we report observations of Centaurus A at
teraelectronvolt energies that resolve its large-scale jet. We interpret
the data as evidence for the acceleration of ultrarelativistic electrons
in the jet, and favour the synchrotron explanation for the X-rays. Given
that this jet is not exceptional in terms of power, length or speed,
it is possible that ultrarelativistic electrons are commonplace in
the large-scale jets of radio-loud active galaxies.
---------------------------------------------------------
Title: Probing the Magnetic Field in the GW170817 Outflow Using
H.E.S.S. Observations
Authors: Abdalla, H.; Adam, R.; Aharonian, F.; Ait Benkhali, F.;
Angüner, E. O.; Arakawa, M.; Arcaro, C.; Armand, C.; Armstrong, T.;
Ashkar, H.; Backes, M.; Baghmanyan, V.; Barbosa-Martins, V.; Barnacka,
A.; Barnard, M.; Becherini, Y.; Berge, D.; Bernlöhr, K.; Blackwell,
R.; Böttcher, M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bregeon,
J.; Breuhaus, M.; Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik,
T.; Bylund, T.; Caroff, S.; Carosi, A.; Casanova, S.; Cerruti, M.;
Chand, T.; Chandra, S.; Chen, A.; Cotter, G.; Curyło, M.; Davids,
I. D.; Davies, J.; Deil, C.; Devin, J.; deWilt, P.; Dirson, L.;
Djannati-Ataï, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.; Dyks,
J.; Egberts, K.; Eichhorn, F.; Emery, G.; Ernenwein, J. -P.; Eschbach,
S.; Feijen, K.; Fegan, S.; Fiasson, A.; Fontaine, G.; Funk, S.;
Füßling, M.; Gabici, S.; Gallant, Y. A.; Giavitto, G.; Giunti, L.;
Glawion, D.; Glicenstein, J. F.; Gottschall, D.; Grondin, M. -H.; Hahn,
J.; Haupt, M.; Heinzelmann, G.; Hermann, G.; Hinton, J. A.; Hofmann,
W.; Hoischen, C.; Holch, T. L.; Holler, M.; Hörbe, M.; Horns, D.;
Huber, D.; Iwasaki, H.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.;
Jardin-Blicq, A.; Joshi, V.; Jung-Richardt, I.; Kastendieck, M. A.;
Katarzyński, K.; Katsuragawa, M.; Katz, U.; Khangulyan, D.; Khélifi,
B.; Klepser, S.; Kluźniak, W.; Komin, Nu.; Konno, R.; Kosack, K.;
Kostunin, D.; Kreter, M.; Lamanna, G.; Lemière, A.; Lemoine-Goumard,
M.; Lenain, J. -P.; Leser, E.; Levy, C.; Lohse, T.; Lypova, I.;
Mackey, J.; Majumdar, J.; Malyshev, D.; Malyshev, D.; Marandon, V.;
Marchegiani, P.; Marcowith, A.; Mares, A.; Martí-Devesa, G.; Marx, R.;
Maurin, G.; Meintjes, P. J.; Moderski, R.; Mohamed, M.; Mohrmann, L.;
Moore, C.; Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima,
S.; Nakashima, K.; de Naurois, M.; Ndiyavala, H.; Niederwanger,
F.; Niemiec, J.; Oakes, L.; O'Brien, P.; Odaka, H.; Ohm, S.; de Ona
Wilhelmi, E.; Ostrowski, M.; Panter, M.; Parsons, R. D.; Peyaud, B.;
Piel, Q.; Pita, S.; Poireau, V.; Noel, A. Priyana; Prokhorov, D. A.;
Prokoph, H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.;
Rauth, R.; Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Rieger, F.;
Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.;
Sahakian, V.; Sailer, S.; Saito, S.; Sanchez, D. A.; Santangelo, A.;
Sasaki, M.; Scalici, M.; Schlickeiser, R.; Schüssler, F.; Schulz,
A.; Schutte, H. M.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.;
Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shiningayamwe, K.; Simoni,
R.; Sinha, A.; Sol, H.; Specovius, A.; Spencer, S.; Spir-Jacob, M.;
Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Steppa, C.; Takahashi, T.;
Tavernier, T.; Taylor, A. M.; Terrier, R.; Tiziani, D.; Tluczykont,
M.; Tomankova, L.; Trichard, C.; Tsirou, M.; Tsuji, N.; Tuffs, R.;
Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.; van Rensburg, C.;
van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.;
Vink, J.; Völk, H. J.; Vuillaume, T.; Wadiasingh, Z.; Wagner, S. J.;
Watson, J.; Werner, F.; White, R.; Wierzcholska, A.; Yang, R.; Yoneda,
H.; Zacharias, M.; Zanin, R.; Zdziarski, A. A.; Zech, A.; Zorn, J.;
Żywucka, N.; H. E. S. S. Collaboration; Rodrigues, X.
2020ApJ...894L..16A Altcode: 2020arXiv200410105H
The detection of the first electromagnetic counterpart to the binary
neutron star (BNS) merger remnant GW170817 established the connection
between short γ-ray bursts and BNS mergers. It also confirmed the
forging of heavy elements in the ejecta (a so-called kilonova) via
the r-process nucleosynthesis. The appearance of nonthermal radio
and X-ray emission, as well as the brightening, which lasted more
than 100 days, were somewhat unexpected. Current theoretical models
attempt to explain this temporal behavior as either originating
from a relativistic off-axis jet or a kilonova-like outflow. In
either scenario, there is some ambiguity regarding how much energy
is transported in the nonthermal electrons versus the magnetic field
of the emission region. Combining the Very Large Array (radio) and
Chandra (X-ray) measurements with observations in the GeV-TeV domain
can help break this ambiguity, almost independently of the assumed
origin of the emission. Here we report for the first time on deep
H.E.S.S. observations of GW170817/GRB 170817A between 124 and 272 days
after the BNS merger with the full H.E.S.S. array of telescopes, as
well as on an updated analysis of the prompt (<5 days) observations
with the upgraded H.E.S.S. phase-I telescopes. We discuss implications
of the H.E.S.S. measurement for the magnetic field in the context of
different source scenarios.
---------------------------------------------------------
Title: Planet Hunters TESS I: TOI 813, a subgiant hosting a transiting
Saturn-sized planet on an 84-day orbit
Authors: Eisner, N. L.; Barragán, O.; Aigrain, S.; Lintott, C.;
Miller, G.; Zicher, N.; Boyajian, T. S.; Briceño, C.; Bryant, E. M.;
Christiansen, J. L.; Feinstein, A. D.; Flor-Torres, L. M.; Fridlund,
M.; Gandolfi, D.; Gilbert, J.; Guerrero, N.; Jenkins, J. M.; Jones, K.;
Kristiansen, M. H.; Vanderburg, A.; Law, N.; López-Sánchez, A. R.;
Mann, A. W.; Safron, E. J.; Schwamb, M. E.; Stassun, K. G.; Osborn,
H. P.; Wang, J.; Zic, A.; Ziegler, C.; Barnet, F.; Bean, S. J.;
Bundy, D. M.; Chetnik, Z.; Dawson, J. L.; Garstone, J.; Stenner,
A. G.; Huten, M.; Larish, S.; Melanson, L. D.; Mitchell, T.; Moore,
C.; Peltsch, K.; Rogers, D. J.; Schuster, C.; Smith, D. S.; Simister,
D. J.; Tanner, C.; Terentev, I.; Tsymbal, A.
2020MNRAS.494..750E Altcode: 2019arXiv190909094E; 2020MNRAS.tmp..148E
We report on the discovery and validation of TOI 813 b (TIC 55525572
b), a transiting exoplanet identified by citizen scientists in data
from NASA's Transiting Exoplanet Survey Satellite (TESS) and the
first planet discovered by the Planet Hunters TESS project. The
host star is a bright (V = 10.3 mag) subgiant (R<SUB>\star</SUB> -
1.94 R<SUB>⊙</SUB>, M<SUB>\star</SUB> = 1.32 M<SUB>⊙</SUB>). It
was observed almost continuously by TESS during its first year of
operations, during which time four individual transit events were
detected. The candidate passed all the standard light curve-based
vetting checks, and ground-based follow-up spectroscopy and speckle
imaging enabled us to place an upper limit of 2 M<SUB>Jup</SUB> (99 per
cent confidence) on the mass of the companion, and to statistically
validate its planetary nature. Detailed modelling of the transits
yields a period of 83.8911<SUB>-0.0031</SUB><SUP>+0.0027</SUP> d,
a planet radius of 6.71 ± 0.38 R<SUB>⊕</SUB> and a semimajor axis
of 0.423<SUB>-0.037</SUB><SUP>+0.031</SUP> AU. The planet's orbital
period combined with the evolved nature of the host star places this
object in a relatively underexplored region of parameter space. We
estimate that TOI 813 b induces a reflex motion in its host star with a
semi-amplitude of ∼6 m s<SUP>-1</SUP>, making this a promising system
to measure the mass of a relatively long-period transiting planet.
---------------------------------------------------------
Title: Detection of very-high-energy γ-ray emission from the
colliding wind binary η Car with H.E.S.S.
Authors: H. E. S. S. Collaboration; Abdalla, H.; Adam, R.; Aharonian,
F.; Ait Benkhali, F.; Angüner, E. O.; Arakawa, M.; Arcaro, C.;
Armand, C.; Armstrong, T.; Ashkar, H.; Backes, M.; Barbosa Martins,
V.; Barnard, M.; Becherini, Y.; Berge, D.; Bernlöhr, K.; Blackwell,
R.; Böttcher, M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bregeon, J.;
Breuhaus, M.; Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.;
Bylund, T.; Caroff, S.; Carosi, A.; Casanova, S.; Cerruti, M.; Chand,
T.; Chandra, S.; Chen, A.; Colafrancesco, S.; Cotter, G.; Curyło, M.;
Davids, I. D.; Davies, J.; Deil, C.; Devin, J.; deWilt, P.; Dirson,
L.; Djannati-Ataï, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.;
Dyks, J.; Egberts, K.; Eichhorn, F.; Emery, G.; Ernenwein, J. -P.;
Eschbach, S.; Feijen, K.; Fegan, S.; Fiasson, A.; Fontaine, G.; Funk,
S.; Füßling, M.; Gabici, S.; Gallant, Y. A.; Gaté, F.; Giavitto, G.;
Giunti, L.; Glawion, D.; Glicenstein, J. F.; Gottschall, D.; Grondin,
M. -H.; Hahn, J.; Haupt, M.; Heinzelmann, G.; Henri, G.; Hermann, G.;
Hinton, J. A.; Hofmann, W.; Hoischen, C.; Holch, T. L.; Holler, M.;
Hörbe, M.; Horns, D.; Huber, D.; Iwasaki, H.; Jamrozy, M.; Jankowsky,
D.; Jankowsky, F.; Jardin-Blicq, A.; Joshi, V.; Jung-Richardt, I.;
Kastendieck, M. A.; Katarzyński, K.; Katsuragawa, M.; Katz, U.;
Khangulyan, D.; Khélifi, B.; King, J.; Klepser, S.; Kluźniak,
W.; Komin, Nu.; Kosack, K.; Kostunin, D.; Kreter, M.; Lamanna, G.;
Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leser, E.; Levy,
C.; Lohse, T.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev, D.;
Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares, A.;
Martí-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Moderski,
R.; Mohamed, M.; Mohrmann, L.; Moore, C.; Morris, P.; Moulin, E.;
Muller, J.; Murach, T.; Nakashima, S.; Nakashima, K.; de Naurois,
M.; Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; O'Brien,
P.; Odaka, H.; Ohm, S.; de Ona Wilhelmi, E.; Ostrowski, M.; Panter,
M.; Parsons, R. D.; Perennes, C.; Petrucci, P. -O.; Peyaud, B.;
Piel, Q.; Pita, S.; Poireau, V.; Priyana Noel, A.; Prokhorov, D. A.;
Prokoph, H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.;
Rauth, R.; Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Rieger, F.;
Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.;
Sahakian, V.; Sailer, S.; Saito, S.; Sanchez, D. A.; Santangelo, A.;
Sasaki, M.; Scalici, M.; Schlickeiser, R.; Schüssler, F.; Schulz,
A.; Schutte, H. M.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.;
Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shiningayamwe, K.; Simoni,
R.; Sinha, A.; Sol, H.; Specovius, A.; Spencer, S.; Spir-Jacob, M.;
Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Steppa, C.; Takahashi, T.;
Tavernier, T.; Taylor, A. M.; Terrier, R.; Tiziani, D.; Tluczykont,
M.; Tomankova, L.; Trichard, C.; Tsirou, M.; Tsuji, N.; Tuffs, R.;
Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.; van Rensburg, C.;
van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.;
Vink, J.; Völk, H. J.; Vuillaume, T.; Wadiasingh, Z.; Wagner, S. J.;
Watson, J.; Werner, F.; White, R.; Wierzcholska, A.; Yang, R.; Yoneda,
H.; Zacharias, M.; Zanin, R.; Zdziarski, A. A.; Zech, A.; Zorn, J.;
Żywucka, N.
2020A&A...635A.167H Altcode: 2020arXiv200202336H; 2020A&A...635A.167.
<BR /> Aims: Colliding wind binary systems have long been suspected to
be high-energy (HE; 100 MeV < E < 100 GeV) γ-ray emitters. η
Car is the most prominent member of this object class and is
confirmed to emit phase-locked HE γ rays from hundreds of MeV to
~100 GeV energies. This work aims to search for and characterise the
very-high-energy (VHE; E >100 GeV) γ-ray emission from η Car around
the last periastron passage in 2014 with the ground-based High Energy
Stereoscopic System (H.E.S.S.). <BR /> Methods: The region around η
Car was observed with H.E.S.S. between orbital phase p = 0.78-1.10,
with a closer sampling at p ≈ 0.95 and p ≈ 1.10 (assuming a period
of 2023 days). Optimised hardware settings as well as adjustments to
the data reduction, reconstruction, and signal selection were needed to
suppress and take into account the strong, extended, and inhomogeneous
night sky background (NSB) in the η Car field of view. Tailored
run-wise Monte-Carlo simulations (RWS) were required to accurately
treat the additional noise from NSB photons in the instrument response
functions. <BR /> Results: H.E.S.S. detected VHE γ-ray emission from
the direction of η Car shortly before and after the minimum in the
X-ray light-curve close to periastron. Using the point spread function
provided by RWS, the reconstructed signal is point-like and the spectrum
is best described by a power law. The overall flux and spectral index
in VHE γ rays agree within statistical and systematic errors before
and after periastron. The γ-ray spectrum extends up to at least ~400
GeV. This implies a maximum magnetic field in a leptonic scenario in
the emission region of 0.5 Gauss. No indication for phase-locked flux
variations is detected in the H.E.S.S. data.
---------------------------------------------------------
Title: CESM-release-cesm2.1.2
Authors: Danabasoglu; Lamarque; Bacmeister; Bailey; DuVivier;
Edwards; Emmons; Fasullo; Garcia; Gettelman; Hannay; Holland; Large;
Lauritzen; Lawrence; Lenaerts; Lindsay; Lipscomb; Mills; Neale; Oleson;
Otto-Bliesner; Phillips; Sacks; Tilmes; Kampenhout, Van; Vertenstein;
Bertini; Dennis; Deser; Fischer; Fox-Kemper; Kay; Kinnison; Kushner;
Larson; Long; Mickelson; Moore; Nienhouse; Polvani; Rasch; Strand
2020zndo...3895328D Altcode:
The Community Earth System Model release version cesm2.1.2
---------------------------------------------------------
Title: X-ray Exoplanet Transits
Authors: Drake, J. J.; Kashyap, V.; Poppenhager, K.; Wolk, S.; Moore,
C.; Hong, J.; Wargelin, B.; Winston, E.; Elvis, M.; Pillitteri, I.
2020AAS...23517311D Altcode:
The evolution of planetary atmospheres is one of the most uncertain
aspects of exoplanetary astrophysics. Successful models require
knowledge of atmospheric source and loss terms and of how they change
on a large range of timescales, from days to Gyrs. Atmospheric
loss is in principle a tractable problem, depending on planetary
characteristics such as orbit, magnetic field, rotation period and
atmospheric chemical composition, and on the host star photon and
particle radiation properties that drive the loss. In practice,
the coupled physics and chemistry involved are extremely complex
and likely require sophisticated time-dependent 3D models to treat
properly. An alternative observational approach that has been pursued
in the ultraviolet is to use planetary transits to detect the escaping
gas in absorption against the stellar background light. Here, we build
on a pioneering detection of the X-ray transit of the hot Jupiter
HD189733b by Poppenhager and co-workers and highlight the utility of
the soft X-ray band for such measurements. We explore X-ray transit
observations of close-in gas giants as a potentially powerful means of
exploring planetary atmospheres and measuring scale heights, outflows
and inferring chemical compositions. The required measurements could
be obtained with either next-generation flagship missions, or with
repeated observations by much more modest small satellite missions.
---------------------------------------------------------
Title: H.E.S.S. detection of very high-energy γ-ray emission from
the quasar PKS 0736+017
Authors: H. E. S. S. Collaboration; Abdalla, H.; Adam, R.; Aharonian,
F.; Ait Benkhali, F.; Angüner, E. O.; Arakawa, M.; Arcaro, C.;
Armand, C.; Ashkar, H.; Backes, M.; Barbosa Martins, V.; Barnard, M.;
Becherini, Y.; Berge, D.; Bernlöhr, K.; Blackwell, R.; Böttcher, M.;
Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bregeon, J.; Breuhaus, M.;
Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.; Bylund, T.;
Capasso, M.; Caroff, S.; Carosi, A.; Casanova, S.; Cerruti, M.; Chand,
T.; Chandra, S.; Chen, A.; Colafrancesco, S.; Curyło, M.; Davids,
I. D.; Deil, C.; Devin, J.; deWilt, P.; Dirson, L.; Djannati-Ataï,
A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.; Drury, L. O. 'C.;
Dyks, J.; Egberts, K.; Emery, G.; Ernenwein, J. -P.; Eschbach, S.;
Feijen, K.; Fegan, S.; Fiasson, A.; Fontaine, G.; Funk, S.; Füßling,
M.; Gabici, S.; Gallant, Y. A.; Gaté, F.; Giavitto, G.; Glawion,
D.; Glicenstein, J. F.; Gottschall, D.; Grondin, M. -H.; Hahn, J.;
Haupt, M.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.;
Hofmann, W.; Hoischen, C.; Holch, T. L.; Holler, M.; Horns, D.;
Huber, D.; Iwasaki, H.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.;
Jardin-Blicq, A.; Jung-Richardt, I.; Kastendieck, M. A.; Katarzyński,
K.; Katsuragawa, M.; Katz, U.; Khangulyan, D.; Khélifi, B.; King,
J.; Klepser, S.; Kluźniak, W.; Komin, Nu.; Kosack, K.; Kostunin, D.;
Kraus, M.; Lamanna, G.; Lau, J.; Lemière, A.; Lemoine-Goumard, M.;
Lenain, J. -P.; Leser, E.; Levy, C.; Lohse, T.; Lypova, I.; Mackey,
J.; Majumdar, J.; Malyshev, D.; Marandon, V.; Marcowith, A.; Mares, A.;
Mariaud, C.; Martí-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.;
Mitchell, A. M. W.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Muller,
J.; Moore, C.; Moulin, E.; Murach, T.; Nakashima, S.; de Naurois,
M.; Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; O'Brien,
P.; Odaka, H.; Ohm, S.; de Oña Wilhelmi, E.; Ostrowski, M.; Oya, I.;
Panter, M.; Parsons, R. D.; Perennes, C.; Petrucci, P. -O.; Peyaud, B.;
Piel, Q.; Pita, S.; Poireau, V.; Priyana Noel, A.; Prokhorov, D. A.;
Prokoph, H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.;
Rauth, R.; Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Rieger, F.;
Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.;
Sahakian, V.; Saito, S.; Sanchez, D. A.; Santangelo, A.; Sasaki, M.;
Schlickeiser, R.; Schüssler, F.; Schulz, A.; Schutte, H.; Schwanke,
U.; Schwemmer, S.; Seglar-Arroyo, M.; Senniappan, M.; Seyffert,
A. S.; Shafi, N.; Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol, H.;
Specovius, A.; Spir-Jacob, M.; Stawarz, Ł.; Steenkamp, R.; Stegmann,
C.; Steppa, C.; Takahashi, T.; Tavernier, T.; Taylor, A. M.; Terrier,
R.; Tiziani, D.; Tluczykont, M.; Trichard, C.; Tsirou, M.; Tsuji,
N.; Tuffs, R.; Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.;
van Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter,
C.; Vincent, P.; Vink, J.; Voisin, F.; Völk, H. J.; Vuillaume, T.;
Wadiasingh, Z.; Wagner, S. J.; White, R.; Wierzcholska, A.; Yang,
R.; Yoneda, H.; Zacharias, M.; Zanin, R.; Zdziarski, A. A.; Zech,
A.; Ziegler, A.; Zorn, J.; Żywucka, N.; Smith, P. S.
2020A&A...633A.162H Altcode: 2019arXiv191104761H
Context. Flat-spectrum radio-quasars (FSRQs) are rarely detected at
very high energies (E ≥ 100 GeV) due to their low-frequency-peaked
spectral energy distributions. At present, only six FSRQs are
known to emit very high-energy (VHE) photons, representing only 7%
of the VHE extragalactic catalog, which is largely dominated by
high-frequency-peaked BL Lacertae objects. <BR /> Aims: Following the
detection of MeV-GeV γ-ray flaring activity from the FSRQ PKS 0736+017
(z = 0.189) with Fermi-LAT, the H.E.S.S. array of Cherenkov telescopes
triggered target-of-opportunity (ToO) observations on February 18, 2015,
with the goal of studying the γ-ray emission in the VHE band. <BR />
Methods: H.E.S.S. ToO observations were carried out during the nights
of February 18, 19, 21, and 24, 2015. Together with Fermi-LAT, the
multi-wavelength coverage of the flare includes Swift observations in
soft X-ray and optical-UV bands, and optical monitoring (photometry
and spectro-polarimetry) by the Steward Observatory, and the ATOM, the
KAIT, and the ASAS-SN telescopes. <BR /> Results: VHE emission from PKS
0736+017 was detected with H.E.S.S. only during the night of February
19, 2015. Fermi-LAT data indicate the presence of a γ-ray flare,
peaking at the time of the H.E.S.S. detection, with a flux doubling
timescale of around six hours. The γ-ray flare was accompanied by at
least a 1 mag brightening of the non-thermal optical continuum. No
simultaneous observations at longer wavelengths are available for
the night of the H.E.S.S. detection. The γ-ray observations with
H.E.S.S. and Fermi-LAT are used to put constraints on the location
of the γ-ray emitting region during the flare: it is constrained to
be just outside the radius of the broad-line region r<SUB>BLR</SUB>
with a bulk Lorentz factor Γ ≃ 20, or at the level of the radius of
the dusty torus r<SUB>torus</SUB> with Γ ≃ 60. <BR /> Conclusions:
PKS 0736+017 is the seventh FSRQ known to emit VHE photons, and at
z = 0.189 is the nearest so far. The location of the γ-ray emitting
region during the flare can be tightly constrained thanks to opacity,
variability, and collimation arguments.
---------------------------------------------------------
Title: Solar Soft X-ray Variations from the 2008-2019 Solar Cycle
inferred from CORONAS/SphinX, GOES/XRS, Hinode/XRT, MinXSS, NuSTAR,
and RHESSI Instruments
Authors: Moore, C.; Takeda, A.; Sylwester, B.; Sylwester, J.; Hannah,
I.; Dennis, B.; Reeves, K.; Woods, T.
2020AAS...23535901M Altcode:
The Solar spectral irradiance (SSI) is vital for understanding the
physics of all layers of the solar atmosphere from the photosphere to
the corona. While most of the contribution to the Total Solar Irradiance
(TSI) reside in visible and infrared light, the UV and X-rays have the
largest change in magnitude. Quantifying the UV and X-ray variations
over the solar cycle is critical for constraining the physics of solar
flares, active regions, the quiet Sun, as well as the atmospheres
of planets and moons in the heliosphere. The GOES/XRS spectrally
integrated 0.1 - 0.8 nm energy flux has been a longstanding diagnostic
of soft x-ray variations, but is limited by non-linearities in signal
response for low solar flux levels and an observed minimum detection
limit. The Hinode/XRT filter images provide a unique alternative proxy
for solar soft X-ray flux inferences with larger dynamic range and a
lower flux sensitivity. We compare the spectral irradiance estimate
from a Hinode/XRT filter-ratio technique results to the lowest spectra
measured-to-date between 1.25 - 3 keV by CORONAS/SPhinX in 2009,
and MinXSS CubeSat spectra in 2016 - 2019. We also highlight the
large variability in the soft X-ray spectra as directly measured by
CORONAS/SphinX, MinXSS, NuSTAR, and RHESSI intermittently between 2009
- 2019.
---------------------------------------------------------
Title: SmallSat Solar Axion and Activity X-ray Imager (SSAXI)
Authors: Hong, J.; Romaine, S.; Kenter, A.; Moore, C.; Reeves, K.;
Ramsey, B.; Kilaru, K.; Vogel, J.; Ruz Armendariz, J.; Hudson, H.;
Perez, K.
2020AAS...23527101H Altcode:
The axion is a promising dark matter candidate as well as a solution
to the strong charge-parity (CP) problem in quantum chromodynamics
(QCD). We describe a new concept for SmallSat Solar Axion and Activity
X-ray Telescope (SSAXI) to search for solar axions or axion-like
particles (ALPs) and to monitor solar activity over a wide dynamic
range. SSAXI aims to unambiguously identify X-rays converted from
axions in the solar magnetic field along the line of sight to the
solar core, effectively imaging the solar core. SSAXI employs Miniature
lightweight Wolter-I focusing X-ray optics (MiXO) and monolithic CMOS
X-ray sensors in a compact package. The wide energy range (0.5 - 5 keV)
of SSAXI can easily distinguish spectra of axion-converted X-rays
from solar X-ray spectra, while encompassing the prime energy band
(3 - 4.5 keV) of axion-converted X-rays. The high angular resolution
(30 arcsec) and large field of view (40 arcmin) in SSAXI will easily
resolve the enhanced X-ray flux over the 3 arcmin wide solar core
while fully covering the X-ray activity over the entire solar disc. The
fast readout in the inherently radiation tolerant CMOS X-ray sensors
enables high resolution spectroscopy over a wide dynamic range with a
broad range of operational temperatures. We present multiple mission
implementation options for SSAXI under ESPA class. SSAXI will operate
in a Sun-synchronous orbit for 1 yr preferably near a solar minimum
to accumulate sufficient X-ray photon statistics.
---------------------------------------------------------
Title: H.E.S.S. and Fermi-LAT observations of PSR B1259-63/LS 2883
during its 2014 and 2017 periastron passages
Authors: H. E. S. S. Collaboration; Abdalla, H.; Adam, R.; Aharonian,
F.; Ait Benkhali, F.; Angüner, E. O.; Arakawa, M.; Arcaro, C.;
Armand, C.; Ashkar, H.; Backes, M.; Barbosa Martins, V.; Barnard, M.;
Becherini, Y.; Berge, D.; Bernlöhr, K.; Blackwell, R.; Böttcher,
M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bregeon, J.; Breuhaus,
M.; Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.; Bylund,
T.; Caroff, S.; Carosi, A.; Casanova, S.; Cerruti, M.; Chand, T.;
Chandra, S.; Chaves, R. C. G.; Chen, A.; Colafrancesco, S.; Curyło,
M.; Davids, I. D.; Deil, C.; Devin, J.; deWilt, P.; Dirson, L.;
Djannati-Ataï, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.;
Dyks, J.; Egberts, K.; Emery, G.; Ernenwein, J. -P.; Eschbach,
S.; Feijen, K.; Fegan, S.; Fiasson, A.; Fontaine, G.; Funk, S.;
Füßling, M.; Gabici, S.; Gallant, Y. A.; Gaté, F.; Giavitto,
G.; Giunti, L.; Glawion, D.; Glicenstein, J. F.; Gottschall, D.;
Grondin, M. -H.; Hahn, J.; Haupt, M.; Heinzelmann, G.; Henri,
G.; Hermann, G.; Hinton, J. A.; Hofmann, W.; Hoischen, C.; Holch,
T. L.; Holler, M.; Horns, D.; Huber, D.; Iwasaki, H.; Jamrozy, M.;
Jankowsky, D.; Jankowsky, F.; Jardin-Blicq, A.; Jung-Richardt, I.;
Kastendieck, M. A.; Katarzyński, K.; Katsuragawa, M.; Katz, U.;
Khangulyan, D.; Khélifi, B.; King, J.; Klepser, S.; Kluźniak,
W.; Komin, Nu.; Kosack, K.; Kostunin, D.; Kreter, M.; Lamanna, G.;
Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leser, E.; Levy,
C.; Lohse, T.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev, D.;
Malyshev, D.; Marandon, V.; Marcowith, A.; Mares, A.; Mariaud, C.;
Martí-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Mitchell,
A. M. W.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Moore, C.; Moulin,
E.; Muller, J.; Murach, T.; Nakashima, S.; de Naurois, M.; Ndiyavala,
H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; O'Brien, P.; Odaka,
H.; Ohm, S.; de Ona Wilhelmi, E.; Ostrowski, M.; Oya, I.; Panter, M.;
Parsons, R. D.; Perennes, C.; Petrucci, P. -O.; Peyaud, B.; Piel, Q.;
Pita, S.; Poireau, V.; Priyana Noel, A.; Prokhorov, D. A.; Prokoph,
H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Rauth, R.;
Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Rieger, F.; Rinchiuso,
L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.; Sahakian,
V.; Sailer, S.; Saito, S.; Sanchez, D. A.; Santangelo, A.; Sasaki,
M.; Schlickeiser, R.; Schüssler, F.; Schulz, A.; Schutte, H. M.;
Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.; Senniappan, M.;
Seyffert, A. S.; Shafi, N.; Shiningayamwe, K.; Simoni, R.; Sinha, A.;
Sol, H.; Specovius, A.; Spir-Jacob, M.; Stawarz, Ł.; Steenkamp, R.;
Stegmann, C.; Steppa, C.; Takahashi, T.; Tavernier, T.; Taylor, A. M.;
Terrier, R.; Tiziani, D.; Tluczykont, M.; Trichard, C.; Tsirou, M.;
Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.;
van Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter,
C.; Vincent, P.; Vink, J.; Völk, H. J.; Vuillaume, T.; Wadiasingh,
Z.; Wagner, S. J.; White, R.; Wierzcholska, A.; Yang, R.; Yoneda,
H.; Zacharias, M.; Zanin, R.; Zdziarski, A. A.; Zech, A.; Zorn, J.;
Żywucka, N.; Bordas, P.
2020A&A...633A.102H Altcode: 2019arXiv191205868H
Context. PSR B1259-63/LS 2883 is a gamma-ray binary system consisting
of a pulsar in an eccentric orbit around a bright Oe stellar-type
companion star that features a dense circumstellar disc. The
bright broad-band emission observed at phases close to periastron
offers a unique opportunity to study particle acceleration and
radiation processes in binary systems. Observations at gamma-ray
energies constrain these processes through variability and spectral
characterisation studies. <BR /> Aims: The high- and very-high-energy
(HE, VHE) gamma-ray emission from PSR B1259-63/LS 2883 around the
times of its periastron passage are characterised, in particular, at
the time of the HE gamma-ray flares reported to have occurred in 2011,
2014, and 2017. Short-term and average emission characteristics of PSR
B1259-63/LS 2883 are determined. Super-orbital variability is searched
for in order to investigate possible cycle-to-cycle VHE flux changes
due to different properties of the companion star's circumstellar disc
and/or the conditions under which the HE gamma-ray flares develop. <BR
/> Methods: Spectra and light curves were derived from observations
conducted with the H.E.S.S-II array in 2014 and 2017. Phase-folded
light curves are compared with the results obtained in 2004, 2007,
and 2011. Fermi-LAT observations from 2010/11, 2014, and 2017 are
analysed. <BR /> Results: A local double-peak profile with asymmetric
peaks in the VHE light curve is measured, with a flux minimum at the
time of periastron t<SUB>p</SUB> and two peaks coinciding with the
times at which the neutron star crosses the companion's circumstellar
disc (~t<SUB>p</SUB> ± 16 d). A high VHE gamma-ray flux is also
observed at the times of the HE gamma-ray flares (~t<SUB>p</SUB> +
30 d) and at phases before the first disc crossing (~t<SUB>p</SUB> -
35 d). The spectral energy range now extends to below 200 GeV and up to
~45 TeV. <BR /> Conclusions: PSR B1259-63/LS 2883 displays periodic flux
variability at VHE gamma-rays without clear signatures of super-orbital
modulation in the time span covered by the monitoring of the source
with the H.E.S.S. telescopes. This flux variability is most probably
caused by the changing environmental conditions, particularly at times
close to periastron passage at which the neutron star is thought to
cross the circumstellar disc of the companion star twice. In contrast,
the photon index remains unchanged within uncertainties for about
200 d around periastron. At HE gamma-rays, PSR B1259-63/LS 2883 has
now been detected also before and after periastron, close to the disc
crossing times. Repetitive flares with distinct variability patterns
are detected in this energy range. Such outbursts are not observed
at VHEs, although a relatively high emission level is measured. The
spectra obtained in both energy regimes displays a similar slope,
although a common physical origin either in terms of a related particle
population, emission mechanism, or emitter location is ruled out.
---------------------------------------------------------
Title: A very-high-energy component deep in the γ-ray burst afterglow
Authors: Abdalla, H.; Adam, R.; Aharonian, F.; Ait Benkhali, F.;
Angüner, E. O.; Arakawa, M.; Arcaro, C.; Armand, C.; Ashkar, H.;
Backes, M.; Barbosa Martins, V.; Barnard, M.; Becherini, Y.; Berge, D.;
Bernlöhr, K.; Bissaldi, E.; Blackwell, R.; Böttcher, M.; Boisson,
C.; Bolmont, J.; Bonnefoy, S.; Bregeon, J.; Breuhaus, M.; Brun, F.;
Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.; Bylund, T.; Capasso, M.;
Caroff, S.; Carosi, A.; Casanova, S.; Cerruti, M.; Chand, T.; Chandra,
S.; Chen, A.; Colafrancesco, S.; Curyło, M.; Davids, I. D.; Deil,
C.; Devin, J.; deWilt, P.; Dirson, L.; Djannati-Ataï, A.; Dmytriiev,
A.; Donath, A.; Doroshenko, V.; Dyks, J.; Egberts, K.; Emery, G.;
Ernenwein, J. -P.; Eschbach, S.; Feijen, K.; Fegan, S.; Fiasson, A.;
Fontaine, G.; Funk, S.; Füßling, M.; Gabici, S.; Gallant, Y. A.;
Gaté, F.; Giavitto, G.; Giunti, L.; Glawion, D.; Glicenstein, J. F.;
Gottschall, D.; Grondin, M. -H.; Hahn, J.; Haupt, M.; Heinzelmann,
G.; Henri, G.; Hermann, G.; Hinton, J. A.; Hofmann, W.; Hoischen, C.;
Holch, T. L.; Holler, M.; Horns, D.; Huber, D.; Iwasaki, H.; Jamrozy,
M.; Jankowsky, D.; Jankowsky, F.; Jardin-Blicq, A.; Jung-Richardt,
I.; Kastendieck, M. A.; Katarzyński, K.; Katsuragawa, M.; Katz,
U.; Khangulyan, D.; Khélifi, B.; King, J.; Klepser, S.; Kluźniak,
W.; Komin, Nu.; Kosack, K.; Kostunin, D.; Kreter, M.; Lamanna, G.;
Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leser, E.; Levy,
C.; Lohse, T.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev, D.;
Marandon, V.; Marcowith, A.; Mares, A.; Mariaud, C.; Martí-Devesa,
G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Mitchell, A. M. W.;
Moderski, R.; Mohamed, M.; Mohrmann, L.; Moore, C.; Moulin, E.;
Muller, J.; Murach, T.; Nakashima, S.; de Naurois, M.; Ndiyavala,
H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; O'Brien, P.; Odaka,
H.; Ohm, S.; de Ona Wilhelmi, E.; Ostrowski, M.; Oya, I.; Panter, M.;
Parsons, R. D.; Perennes, C.; Petrucci, P. -O.; Peyaud, B.; Piel, Q.;
Pita, S.; Poireau, V.; Priyana Noel, A.; Prokhorov, D. A.; Prokoph,
H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Rauth, R.;
Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Rieger, F.; Rinchiuso,
L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.; Sahakian,
V.; Sailer, S.; Saito, S.; Sanchez, D. A.; Santangelo, A.; Sasaki,
M.; Schlickeiser, R.; Schüssler, F.; Schulz, A.; Schutte, H. M.;
Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.; Senniappan, M.;
Seyffert, A. S.; Shafi, N.; Shiningayamwe, K.; Simoni, R.; Sinha, A.;
Sol, H.; Specovius, A.; Spir-Jacob, M.; Stawarz, Ł.; Steenkamp, R.;
Stegmann, C.; Steppa, C.; Takahashi, T.; Tavernier, T.; Taylor, A. M.;
Terrier, R.; Tiziani, D.; Tluczykont, M.; Trichard, C.; Tsirou, M.;
Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.;
van Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter,
C.; Vincent, P.; Vink, J.; Völk, H. J.; Vuillaume, T.; Wadiasingh,
Z.; Wagner, S. J.; White, R.; Wierzcholska, A.; Yang, R.; Yoneda,
H.; Zacharias, M.; Zanin, R.; Zdziarski, A. A.; Zech, A.; Ziegler,
A.; Zorn, J.; Żywucka, N.; de Palma, F.; Axelsson, M.; Roberts, O. J.
2019Natur.575..464A Altcode: 2019arXiv191108961A
Gamma-ray bursts (GRBs) are brief flashes of γ-rays and are
considered to be the most energetic explosive phenomena in the
Universe<SUP>1</SUP>. The emission from GRBs comprises a short
(typically tens of seconds) and bright prompt emission, followed by a
much longer afterglow phase. During the afterglow phase, the shocked
outflow—produced by the interaction between the ejected matter and the
circumburst medium—slows down, and a gradual decrease in brightness
is observed<SUP>2</SUP>. GRBs typically emit most of their energy
via γ-rays with energies in the kiloelectronvolt-to-megaelectronvolt
range, but a few photons with energies of tens of gigaelectronvolts
have been detected by space-based instruments<SUP>3</SUP>. However,
the origins of such high-energy (above one gigaelectronvolt) photons
and the presence of very-high-energy (more than 100 gigaelectronvolts)
emission have remained elusive<SUP>4</SUP>. Here we report observations
of very-high-energy emission in the bright GRB 180720B deep in the
GRB afterglow—ten hours after the end of the prompt emission phase,
when the X-ray flux had already decayed by four orders of magnitude. Two
possible explanations exist for the observed radiation: inverse Compton
emission and synchrotron emission of ultrarelativistic electrons. Our
observations show that the energy fluxes in the X-ray and γ-ray range
and their photon indices remain comparable to each other throughout
the afterglow. This discovery places distinct constraints on the GRB
environment for both emission mechanisms, with the inverse Compton
explanation alleviating the particle energy requirements for the
emission observed at late times. The late timing of this detection
has consequences for the future observations of GRBs at the highest
energies.
---------------------------------------------------------
Title: Data-driven modeling of electron recoil nucleation in PICO
C<SUB>3</SUB>F<SUB>8</SUB> 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
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 C<SUB>3</SUB>F<SUB>8</SUB> 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<SUP>-2</SUP> 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<SUP>-2</SUP> .
---------------------------------------------------------
Title: CESM-release-cesm2.1.1
Authors: Danabasoglu; Lamarque; Bacmeister; Bailey; DuVivier;
Edwards; Emmons; Fasullo; Garcia; Gettelman; Hannay; Holland; Large;
Lauritzen; Lawrence; Lenaerts; Lindsay; Lipscomb; Mills; Neale; Oleson;
Otto-Bliesner; Phillips; Sacks; Tilmes; Kampenhout, van; Vertenstein;
Bertini; Dennis; Deser; Fischer; Fox-Kemper; Kay; Kinnison; Kushner;
Larson; Long; Mickelson; Moore; Nienhouse; Polvani; Rasch; Strand
2019zndo...3895315D Altcode:
The Community Climate Earth System Model release version cesm2.1.1
---------------------------------------------------------
Title: H.E.S.S. observations of the flaring gravitationally lensed
galaxy PKS 1830-211
Authors: H. E. S. S. Collaboration; Abdalla, H.; Aharonian, F.; Ait
Benkhali, F.; Angüner, E. O.; Arakawa, M.; Arcaro, C.; Armand, C.;
Arrieta, M.; Backes, M.; Barnard, M.; Becherini, Y.; Becker Tjus, J.;
Berge, D.; Bernlöhr, K.; Blackwell, R.; Böttcher, M.; Boisson, C.;
Bolmont, J.; Bonnefoy, S.; Bordas, P.; Bregeon, J.; Brun, F.; Brun,
P.; Bryan, M.; Büchele, M.; Bulik, T.; Bylund, T.; Capasso, M.;
Caroff, S.; Carosi, A.; Casanova, S.; Cerruti, M.; Chakraborty, N.;
Chand, T.; Chandra, S.; Chaves, R. C. G.; Chen, A.; Colafrancesco, S.;
Condon, B.; Davids, I. D.; Deil, C.; Devin, J.; deWilt, P.; Dirson, L.;
Djannati-Ataï, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.; Drury,
L. O'C.; Dyks, J.; Egberts, K.; Emery, G.; Ernenwein, J. -P.; Eschbach,
S.; Fegan, S.; Fiasson, A.; Fontaine, G.; Funk, S.; Füßling, M.;
Gabici, S.; Gallant, Y. A.; Gaté, F.; Giavitto, G.; Glawion, D.;
Glicenstein, J. F.; Gottschall, D.; Grondin, M. -H.; Hahn, J.; Haupt,
M.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.; Hofmann,
W.; Hoischen, C.; Holch, T. L.; Holler, M.; Horns, D.; Huber, D.;
Iwasaki, H.; Jacholkowska, A.; Jamrozy, M.; Jankowsky, D.; Jankowsky,
F.; Jouvin, L.; Jung-Richardt, I.; Kastendieck, M. A.; Katarzyński,
K.; Katsuragawa, M.; Katz, U.; Khangulyan, D.; Khélifi, B.; King,
J.; Klepser, S.; Kluźniak, W.; Komin, Nu; Kosack, K.; Kraus, M.;
Lamanna, G.; Lau, J.; Lefaucheur, J.; Lemière, A.; Lemoine-Goumard,
M.; Lenain, J. -P.; Leser, E.; Lohse, T.; López-Coto, R.; Lorentz,
M.; Lypova, I.; Malyshev, D.; Marandon, V.; Marcowith, A.; Mariaud,
C.; Martí-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.;
Mitchell, A. M. W.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Moore,
C.; Moulin, E.; Murach, T.; Nakashima, S.; de Naurois, M.; Ndiyavala,
H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; O'Brien, P.; Odaka, H.;
Ohm, S.; Ostrowski, M.; Oya, I.; Panter, M.; Parsons, R. D.; Perennes,
C.; Petrucci, P. -O.; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V.;
Priyana Noel, A.; Prokhorov, D. A.; Prokoph, H.; Pühlhofer, G.;
Punch, M.; Quirrenbach, A.; Raab, S.; Rauth, R.; Reimer, A.; Reimer,
O.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli, C.; Rowell, G.;
Rudak, B.; Ruiz-Velasco, E.; Sahakian, V.; Saito, S.; Sanchez, D. A.;
Santangelo, A.; Sasaki, M.; Schlickeiser, R.; Schüssler, F.; Schulz,
A.; Schutte, H.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.;
Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shilon, I.; Shiningayamwe,
K.; Simoni, R.; Sinha, A.; Sol, H.; Specovius, A.; Spir-Jacob, M.;
Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Steppa, C.; Takahashi, T.;
Tavernet, J. -P.; Tavernier, T.; Taylor, A. M.; Terrier, R.; Tiziani,
D.; Tluczykont, M.; Trichard, C.; Tsirou, M.; Tsuji, N.; Tuffs, R.;
Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.; van Rensburg, C.;
van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.;
Vink, J.; Voisin, F.; Völk, H. J.; Vuillaume, T.; Wadiasingh, Z.;
Wagner, S. J.; Wagner, R. M.; White, R.; Wierzcholska, A.; Yang, R.;
Yoneda, H.; Zaborov, D.; Zacharias, M.; Zanin, R.; Zdziarski, A. A.;
Zech, A.; Ziegler, A.; Zorn, J.; Żywucka, N.
2019MNRAS.486.3886H Altcode: 2019MNRAS.tmp.1061A; 2019arXiv190405139H
PKS 1830-211 is a known macrolensed quasar located at a redshift of z
= 2.5. Its high-energy gamma-ray emission has been detected with the
Fermi-Large Area Telescope (LAT) instrument and evidence for lensing
was obtained by several authors from its high-energy data. Observations
of PKS 1830-211 were taken with the High Energy Stereoscopic System
(H.E.S.S.) array of Imaging Atmospheric Cherenkov Telescopes in 2014
August, following a flare alert by the Fermi-LAT Collaboration. The
H.E.S.S observations were aimed at detecting a gamma-ray flare delayed
by 20-27 d from the alert flare, as expected from observations at other
wavelengths. More than 12 h of good-quality data were taken with an
analysis threshold of ∼67 GeV. The significance of a potential signal
is computed as a function of the date and the average significance
over the whole period. Data are compared to simultaneous observations
by Fermi-LAT. No photon excess or significant signal is detected. An
upper limit on PKS 1830-211 flux above 67 GeV is computed and compared
to the extrapolation of the Fermi-LAT flare spectrum.
---------------------------------------------------------
Title: Dark matter search results from the complete exposure of the
PICO-60 C<SUB>3</SUB>F<SUB>8</SUB> 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
2019PhRvD.100b2001A Altcode: 2019arXiv190204031A
Final results are reported from operation of the PICO-60
C<SUB>3</SUB>F<SUB>8</SUB> dark matter detector, a bubble chamber
filled with 52 kg of C<SUB>3</SUB> F<SUB>8</SUB> 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<SUP>-41</SUP> cm<SUP>2</SUP> for a 25 GeV WIMP, improving
on previous PICO results for 3-5 GeV WIMPs by an order of magnitude.
---------------------------------------------------------
Title: H.E.S.S. and Suzaku observations of the Vela X pulsar wind
nebula
Authors: H. E. S. S. Collaboration; Abdalla, H.; Aharonian, F.;
Ait Benkhali, F.; Angüner, E. O.; Arakawa, M.; Arcaro, C.; Armand,
C.; Backes, M.; Barnard, M.; Becherini, Y.; Berge, D.; Bernlöhr, K.;
Blackwell, R.; Böttcher, M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.;
Bregeon, J.; Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.;
Bylund, T.; Capasso, M.; Caroff, S.; Carosi, A.; Casanova, S.; Cerruti,
M.; Chakraborty, N.; Chand, T.; Chandra, S.; Chaves, R. C. G.; Chen,
A.; Colafrancesco, S.; Condon, B.; Davids, I. D.; Deil, C.; Devin, J.;
deWilt, P.; Dirson, L.; Djannati-Ataï, A.; Dmytriiev, A.; Donath,
A.; Doroshenko, V.; Drury, L. O. 'C.; Dyks, J.; Egberts, K.; Emery,
G.; Ernenwein, J. -P.; Eschbach, S.; Feijen, K.; Fegan, S.; Fiasson,
A.; Fontaine, G.; Funk, S.; Füßling, M.; Gabici, S.; Gallant, Y. A.;
Gaté, F.; Giavitto, G.; Glawion, D.; Glicenstein, J. F.; Gottschall,
D.; Grondin, M. -H.; Hahn, J.; Haupt, M.; Heinzelmann, G.; Henri, G.;
Hermann, G.; Hinton, J. A.; Hofmann, W.; Hoischen, C.; Holch, T. L.;
Holler, M.; Horns, D.; Huber, D.; Iwasaki, H.; Jacholkowska, A.;
Jamrozy, M.; Jankowsky, D.; Jankowsky, F.; Jouvin, L.; Jung-Richardt,
I.; Kastendieck, M. A.; Katarzyński, K.; Katsuragawa, M.; Katz, U.;
Khangulyan, D.; Khélifi, B.; King, J.; Klepser, S.; Kluźniak, W.;
Komin, Nu.; Kosack, K.; Kostunin, D.; Kraus, M.; Lamanna, G.; Lau, J.;
Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leser, E.; Lohse,
T.; López-Coto, R.; Lypova, I.; Malyshev, D.; Marandon, V.; Marcowith,
A.; Mariaud, C.; Martí-Devesa, G.; Marx, R.; Maurin, G.; Maxted,
N. I.; Meintjes, P. J.; Mitchell, A. M. W.; Moderski, R.; Mohamed,
M.; Mohrmann, L.; Moore, C.; Moulin, E.; Murach, T.; Nakashima, S.;
de Naurois, M.; Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes,
L.; O'Brien, P.; Odaka, H.; Ohm, S.; de Ona Wilhelmi, E.; Ostrowski,
M.; Oya, I.; Panter, M.; Parsons, R. D.; Perennes, C.; Petrucci,
P. -O.; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V.; Priyana Noel, A.;
Prokhorov, D. A.; Prokoph, H.; Pühlhofer, G.; Punch, M.; Quirrenbach,
A.; Raab, S.; Rauth, R.; Reimer, A.; Reimer, O.; Renaud, M.; Rieger,
F.; Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.;
Sahakian, V.; Saito, S.; Sanchez, D. A.; Santangelo, A.; Sasaki, M.;
Schlickeiser, R.; Schüssler, F.; Schulz, A.; Schutte, H.; Schwanke,
U.; Schwemmer, S.; Seglar-Arroyo, M.; Senniappan, M.; Seyffert, A. S.;
Shafi, N.; Shilon, I.; Shiningayamwe, K.; Simoni, R.; Sinha, A.;
Sol, H.; Specovius, A.; Spir-Jacob, M.; Stawarz, Ł.; Steenkamp, R.;
Stegmann, C.; Steppa, C.; Takahashi, T.; Tavernet, J. -P.; Tavernier,
T.; Taylor, A. M.; Terrier, R.; Tibaldo, L.; Tiziani, D.; Tluczykont,
M.; Trichard, C.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.;
van der Walt, D. J.; van Eldik, C.; van Rensburg, C.; van Soelen,
B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.;
Voisin, F.; Völk, H. J.; Vuillaume, T.; Wadiasingh, Z.; Wagner,
S. J.; White, R.; Wierzcholska, A.; Yang, R.; Yoneda, H.; Zaborov,
D.; Zacharias, M.; Zanin, R.; Zdziarski, A. A.; Zech, A.; Ziegler,
A.; Zorn, J.; Żywucka, N.
2019A&A...627A.100H Altcode: 2019arXiv190507975H
Context. Pulsar wind nebulae (PWNe) represent the most prominent
population of Galactic very-high-energy gamma-ray sources and are
thought to be an efficient source of leptonic cosmic rays. Vela X is
a nearby middle-aged PWN, which shows bright X-ray and TeV gamma-ray
emission towards an elongated structure called the cocoon. <BR /> Aims:
Since TeV emission is likely inverse-Compton emission of electrons,
predominantly from interactions with the cosmic microwave background,
while X-ray emission is synchrotron radiation of the same electrons,
we aim to derive the properties of the relativistic particles
and of magnetic fields with minimal modelling. <BR /> Methods:
We used data from the Suzaku XIS to derive the spectra from three
compact regions in Vela X covering distances from 0.3 to 4 pc from
the pulsar along the cocoon. We obtained gamma-ray spectra of the
same regions from H.E.S.S. observations and fitted a radiative model
to the multi-wavelength spectra. <BR /> Results: The TeV electron
spectra and magnetic field strengths are consistent within the
uncertainties for the three regions, with energy densities of the
order 10<SUP>-12</SUP> erg cm<SUP>-3</SUP>. The data indicate the
presence of a cutoff in the electron spectrum at energies of 100 TeV
and a magnetic field strength of 6 μG. Constraints on the presence of
turbulent magnetic fields are weak. <BR /> Conclusions: The pressure
of TeV electrons and magnetic fields in the cocoon is dynamically
negligible, requiring the presence of another dominant pressure
component to balance the pulsar wind at the termination shock. Sub-TeV
electrons cannot completely account for the missing pressure, which
may be provided either by relativistic ions or from mixing of the
ejecta with the pulsar wind. The electron spectra are consistent with
expectations from transport scenarios dominated either by advection
via the reverse shock or by diffusion, but for the latter the role
of radiative losses near the termination shock needs to be further
investigated in the light of the measured cutoff energies. Constraints
on turbulent magnetic fields and the shape of the electron cutoff
can be improved by spectral measurements in the energy range ≳ 10
keV. <P />Spectra are only available at the CDS via anonymous ftp to <A
href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
(ftp://130.79.128.5) or via <A
href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/627/A100">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/627/A100</A>
---------------------------------------------------------
Title: Constraints on the emission region of <ASTROBJ>3C 279</ASTROBJ>
during strong flares in 2014 and 2015 through VHE γ-ray observations
with H.E.S.S.
Authors: H. E. S. S. Collaboration; Abdalla, H.; Adam, R.; Aharonian,
F.; Ait Benkhali, F.; Angüner, E. O.; Arakawa, M.; Arcaro, C.;
Armand, C.; Ashkar, H.; Backes, M.; Barbosa Martins, V.; Barnard, M.;
Becherini, Y.; Berge, D.; Bernlöhr, K.; Blackwell, R.; Böttcher, M.;
Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bregeon, J.; Breuhaus, M.;
Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.; Bylund, T.;
Capasso, M.; Caroff, S.; Carosi, A.; Casanova, S.; Cerruti, M.; Chand,
T.; Chandra, S.; Chen, A.; Colafrancesco, S.; Curyło, M.; Davids,
I. D.; Deil, C.; Devin, J.; deWilt, P.; Dirson, L.; Djannati-Ataï,
A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.; Drury, L. O. 'C.;
Dyks, J.; Egberts, K.; Emery, G.; Ernenwein, J. -P.; Eschbach, S.;
Feijen, K.; Fegan, S.; Fiasson, A.; Fontaine, G.; Funk, S.; Füßling,
M.; Gabici, S.; Gallant, Y. A.; Gaté, F.; Giavitto, G.; Glawion,
D.; Glicenstein, J. F.; Gottschall, D.; Grondin, M. -H.; Hahn, J.;
Haupt, M.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.;
Hofmann, W.; Hoischen, C.; Holch, T. L.; Holler, M.; Horns, D.;
Huber, D.; Iwasaki, H.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.;
Jardin-Blicq, A.; Jung-Richardt, I.; Kastendieck, M. A.; Katarzyński,
K.; Katsuragawa, M.; Katz, U.; Khangulyan, D.; Khélifi, B.; King,
J.; Klepser, S.; Kluźniak, W.; Komin, Nu.; Kosack, K.; Kostunin, D.;
Kraus, M.; Lamanna, G.; Lau, J.; Lemière, A.; Lemoine-Goumard, M.;
Lenain, J. -P.; Leser, E.; Levy, C.; Lohse, T.; Lypova, I.; Mackey,
J.; Majumdar, J.; Malyshev, D.; Marandon, V.; Marcowith, A.; Mares, A.;
Mariaud, C.; Martí-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.;
Mitchell, A. M. W.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Moore,
C.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, S.; de Naurois,
M.; Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; O'Brien,
P.; Odaka, H.; Ohm, S.; de Ona Wilhelmi, E.; Ostrowski, M.; Oya, I.;
Panter, M.; Parsons, R. D.; Perennes, C.; Petrucci, P. -O.; Peyaud, B.;
Piel, Q.; Pita, S.; Poireau, V.; Priyana Noel, A.; Prokhorov, D. A.;
Prokoph, H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.;
Rauth, R.; Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Rieger, F.;
Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.;
Sahakian, V.; Saito, S.; Sanchez, D. A.; Santangelo, A.; Sasaki, M.;
Schlickeiser, R.; Schüssler, F.; Schulz, A.; Schutte, H.; Schwanke,
U.; Schwemmer, S.; Seglar-Arroyo, M.; Senniappan, M.; Seyffert,
A. S.; Shafi, N.; Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol, H.;
Specovius, A.; Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann,
C.; Steppa, C.; Takahashi, T.; Tavernier, T.; Taylor, A. M.; Terrier,
R.; Tiziani, D.; Tluczykont, M.; Trichard, C.; Tsirou, M.; Tsuji,
N.; Tuffs, R.; Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.;
van Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter,
C.; Vincent, P.; Vink, J.; Voisin, F.; Völk, H. J.; Vuillaume, T.;
Wadiasingh, Z.; Wagner, S. J.; White, R.; Wierzcholska, A.; Yang,
R.; Yoneda, H.; Zacharias, M.; Zanin, R.; Zdziarski, A. A.; Zech,
A.; Ziegler, A.; Zorn, J.; Żywucka, N.; Meyer, M.
2019A&A...627A.159H Altcode: 2019arXiv190604996H
The flat spectrum radio quasar <ASTROBJ>3C 279</ASTROBJ> is known
to exhibit pronounced variability in the high-energy (100 MeV <
E < 100 GeV) γ-ray band, which is continuously monitored with
Fermi-LAT. During two periods of high activity in April 2014 and June
2015 target-of-opportunity observations were undertaken with the
High Energy Stereoscopic System (H.E.S.S.) in the very-high-energy
(VHE, E > 100 GeV) γ-ray domain. While the observation in 2014
provides an upper limit, the observation in 2015 results in a signal
with 8.7σ significance above an energy threshold of 66 GeV. No
VHE variability was detected during the 2015 observations. The VHE
photon spectrum is soft and described by a power-law index of 4.2
± 0.3. The H.E.S.S. data along with a detailed and contemporaneous
multiwavelength data set provide constraints on the physical parameters
of the emission region. The minimum distance of the emission region from
the central black hole was estimated using two plausible geometries
of the broad-line region and three potential intrinsic spectra. The
emission region is confidently placed at r ≳ 1.7 × 10<SUP>17</SUP>
cm from the black hole, that is beyond the assumed distance of the
broad-line region. Time-dependent leptonic and lepto-hadronic one-zone
models were used to describe the evolution of the 2015 flare. Neither
model can fully reproduce the observations, despite testing various
parameter sets. Furthermore, the H.E.S.S. data were used to derive
constraints on Lorentz invariance violation given the large redshift
of <ASTROBJ>3C 279</ASTROBJ>.
---------------------------------------------------------
Title: Upper limits on very-high-energy gamma-ray emission from
core-collapse supernovae observed with H.E.S.S.
Authors: H. E. S. S. Collaboration; Abdalla, H.; Aharonian, F.;
Ait Benkhali, F.; Angüner, E. O.; Arakawa, M.; Arcaro, C.; Armand,
C.; Ashkar, H.; Backes, M.; Barbosa Martins, V.; Barnard, M.;
Becherini, Y.; Berge, D.; Bernlöhr, K.; Blackwell, R.; Böttcher,
M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bregeon, J.; Breuhaus,
M.; Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.; Bylund,
T.; Capasso, M.; Caroff, S.; Carosi, A.; Casanova, S.; Cerruti, M.;
Chakraborty, N.; Chand, T.; Chandra, S.; Chaves, R. C. G.; Chen, A.;
Colafrancesco, S.; Curylo, M.; Davids, I. D.; Deil, C.; Devin, J.;
de Wilt, P.; Dirson, L.; Djannati-Ataï, A.; Dmytriiev, A.; Donath,
A.; Doroshenko, V.; Drury, L. O. 'C.; Dyks, J.; Egberts, K.; Emery,
G.; Ernenwein, J. -P.; Eschbach, S.; Feijen, K.; Fegan, S.; Fiasson,
A.; Fontaine, G.; Funk, S.; Füßling, M.; Gabici, S.; Gallant,
Y. A.; Gaté, F.; Giavitto, G.; Glawion, D.; Glicenstein, J. F.;
Gottschall, D.; Grondin, M. -H.; Hahn, J.; Haupt, M.; Heinzelmann,
G.; Henri, G.; Hermann, G.; Hinton, J. A.; Hofmann, W.; Hoischen, C.;
Holch, T. L.; Holler, M.; Horns, D.; Huber, D.; Iwasaki, H.; Jamrozy,
M.; Jankowsky, D.; Jankowsky, F.; Jung-Richardt, I.; Kastendieck,
M. A.; Katarzyński, K.; Katsuragawa, M.; Katz, U.; Khangulyan,
D.; Khélifi, B.; King, J.; Klepser, S.; Kluźniak, W.; Komin,
Nu.; Kosack, K.; Kostunin, D.; Kraus, M.; Lamanna, G.; Lau, J.;
Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leser, E.; Levy,
C.; Lohse, T.; López-Coto, R.; Lypova, I.; Mackey, J.; Majumdar, J.;
Malyshev, D.; Marandon, V.; Marcowith, A.; Mares, A.; Mariaud, C.;
Martí-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Mitchell,
A. M. W.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Muller, J.; Moore,
C.; Moulin, E.; Murach, T.; Nakashima, S.; de Naurois, M.; Ndiyavala,
H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; O'Brien, P.; Odaka,
H.; Ohm, S.; de Ona Wilhelmi, E.; Ostrowski, M.; Oya, I.; Panter, M.;
Parsons, R. D.; Perennes, C.; Petrucci, P. -O.; Peyaud, B.; Piel, Q.;
Pita, S.; Poireau, V.; Priyana Noel, A.; Prokhorov, D. A.; Prokoph,
H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Rauth, R.;
Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Rieger, F.; Rinchiuso,
L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.; Sahakian, V.;
Saito, S.; Sanchez, D. A.; Santangelo, A.; Sasaki, M.; Schlickeiser,
R.; Schüssler, F.; Schulz, A.; Schutte, H.; Schwanke, U.; Schwemmer,
S.; Seglar-Arroyo, M.; Senniappan, M.; Seyffert, A. S.; Shafi, N.;
Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol, H.; Specovius, A.;
Spir-Jacob, M.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Steppa, C.;
Takahashi, T.; Tavernier, T.; Taylor, A. M.; Terrier, R.; Tiziani,
D.; Tluczykont, M.; Trichard, C.; Tsirou, M.; Tsuji, N.; Tuffs, R.;
Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.; van Rensburg, C.;
van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.;
Vink, J.; Voisin, F.; Völk, H. J.; Vuillaume, T.; Wadiasingh, Z.;
Wagner, S. J.; White, R.; Wierzcholska, A.; Yang, R.; Yoneda, H.;
Zacharias, M.; Zanin, R.; Zdziarski, A. A.; Zech, A.; Ziegler, A.;
Zorn, J.; Żywucka, N.; Maxted, N. I.
2019A&A...626A..57H Altcode: 2019arXiv190410526H
Young core-collapse supernovae with dense-wind progenitors may be able
to accelerate cosmic-ray hadrons beyond the knee of the cosmic-ray
spectrum, and this may result in measurable gamma-ray emission. We
searched for gamma-ray emission from ten supernovae observed with
the High Energy Stereoscopic System (H.E.S.S.) within a year of
the supernova event. Nine supernovae were observed serendipitously
in the H.E.S.S. data collected between December 2003 and December
2014, with exposure times ranging from 1.4 to 53 h. In addition we
observed SN 2016adj as a target of opportunity in February 2016 for 13
h. No significant gamma-ray emission has been detected for any of the
objects, and upper limits on the >1 TeV gamma-ray flux of the order
of 10<SUP>-13</SUP> cm<SUP>-2</SUP>s<SUP>-1</SUP> are established,
corresponding to upper limits on the luminosities in the range 2 ×
10<SUP>39</SUP> to 1 × 10<SUP>42</SUP> erg s<SUP>-1</SUP>. These
values are used to place model-dependent constraints on the mass-loss
rates of the progenitor stars, implying upper limits between 2 ×
10<SUP>-5</SUP> and 2 × 10<SUP>-3</SUP> M<SUB>⊙</SUB> yr<SUP>-1</SUP>
under reasonable assumptions on the particle acceleration parameters.
---------------------------------------------------------
Title: VizieR Online Data Catalog: HESS and Suzaku observations of
Vela X (HESS Coll+, 2019)
Authors: H. E. S. S. Collaboration; Abdalla, H.; Aharonian, F.;
Ait Benkhali, F.; Anguener, E. O.; Arakawa, M.; Arcaro, C.; Armand,
C.; Backes, M.; Barnard, M.; Becherini, Y.; Berge, D.; Bernloehr, K.;
Blackwell, R.; Boettcher, M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.;
Bregeon, J.; Brun, F.; Brun, P.; Bryan, M.; Buechele, M.; Bulik, T.;
Bylund, T.; Capasso, M.; Caro, S.; Carosi, A.; Casanova, S.; Cerruti,
M.; Chakraborty, N.; Chand, T.; Chandra, S.; Chaves, R. C. G.; Chen,
A.; Colafrancesco, S.; Condon, B.; Davids, I. D.; Deil, C.; Devin,
J.; Dewilt, P.; Dirson, L.; Djannati-Atai, A.; Dmytriiev, A.; Donath,
A.; Doroshenko, V.; Drury, L. O'c.; Dyks, J.; Egberts, K.; Emery, G.;
Ernenwein, J. -P.; Eschbach, S.; Feijen, K.; Fegan, S.; Fiasson, A.;
Fontaine, G.; Funk, S.; Fuessling, M.; Gabici, S.; Gallant, Y. A.;
Gate, F.; Giavitto, G.; Glawion, D.; Glicenstein, J. F.; Gottschall,
D.; Grondin, M. -H.; Hahn, J.; Haupt, M.; Heinzelmann, G.; Henri, G.;
Hermann, G.; Hinton, J. A.; Hofmann, W.; Hoischen, C.; Holch, T. L.;
Holler, M.; Horns, D.; Huber, D.; Iwasaki, H.; Jacholkowska, Y. A.;
Jamrozy, M.; Jankowsky, D.; Jankowsky, F.; Jouvin, L.; Jung-Richardt,
I.; Kastendieck, M. A.; Katarzy'nski, K.; Katsuragawa, M.; Katz, U.;
Khangulyan, D.; Khelifi, B.; King, J.; Klepser, S.; Klu'Zniak, W.;
Komin, Nu.; Kosack, K.; Kostunin, D.; Kraus, M.; Lamanna, G.; Lau, J.;
Lemiere, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leser, E.; Lohse,
T.; Lopez-Coto, R.; Lypova, I.; Malyshev, D.; Marandon, V.; Marcowith,
A.; Mariaud, C.; Marti-Devesa, G.; Marx, R.; Maurin, G.; Maxted,
N. I.; Meintjes, P. J.; Mitchell, A. M. W.; Moderski, R.; Mohamed,
M.; Mohrmann, L.; Moore, C.; Moulin, E.; Murach, T.; Nakashima, S.;
de Naurois, M.; Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes,
L.; O'Brien, P.; Odaka, H.; Ohm, S.; de Ona Wilhelmi, E.; Ostrowski,
M.; Oya, I.; Panter, M.; Parsons, R. D.; Perennes, C.; Petrucci,
P. -O.; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V.; Priyana, Noel A.;
Prokhorov, D. A.; Prokoph, H.; Puehlhofer, G.; Punch, M.; Quirrenbach,
A.; Raab, S.; Rauth, R.; Reimer, A.; Reimer, O.; Renaud, M.; Rieger,
F.; Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.;
Sahakian, V.; Saito, S.; Sanchez, D. A.; Santangelo, A.; Sasaki, M.;
Schlickeiser, R.; Schuessler, F.; Schulz, A.; Schutte, H.; Schwanke,
U.; Schwemmer, S.; Seglar-Arroyo, M.; Senniappan, M.; Seyert, A. S.;
Shafi, N.; Shilon, I.; Shiningayamwe, K.; Simoni, R.; Sinha, A.;
Sol, H.; Specovius, A.; Spir-Jacob, M.; Stawarz, L.; Steenkamp,
R.; Stegmann, C.; Steppa, C.; Takahashi, T.; Tavernet, J. -P.;
Tavernier, T.; Taylor, A. M.; Terrier, R.; Tibaldo, L.; Tiziani,
D.; Tluczykont, M.; Trichard, C.; Tsirou, M.; Tsuji, N.; Tus, R.;
Uchiyama, Y.; van der, Walt D. J.; van Eldik, C.; van Rensburg, C.;
van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.;
Vink, J.; Voisin, F.; Voelk, H. J.; Vuillaume, T.; Wadiasingh, Z.;
Wagner, S. J.; White, R.; Wierzcholska, A.; Yang, R.; Yoneda, H.;
Zaborov, D.; Zacharias, M.; Zanin, R.; Zdziarski, A. A.; Zech, A.;
Ziegler, A.; Zorn, J.; Zywucka, N.
2019yCat..36270100H Altcode:
Spectra from H.E.S.S. and Suzaku XIS observations of three regions in
the Vela X cocoon referred to in the paper as pointing 0 (p0), pointing
1 (p1), and pointing (p2). Errors combine statistical and systematic
uncertainties of instrumental origin and from the analysis method. <P
/>HESS spectra contain Centre of energy bin (energy, eV), Lower width
of energy bin (energy<SUB>error</SUB>lo, eV), Higher width of energy
bin (energy<SUB>error</SUB>hi, eV), Flux (flux, 1/cm2/TeV), Lower
flux error (flux<SUB>error</SUB>lo, 1/cm2/TeV) and Higher flux error
(flux<SUB>error</SUB>hi, 1/cm2/TeV) <P />Suzaku XIS spectra contain
Centre of energy bin (energy, eV), Width of energy bin (energy_error,
eV), Flux (flux, 1/cm2/TeV), and Flux error (flux_error, 1/cm2/TeV)
<P />(2 data files).
---------------------------------------------------------
Title: Particle transport within the pulsar wind nebula HESS J1825-137
Authors: H. E. S. S. Collaboration; Abdalla, H.; Aharonian, F.; Ait
Benkhali, F.; Angüner, E. O.; Arakawa, M.; Arcaro, C.; Armand, C.;
Arrieta, M.; Backes, M.; Barnard, M.; Becherini, Y.; Becker Tjus, J.;
Berge, D.; Bernlöhr, K.; Blackwell, R.; Böttcher, M.; Boisson, C.;
Bolmont, J.; Bonnefoy, S.; Bordas, P.; Bregeon, J.; Brun, F.; Brun,
P.; Bryan, M.; Büchele, M.; Bulik, T.; Bylund, T.; Capasso, M.;
Caroff, S.; Carosi, A.; Casanova, S.; Cerruti, M.; Chakraborty, N.;
Chand, T.; Chandra, S.; Chaves, R. C. G.; Chen, A.; Colafrancesco, S.;
Condon, B.; Davids, I. D.; Deil, C.; Devin, J.; deWilt, P.; Dirson,
L.; Djannati-Ataï, A.; Dmytriiev, A.; Donath, A.; Doroshenko,
V.; Drury, L. O. 'C.; Dyks, J.; Egberts, K.; Emery, G.; Ernenwein,
J. -P.; Eschbach, S.; Fegan, S.; Fiasson, A.; Fontaine, G.; Funk,
S.; Füßling, M.; Gabici, S.; Gallant, Y. A.; Gaté, F.; Giavitto,
G.; Glawion, D.; Glicenstein, J. F.; Gottschall, D.; Grondin, M. -H.;
Hahn, J.; Haupt, M.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton,
J. A.; Hofmann, W.; Hoischen, C.; Holch, T. L.; Holler, M.; Horns, D.;
Huber, D.; Iwasaki, H.; Jacholkowska, A.; Jamrozy, M.; Jankowsky,
D.; Jankowsky, F.; Jouvin, L.; Jung-Richardt, I.; Kastendieck,
M. A.; Katarzyński, K.; Katsuragawa, M.; Katz, U.; Kerszberg, D.;
Khangulyan, D.; Khélifi, B.; King, J.; Klepser, S.; Kluźniak, W.;
Komin, Nu.; Kosack, K.; Kraus, M.; Lamanna, G.; Lau, J.; Lefaucheur,
J.; Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leser, E.;
Lohse, T.; López-Coto, R.; Lypova, I.; Malyshev, D.; Marandon, V.;
Marcowith, A.; Mariaud, C.; Martí-Devesa, G.; Marx, R.; Maurin,
G.; Meintjes, P. J.; Mitchell, A. M. W.; Moderski, R.; Mohamed, M.;
Mohrmann, L.; Moore, C.; Moulin, E.; Murach, T.; Nakashima, S.; de
Naurois, M.; Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes, L.;
O'Brien, P.; Odaka, H.; Ohm, S.; Ostrowski, M.; Oya, I.; Panter, M.;
Parsons, R. D.; Perennes, C.; Petrucci, P. -O.; Peyaud, B.; Piel, Q.;
Pita, S.; Poireau, V.; Priyana Noel, A.; Prokhorov, D. A.; Prokoph,
H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Rauth, R.;
Reimer, A.; Reimer, O.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli,
C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.; Sahakian, V.; Saito,
S.; Sanchez, D. A.; Santangelo, A.; Sasaki, M.; Schlickeiser, R.;
Schüssler, F.; Schulz, A.; Schutte, H.; Schwanke, U.; Schwemmer, S.;
Seglar-Arroyo, M.; Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shilon,
I.; Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol, H.; Specovius, A.;
Spir-Jacob, M.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Steppa,
C.; Takahashi, T.; Tavernet, J. -P.; Tavernier, T.; Taylor, A. M.;
Terrier, R.; Tibaldo, L.; Tiziani, D.; Tluczykont, M.; Trichard, C.;
Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, D. J.;
van Eldik, C.; van Rensburg, C.; van Soelen, B.; Vasileiadis, G.;
Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Voisin, F.; Völk, H. J.;
Vuillaume, T.; Wadiasingh, Z.; Wagner, S. J.; Wagner, R. M.; White,
R.; Wierzcholska, A.; Yang, R.; Yoneda, H.; Zaborov, D.; Zacharias,
M.; Zanin, R.; Zdziarski, A. A.; Zech, A.; Zefi, F.; Ziegler, A.;
Zorn, J.; Żywucka, N.
2019A&A...621A.116H Altcode: 2018arXiv181012676H
Context. We present a detailed view of the pulsar wind nebula (PWN)
HESS J1825-137. We aim to constrain the mechanisms dominating the
particle transport within the nebula, accounting for its anomalously
large size and spectral characteristics. <BR /> Aims: The nebula
was studied using a deep exposure from over 12 years of H.E.S.S. I
operation, together with data from H.E.S.S. II that improve the
low-energy sensitivity. Enhanced energy-dependent morphological and
spatially resolved spectral analyses probe the very high energy
(VHE, E > 0.1 TeV) γ-ray properties of the nebula. <BR />
Methods: The nebula emission is revealed to extend out to 1.5°
from the pulsar, 1.5 times farther than previously seen, making
HESS J1825-137, with an intrinsic diameter of 100 pc, potentially
the largest γ-ray PWN currently known. Characterising the strongly
energy-dependent morphology of the nebula enables us to constrain the
particle transport mechanisms. A dependence of the nebula extent with
energy of R ∝ E<SUP>α</SUP> with α = -0.29 ± 0.04<SUB>stat</SUB>
± 0.05<SUB>sys</SUB> disfavours a pure diffusion scenario for
particle transport within the nebula. The total γ-ray flux of the
nebula above 1 TeV is found to be (1.12 ± 0.03<SUB>stat</SUB> ±
0.25<SUB>sys</SUB>) × 10<SUP>-11</SUP> cm<SUP>-2</SUP> s<SUP>-1</SUP>,
corresponding to 64% of the flux of the Crab nebula. <BR /> Results:
HESS J1825-137 is a PWN with clearly energy-dependent morphology
at VHE γ-ray energies. This source is used as a laboratory to
investigate particle transport within intermediate-age PWNe. Based
on deep observations of this highly spatially extended PWN, we
produce a spectral map of the region that provides insights into the
spectral variation within the nebula. <P />Sky maps as FITS files
and spectra are only available at the CDS via anonymous ftp to <A
href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
(ftp://130.79.128.5) or via <A
href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/621/A116">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/621/A116</A>
---------------------------------------------------------
Title: CESM-release-cesm2.1.0
Authors: Danabasoglu; Lamarque; Bacmeister; Bailey; DuVivier;
Edwards; Emmons; Fasullo; Garcia; Gettelman; Hannay; Holland; Large;
Lauritzen; Lawrence; Lenaerts; Lindsay; Lipscomb; Mills; Neale; Oleson;
Otto-Bliesner; Phillips; Sacks; Tilmes; Kampenhout, Van; Vertenstein;
Bertini; Dennis; Deser; Fischer; Fox-Kemper; Kay; Kinnison; Kushner;
Larson; Long; Mickelson; Moore; Nienhouse; Polvani; Rasch; Strand
2018zndo...3895306D Altcode:
The Community Earth System Model release version 2.1.0
---------------------------------------------------------
Title: VizieR Online Data Catalog: HESS J1825-137 particle transport
(H.E.S.S. Collaboration, 2019)
Authors: H. E. S. S. Collaboration; Abdalla, H.; Aharonian, F.; Ait
Benkhali, F.; Anguener, E. O.; Arakawa, M.; Arcaro, C.; Armand, C.;
Arrieta, M.; Backes, M.; Barnard, M.; Becherini, Y.; Becker Tjus, J.;
Berge, D.; Bernloehr, K.; Blackwell, R.; Boettcher, M.; Boisson, C.;
Bolmont, J.; Bonnefoy, S.; Bordas, P.; Bregeon, J.; Brun, F.; Brun,
P.; Bryan, M.; Buechele, M.; Bulik, T.; Bylund, T.; Capasso, M.;
Caroff, S.; Carosi, A.; Casanova, S.; Cerruti, M.; Chakraborty, N.;
Chand, T.; Chandra, S.; Chaves, R. C. G.; Chen, A.; Colafrancesco,
S.; Condon, B.; Davids, I. D.; Deil, C.; Devin, J.; Dewilt, P.;
Dirson, L.; Djannati-Atai, A.; Dmytriiev, A.; Donath, A.; Doroshenko,
V.; Drury, L. O'c.; Dyks, J.; Egberts, K.; Emery, G.; Ernenwein,
J. -P.; Eschbach, S.; Fegan, S.; Fiasson, A.; Fontaine, G.; Funk,
S.; Fuessling, M.; Gabici, S.; Gallant, Y. A.; Gate, F.; Giavitto,
G.; Glawion, D.; Glicenstein, J. F.; Gottschall, D.; Grondin, M. -H.;
Hahn, J.; Haupt, M.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton,
J. A.; Hofmann, W.; Hoischen, C.; Holch, T. L.; Holler, M.; Horns, D.;
Huber, D.; Iwasaki, H.; Jacholkowska, A.; Jamrozy, M.; Jankowsky,
D.; Jankowsky, F.; Jouvin, L.; Jung-Richardt, I.; Kastendieck,
M. A.; Katarzynski, K.; Katsuragawa, M.; Katz, U.; Kerszberg, D.;
Khangulyan, D.; Khelifi, B.; King, J.; Klepser, S.; Kluzniak, W.;
Komin, Nu.; Kosack, K.; Kraus, M.; Lamanna, G.; Lau, J.; Lefaucheur,
J.; Lemiere, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leser, E.;
Lohse, T.; Lopez-Coto, R.; Lypova, I.; Malyshev, D.; Marandon, V.;
Marcowith, A.; Mariaud, C.; Marti-Devesa, G.; Marx, R.; Maurin,
G.; Meintjes, P. J.; Mitchell, A. M. W.; Moderski, R.; Mohamed, M.;
Mohrmann, L.; Moore, C.; Moulin, E.; Murach, T.; Nakashima, S.; de
Naurois, M.; Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes, L.;
O'Brien, P.; Odaka, H.; Ohm, S.; Ostrowski, M.; Oya, I.; Panter, M.;
Parsons, R. D.; Perennes, C.; Petrucci, P. -O.; Peyaud, B.; Piel, Q.;
Pita, S.; Poireau, V.; Priyana, Noel A.; Prokhorov, D. A.; Prokoph,
H.; Puehlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Rauth, R.;
Reimer, A.; Reimer, O.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli,
C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.; Sahakian, V.; Saito,
S.; Sanchez, D. A.; Santangelo, A.; Sasaki, M.; Schlickeiser, R.;
Schuessler, F.; Schulz, A.; Schutte, H.; Schwanke, U.; Schwemmer, S.;
Seglar-Arroyo, M.; Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shilon,
I.; Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol, H.; Specovius, A.;
Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, C.; Steppa,
C.; Takahashi, T.; Tavernet, J. -P.; Tavernier, T.; Taylor, A. M.;
Terrier, R.; Tibaldo, L.; Tiziani, D.; Tluczykont, M.; Trichard, C.;
Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der, Walt D. J.;
van Eldik, C.; van Rensburg, C.; van Soelen, B.; Vasileiadis, G.;
Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Voisin, F.; Voelk, H. J.;
Vuillaume, T.; Wadiasingh, Z.; Wagner, S. J.; Wagner, R. M.; White,
R.; Wierzcholska, A.; Yang, R.; Yoneda, H.; Zaborov, D.; Zacharias,
M.; Zanin, R.; Zdziarski, A. A.; Zech, A.; Zefi, F.; Ziegler, A.;
Zorn, J.; Zywucka, N.
2018yCat..36210116H Altcode:
FITS files with sky maps corresponding to figures 1 and 3 in the
paper. Spectral points corresponding to figures 2 and 10, as well as
spectral fit information corresponding to table 5 in the paper. <P
/>(7 data files).
---------------------------------------------------------
Title: Probing the gravitational redshift with an Earth-orbiting
satellite
Authors: Litvinov, D. A.; Rudenko, V. N.; Alakoz, A. V.; Bach,
U.; Bartel, N.; Belonenko, A. V.; Belousov, K. G.; Bietenholz, M.;
Biriukov, A. V.; Carman, R.; Cimó, G.; Courde, C.; Dirkx, D.; Duev,
D. A.; Filetkin, A. I.; Granato, G.; Gurvits, L. I.; Gusev, A. V.;
Haas, R.; Herold, G.; Kahlon, A.; Kanevsky, B. Z.; Kauts, V. L.;
Kopelyansky, G. D.; Kovalenko, A. V.; Kronschnabl, G.; Kulagin,
V. V.; Kutkin, A. M.; Lindqvist, M.; Lovell, J. E. J.; Mariey, H.;
McCallum, J.; Molera Calvés, G.; Moore, C.; Moore, K.; Neidhardt, A.;
Plötz, C.; Pogrebenko, S. V.; Pollard, A.; Porayko, N. K.; Quick,
J.; Smirnov, A. I.; Sokolovsky, K. V.; Stepanyants, V. A.; Torre,
J. -M.; de Vicente, P.; Yang, J.; Zakhvatkin, M. V.
2018PhLA..382.2192L Altcode: 2017arXiv171010074L
We present an approach to testing the gravitational redshift
effect using the RadioAstron satellite. The experiment is based
on a modification of the Gravity Probe A scheme of nonrelativistic
Doppler compensation and benefits from the highly eccentric orbit
and ultra-stable atomic hydrogen maser frequency standard of the
RadioAstron satellite. Using the presented techniques we expect
to reach an accuracy of the gravitational redshift test of order
10<SUP>-5</SUP>, a magnitude better than that of Gravity Probe A. Data
processing is ongoing, our preliminary results agree with the validity
of the Einstein Equivalence Principle.
---------------------------------------------------------
Title: The Vertical Dust Profile over Gale Crater
Authors: Guzewich, S.; Newman, C. E.; Smith, M. D.; Moores, J.; Smith,
C. L.; Moore, C.; Richardson, M. I.; Kass, D. M.; Kleinboehl, A.;
Martin-Torres, F. J.; Zorzano, M. P.; Battalio, J. M.
2017AGUFM.P23D2758G Altcode:
Regular joint observations of the atmosphere over Gale Crater from
the orbiting Mars Reconnaissance Orbiter/Mars Climate Sounder (MCS)
and Mars Science Laboratory (MSL) Curiosity rover allow us to create
a coarse, but complete, vertical profile of dust mixing ratio from
the surface to the upper atmosphere. We split the atmospheric column
into three regions: the planetary boundary layer (PBL) within Gale
Crater that is directly sampled by MSL (typically extending from the
surface to 2-6 km in height), the region of atmosphere sampled by MCS
profiles (typically 25-80 km above the surface), and the region of
atmosphere between these two layers. Using atmospheric optical depth
measurements from the Rover Environmental Monitoring System (REMS)
ultraviolet photodiodes (in conjunction with MSL Mast Camera solar
imaging), line-of-sight opacity measurements with the MSL Navigation
Cameras (NavCam), and an estimate of the PBL depth from the MarsWRF
general circulation model, we can directly calculate the dust mixing
ratio within the Gale Crater PBL and then solve for the dust mixing
ratio in the middle layer above Gale Crater but below the atmosphere
sampled by MCS. Each atmospheric layer has a unique seasonal cycle
of dust opacity, with Gale Crater's PBL reaching a maximum in dust
mixing ratio near Ls = 270° and a minimum near Ls = 90°. The layer
above Gale Crater, however, has a seasonal cycle that closely follows
the global opacity cycle and reaches a maximum near Ls = 240° and
exhibits a local minimum (associated with the "solsticial pauses")
near Ls = 270°. Knowing the complete vertical profile also allows us
to determine the frequency of high-altitude dust layers above Gale,
and whether such layers truly exhibit the maximum dust mixing ratio
within the entire vertical column. We find that 20% of MCS profiles
contain an "absolute" high-altitude dust layer, i.e., one in which the
dust mixing ratio within the high-altitude dust layer is the maximum
dust mixing ratio in the vertical column of atmosphere over Gale Crater.
---------------------------------------------------------
Title: The Vertical Dust Profile Over Gale Crater, Mars
Authors: Guzewich, Scott D.; Newman, C. E.; Smith, M. D.; Moores,
J. E.; Smith, C. L.; Moore, C.; Richardson, M. I.; Kass, D.;
Kleinböhl, A.; Mischna, M.; Martín-Torres, F. J.; Zorzano-Mier,
M. -P.; Battalio, M.
2017JGRE..122.2779G Altcode:
We create a vertically coarse, but complete, profile of dust mixing
ratio from the surface to the upper atmosphere over Gale Crater, Mars,
using the frequent joint atmospheric observations of the orbiting
Mars Climate Sounder (MCS) and the Mars Science Laboratory Curiosity
rover. Using these data and an estimate of planetary boundary layer
(PBL) depth from the MarsWRF general circulation model, we divide the
vertical column into three regions. The first region is the Gale Crater
PBL, the second is the MCS-sampled region, and the third is between
these first two. We solve for a well-mixed dust mixing ratio within
this third (middle) layer of atmosphere to complete the profile. We
identify a unique seasonal cycle of dust within each atmospheric
layer. Within the Gale PBL, dust mixing ratio maximizes near southern
hemisphere summer solstice (L<SUB>s</SUB> = 270°) and minimizes near
winter solstice (L<SUB>s</SUB> = 90-100°) with a smooth sinusoidal
transition between them. However, the layer above Gale Crater and below
the MCS-sampled region more closely follows the global opacity cycle
and has a maximum in opacity near L<SUB>s</SUB> = 240° and exhibits
a local minimum (associated with the "solsticial pause" in dust storm
activity) near L<SUB>s</SUB> = 270°. With knowledge of the complete
vertical dust profile, we can also assess the frequency of high-altitude
dust layers over Gale. We determine that 36% of MCS profiles near Gale
Crater contain an "absolute" high-altitude dust layer wherein the dust
mixing ratio is the maximum in the entire vertical column.
---------------------------------------------------------
Title: New Solar Soft X-Ray (SXR) Spectral Irradiance Measurements
Bridge the SDO and RHESSI Spectral Gap to Study Flare Energetics
Authors: Woods, T. N.; Jones, A.; Mason, J.; Moore, C.; Eparvier,
F.; Caspi, A.; Chamberlin, P.
2016usc..confE..14W Altcode:
The extreme ultraviolet (EUV) spectrum is rich in many different
emission lines that reveal plasma characteristics concerning
active region evolution and explosive energy release during coronal
eruptions. Solar EUV imagers, such as SDO AIA, provide insight into the
location, thermal structure, and dynamics of the coronal eruptions and
associated flares. In addition, the solar EUV spectral irradiance from
SDO EVE, with its higher spectral resolution, provides more detailed
thermal evolution of the eruption and has better characterized some
aspects of the eruptions such as relationship of coronal dimming and
mass loss and post-eruption coronal loop cooling. Complementary to
SDO are hard x-ray (HXR) measurements by RHESSI that have clarified
the initiation of energy release from magnetic reconnection in
the corona. New solar soft x-ray (SXR) spectral irradiance from the
Miniature X-ray Solar Spectrometer (MinXSS) CubeSat is now bridging this
spectral gap between SDO EUV and RHESSI HXR observations. MinXSS-1 was
deployed from the ISS in May 2016 for a 1-year mission, and MinXSS-2 is
being launched in October 2016 for a 5-year mission. The energy release
during solar flares is expected to peak in the SXR and thus the SXR has
been monitored with GOES broadband photometers for decades, but there
has been very limited SXR spectral measurements. With the new and unique
MinXSS measurements of the SXR spectral variability during flares,
coupled with solar SXR images from Hinode, EUV data from SDO, and HXR
data from RHESSI, the processes for releasing energy during an eruption
and affecting post-eruption thermal evolution can be explored in more
detail. Furthermore, the new SXR spectral irradiance measurements can
help improve the accuracy of broad band SXR measurements by GOES XRS,
SDO EVE ESP, and XPS aboard TIMED and SORCE. Such improvements can
lead to better understanding the solar impacts in Earth's ionosphere
and thermosphere and how they might affect some of our space-based
communication and navigation systems. This presentation will focus
on how these new solar SXR spectral measurements can enhance the SDO
studies of eruptive flares.
---------------------------------------------------------
Title: Establishment of Laser Link Between Ground Station and
Hayabusa2 LIDAR
Authors: Noda, H.; Mizuno, T.; Kunimori, H.; Takeuchi, H.; Senshu,
H.; Ogawa, N.; Saiki, T.; Yamaguchi, T.; Pollard, A.; Moore, C.;
Namiki, N.; Tsuda, Y.
2016LPI....47.1289N Altcode:
Laser link experiment between ground SLR stations and a laser altimeter
named LIDAR on Hayabusa2 was carried out, and the uplink laser pulses
were detected.
---------------------------------------------------------
Title: Optical Survey of the Tumble Rates of Retired GEO Satellites
Authors: Binz, C.; Davis, M.; Kelm, B.; Moore, C.
2014amos.confE..61B Altcode:
The Naval Research Lab (NRL) and the Defense Advanced Research Projects
Agency (DARPA) have made significant progress toward robotic rendezvous
and docking between spacecraft, however the long-term attitude
motion evolution of uncontrolled resident space objects has never been
well-characterized. This effort set out to identify the motion exhibited
in retired satellites at or near geosynchronous orbit (GEO). Through
analysis of the periodic structure of observed reflected light curves,
estimated tumble rates were determined for several retired satellites,
typically in a super-GEO disposal orbit. The NRL's 1-meter telescope at
Midway Research Center was used to track and observe the objects while
the sun-satellite-observer geometry was most favorable; typically over
a one- to two-hour period, repeated multiple times over the course
of weeks. By processing each image with calibration exposures, the
relative apparent magnitude of the brightness of the object over time
was determined. Several tools, including software developed internally,
were used for frequency analysis of the brightness curves. Results show
that observed satellites generally exhibit a tumble rate well below
the notional bounding case of one degree per second. When harmonics
are found to exist in the data, modeling and simulation of the optical
characteristics of the satellite can help to resolve ambiguities. This
process was validated on spacecraft for which an attitude history is
known, and agreement was found.
---------------------------------------------------------
Title: The World's Strangest Supernova May Not Be a Supernova At All
Authors: Moore, C.
2012JAVSO..40..421M Altcode:
(Abstract only) SN 2008ha is the least luminous supernova ever to be
observed. It is unclear what caused this obscurity to occur. For the
last three years I have been doing independent follow-up research
on SN 2008ha. SN 2008ha is believed to be 100 times brighter than
a nova, but 1,000 times dimmer then a supernova. The spectrum to
some degree was classic Type Ia supernova because of the lack of
hydrogen and abundance of silicon, but there are many other factors
to be considered. SN 2008ha had a short rise time of only 10 days
(typical Type Ia is 19.5 days). It has low expansion velocities of
only 2,000km compared to the typical Ia with very small kinetic energy
per unit mass of ejecta. Although some elements of the spectrum are
consistent with those of a Type Ia, narrow lines were observed. This
is just one of several characteristics that SN 2008ha shares with the
"SN 2002cx-like class" of supernovae. SN 2008ha is believed to be the
most extreme of this sub-class of supernovae with the smallest amount
of space between lines, 5 days shorter rise time, being significantly
fainter, and having lower velocities. With all these things considered,
it does make classification as a Type Ia questionable. In fact it
is even questionable if this is a supernova at all, and not just an
"imposter." This may have just been a "star burp" which means that
the supernova may have failed, resulting in some parts of the star
being left, maybe even enough remains to explode again as seen in the
case of SN 2006jc. This may have occurred because the explosion was
not deep enough in the core of the star, and only eliminating some
or all of the hydrogen envelope and leaving behind the carbon and
oxygen inner layers, instead resulting in a Type Ic supernova. It
would be interesting to see what, if anything is left of the star;
this could make it a possible Hubble candidate. The idea that it may
"burp" again makes it especially important.
---------------------------------------------------------
Title: Cavity ring-down spectroscopy (CRDS) system for measuring
atmospheric mercury using differential absorption
Authors: Pierce, A.; Obrist, D.; Moosmuller, H.; Moore, C.
2012EGUGA..1411454P Altcode:
Atmospheric elemental mercury (Hg0) is a globally pervasive element
that can be transported and deposited to remote ecosystems where
it poses — particularly in its methylated form — harm to many
organisms including humans. Current techniques for measurement
of atmospheric Hg0 require several liters of sample air and
several minutes for each analysis. Fast-response (i.e., 1 second
or faster) measurements would improve our ability to understand
and track chemical cycling of mercury in the atmosphere, including
high frequency Hg0 fluctuations, sources and sinks, and chemical
transformation processes. We present theory, design, challenges,
and current results of our new prototype sensor based on cavity
ring-down spectroscopy (CRDS) for fast-response measurement of Hg0 mass
concentrations. CRDS is a direct absorption technique that implements
path-lengths of multiple kilometers in a compact absorption cell using
high-reflectivity mirrors, thereby improving sensitivity and reducing
sample volume compared to conventional absorption spectroscopy. Our
sensor includes a frequency-doubled, dye-laser emitting laser pulses
tunable from 215 to 280 nm, pumped by a Q-switched, frequency tripled
Nd:YAG laser with a pulse repetition rate of 50 Hz. We present how we
successfully perform automated wavelength locking and stabilization
of the laser to the peak Hg0 absorption line at 253.65 nm using an
external isotopically-enriched mercury (202Hg0) cell. An emphasis
of this presentation will be on the implementation of differential
absorption measurement whereby measurements are alternated between
the peak Hg0 absorption wavelength and a nearby wavelength "off" the
absorption line. This can be achieved using a piezo electric tuning
element that allows for pulse-by-pulse tuning and detuning of the laser
"online" and "offline" of the Hg absorption line, and thereby allows
for continuous correction of baseline extinction losses. Unexpected
challenges with this approach included different efficiencies of laser
performance (e.g., frequency doubling) at the two wavelengths and
temperature dependence. We will discuss improvements on the control
of our system to eliminate drift due to conversion efficiency and
temperature dependence. We will detail complications with operating
this instrument from a mobile platform for in situ measurements in
the field. Finally, we will present data acquisition and processing
approaches along with results of calibration curves, and comparisons
to conventional mercury analyzers (i.e., a Tekran 2537 mercury vapor
analyzer) during ambient air measurements.
---------------------------------------------------------
Title: Bromine-induced Atmospheric Mercury Depletion Events (AMDEs)
at the Dead Sea: magnitude, frequency, spatial extent, and modeled
reaction pathways
Authors: Tas, E.; Obrist, D.; Moore, C.; Peleg, M.; Luria, M.
2012EGUGA..1412475T Altcode:
Bromine-induced Atmospheric Mercury Depletion Events (AMDEs) at the Dead
Sea: magnitude, frequency, spatial extent, and modeled reaction pathways
---------------------------------------------------------
Title: NESSI: the New Mexico Tech Extrasolar Spectroscopic Survey
Instrument
Authors: Jurgenson, C.; Santoro, F.; Creech-Eakman, M.; Houairi, K.;
Bloemhard, H.; Vasisht, G.; Swain, M.; Deroo, P.; Moore, C.; Schmidt,
L.; Boston, P.; Rodeheffer, D.; Chen, P.
2010SPIE.7735E..19J Altcode: 2010SPIE.7735E..43J
Less than 20 years after the discovery of the first extrasolar planet,
exoplanetology is rapidly growing with more than one discovery every
week on average since 2007. An important step in exoplanetology is the
chemical characterization of exoplanet atmospheres. It has recently
been shown that molecular signatures of transiting exoplanets can be
studied from the ground. To advance this idea and prepare more ambitious
missions such as THESIS, a dedicated spectrometer named the New Mexico
Tech Extrasolar Spectroscopic Survey Instrument (NESSI) is being
built at New Mexico Tech in collaboration with the NASA Jet Propulsion
Laboratory. NESSI is a purpose-built multi-object spectrograph that
operates in the J, H, and K-bands with a resolution of R = 1000 in each,
as well as a lower resolution of R = 250 across the entire J/H/K region.
---------------------------------------------------------
Title: Monte Carlo modeling of Io’s [OI] 6300 Å and [SII] 6716
Å auroral emission in eclipse
Authors: Moore, C.; Miki, K.; Goldstein, D. B.; Stapelfeldt, K.;
Varghese, P. L.; Trafton, L. M.; Evans, R. W.
2010Icar..207..810M Altcode:
We present a Monte Carlo (MC) model of [OI] 6300 Å and [SII] 6716 Å
emission from Io entering eclipse. The simulation accounts for the
3-D distribution of SO <SUB>2</SUB>, O, SO, S, and O <SUB>2</SUB>
in Io's atmosphere, several volcanic plumes, and the magnetic field
around Io. Thermal electrons from the jovian plasma torus are input
along the simulation domain boundaries and move along the magnetic
field lines distorted by Io, occasionally participating in collisions
with neutrals. We find that the atmospheric asymmetry resulting from
varying degrees of atmospheric collapse across Io (due to eclipse
ingress) and the presence of volcanoes contributes significantly to the
unique morphology of the [OI] 6300 Å emission. The [OI] radiation
lifetime of ∼134 s limits the emission to regions that have a
sufficiently low neutral density so that intermolecular collisions
are rare. We find that at low altitudes (typically <40 km) and in
volcanic plumes (Pele, Prometheus, etc.) the number density is large
enough (>4 × 10 <SUP>9</SUP> cm <SUP>-3</SUP>) to collisionally
quench nearly all (>95%) of the excited oxygen for reasonable
quenching efficiencies. Upstream (relative to the plasma flow), Io's
perturbation of the jovian magnetic field mirrors electrons with high
pitch angles, while downstream collisions can trap the electrons. This
magnetic field perturbation is one of the main physical mechanisms
that results in the upstream/downstream brightness asymmetry in
[OI] emission seen in the observation by Trauger et al. (Trauger,
J.T., Stapelfeldt, K.R., Ballester, G.E., Clarke, J.I., 1997. HST
observations of [OI] emissions from Io in eclipse. AAS-DPS Abstract
(1997DPS29.1802T)). There are two other main causes for the observed
brightness asymmetry. First, the observation's viewing geometry of
the wake spot crosses the dayside atmosphere and therefore the wake's
observational field of view includes higher oxygen column density than
the upstream side. Second, the phased entry into eclipse results in
less atmospheric collapse and thus higher collisional quenching on
the upstream side relative to the wake. We compute a location (both
in altitude and latitude) for the intense wake emission feature that
agrees reasonably well with this observation. Furthermore, the peak
intensity of the simulated wake feature is less than that observed
by a factor of ∼3, most likely because our model does not include
direct dissociation-excitation of SO <SUB>2</SUB> and SO. We find that
the latitudinal location of the emission feature depends not so much
on the tilt of the magnetic field as on the relative north/south flux
tube depletion that occurs due to Io's changing magnetic latitude in the
plasma torus. From 1-D simulations, we also find that the intensity of
[SII] 6716 and 6731 Å emission is much weaker than that of [OI] even
if the [SII] excitation cross section is 10 <SUP>3</SUP> times larger
than excitation to [OI]. This is because the density of S <SUP>+</SUP>
is much less than that of O and because the Einstein- A coefficient
of the [SII] emission is a factor of ∼10 smaller than that of [OI].
---------------------------------------------------------
Title: Supernova 2009he in UGC 10361
Authors: Puckett, T.; Moore, C.; Orff, T.
2009CBET.1868....1P Altcode: 2009CBET.1868A...1P
T. Puckett, Ellijay, GA, U.S.A.; and C. Moore, Warwick, NY, U.S.A.,
report the discovery of an apparent supernova (mag 17.5) on unfiltered
CCD images (limiting mag 18.9) taken with a 0.50-m reflector at Ellijay
on July 3.16 UT in the course of the Puckett Observatory Supernova
Search. The new object, which was confirmed at mag 17.5 on images
(limiting mag 19.5) taken by T. Orff on July 4.17 with a 0.60-m
reflector at Ellijay, is located at R.A. = 16h22m12s.33, Decl. =
+57o16'22".5 (equinox 2000.0), which is 21".8 east and 6".9 north of
the center of UGC 10361. Nothing is visible at this position on images
taken by Puckett on June 22 (limiting mag 19.4).
---------------------------------------------------------
Title: Extending Deep H-alpha Galaxy Surveys to Higher Redshift
with NEWFIRM
Authors: Lee, Janice C.; Ly, C.; Moore, C.; Salim, S.; Dale, D.;
Finn, R.; Momcheva, I.
2009AAS...21342401L Altcode: 2009BAAS...41Q.246L
H-alpha nebular emission is one of the most direct tracers of star
formation. As such, a great deal of our current understanding
of star formation in local galaxies is based on a long and rich
history of H-alpha observational studies. However, there is a dearth
of analogous work at intermediate redshifts -- a critical period in
galaxy evolution where the overall star formation activity reaches its
maximum. Here, we present first results from our on-going campaign to
extend deep, wide H-alpha galaxy surveys to earlier cosmic times by
taking advantage of the new capabilities offered by the NOAO Extremely
Wide-Field Infrared Imager (NEWFIRM) at the KPNO 4m. Our strategy is to
obtain (1%) narrowband imaging of key extragalactic fields in low-OH
airglow windows at 1.19 and 2.09 microns (H-alpha at z 0.8 and 2.2,
respectively). Our filters are coupled such that the [OII] emission of
H-alpha emitters detected at 2.09 microns will also be captured in the
1.19 micron narrowband. Continuum measurements are provided by J and
Ks-band observations. Follow-up spectroscopy is being obtained with
IMACS at the Magellan 6.5m at Las Campanas. We discuss our overall
survey design and candidate selection, examine the properties of our
narrowband excess emitters, and give an overview of the science that our
survey data will address. The H-alpha SFR limits of our 1.19 and 2.09
micron data will reach to 1 M_sun/yr and 12 M_sun/yr, respectively. A
companion poster describes preliminary results on H-alpha luminosity
functions and star formation rate densities.
---------------------------------------------------------
Title: A Comparison of UV and Hα Star Formation Rates In Intermediate
Redshift Galaxies
Authors: Walton, Josiah; Salim, S.; Lee, J.; Ly, C.; Finn, R.; Moore,
C.; Dale, D.; McCarthy, D.; Kulesa, C.; Kennefick, J.
2009AAS...21342403W Altcode: 2009BAAS...41..246W
We present results of a study which directly compares star formation
rates (SFRs) based on two commonly used indicators, the UV non-ionizing
continuum and H-alpha nebular emission, for star-forming galaxies at
z 0.8. Using UV data from the GALEX ultra-deep imaging survey in the
Extended Groth Strip (EGS), Hubble Deep Field North (HDFN), and COSMOS
fields, we construct a PSF-based UV flux catalog, which effectively
deals with object blending. In the EGS and HDFN regions, we extract
H-alpha fluxes from new near-IR (NIR) narrowband imaging observations
obtained with the PISCES NIR camera on the 2.3m Bok telescope on Kitt
Peak. For the COSMOS field, H-alpha fluxes are extracted from new NIR
narrowband imaging observations taken with the NEWFIRM NIR camera on
the Kitt Peak 4m. From the rest-frame far-UV flux and UV slope, we
calculate dust-corrected UV SFRs. We also calculate SFRs from H-alpha
fluxes, corrected for 1 magnitude of extinction. For galaxies at z
0.8, we examine the correlation between dust-corrected UV and H-alpha
SFRs, and compare with previous results at lower redshifts. Walton's
research was supported by the NOAO/KPNO Research Experiences for
Undergraduates (REU) Program which is funded by the National Science
Foundation through Scientific Program Order No. 3 (AST-0243875) of
the Cooperative Agreement No. AST-0132798 between the Association of
Universities for Research in Astronomy (AURA) and the NSF, and The
Observatories of the Carnegie Institute of Washington.
---------------------------------------------------------
Title: Stellar Surface Image of LO Pegasi via Light-curve Inversion
Authors: Harmon, Robert O.; Moore, C.; Decker, R.
2009AAS...21343406H Altcode: 2009BAAS...41Q.304H
We present images of dark starspots on the surface of the K8
main-sequence star LO Pegasi. CCD images of the star and surrounding
field were acquired through B, V, R and I filters at Perkins Observatory
in June and July, 2008. The images were dark-subtracted and flat-fielded
and then aperture photometry was performed to yield light curves through
each of the four filters. These light curves were then simultaneously
inverted via an algorithm devised by one of us (Harmon) so as to yield
images of the spots based on the rotational modulation they produced in
the light curves. The use of multiple filters significantly improves
the latitude resolution of the reconstructions. Comparison of our
results with results from 2006 and 2007 shows that the spot structure
was more complex in 2008 than in the prior years. <P />This research
was funded by the NSF REU Program and the Ohio Wesleyan University
Summer Science Research Program.
---------------------------------------------------------
Title: Hα Luminosity Functions and Star Formation Rate Volume
Densities at z=0.8
Authors: Ly, Chun; Lee, J.; Dale, D.; Salim, S.; Moore, C.; Finn,
R.; Momcheva, I.
2009AAS...21342402L Altcode: 2009BAAS...41R.246L
As part of a larger effort to extend deep, wide H-alpha galaxy surveys
to higher redshift using the NOAO Extremely Wide-Field Infrared Mosaic
(NEWFIRM) at the KPNO-4m, we have identified a sample of galaxies with
H-alpha emission at z=0.8. The galaxies are selected as narrowband
excess emitters in a 1% custom filter centered on the 1.187 micron
low OH-airglow window (hereafter 1190NB). Thus far, the observations
include three NEWFIRM pointings (FOV 27.'6x27.'6) in the Subaru-XMM
Deep Survey (SXDS), one pointing in the Cosmic Origins Survey (COSMOS)
and one in SSA22. These fields have been chosen for the panchromatic
ancillary data that are available. Emission-line galaxy candidates are
identified by the comparison of 1190NB and J-band fluxes, and we detect
sources to a 5sigma sensitivity of 23.0 AB and an SFR of 1 Msun/yr. We
present H-alpha and rest-frame optical and UV luminosity functions,
and star formation rate volume densities, and compare our results with
previous studies.
---------------------------------------------------------
Title: Dark Skies from the Ground Up: Part 2. Programs to Raise
Awareness During the International Year of Astronomy
Authors: Walker, C. E.; Bueter, C.; Crelin, G.; Duriscoe, D.; Moore,
C.; Heatherly, S. A.; Maddalena, R.; Mann, T.; Patten, K.; Pompea,
S. M.; Sparks, R.; Schaaf, F.; Simmons, M.; Smith, M.; Tafreshi, B.
2008ASPC..400..116W Altcode:
Six dark skies-related programs assembled for the International Year
of Astronomy (IYA) are described here. Programs on dark skies awareness
and preservation like GLOBE at Night, Dark Skies Discovery Sites, Quiet
Skies, Astronomy Nights at the (National) Parks, a digital photography
contest and the Good Neighbor Lighting program are presented.
---------------------------------------------------------
Title: “Dark Skies are a Universal Resource” Programs Planned for
the International Year of Astronomy
Authors: Walker, C. E.; Berglund, K.; Bueter, C.; Crelin, B.; Duriscoe,
D.; Moore, C.; Gauthier, A.; Gay, P. L.; Foster, T.; Heatherly,
S. A.; Maddalena, R.; Mann, T.; Patten, K.; Pompea, S. M.; Sparks,
R.; Schaaf, F.; Simmons, M.; Smith, C.; Smith, M.; Tafreshi, B.
2008ASPC..400..298W Altcode:
In an effort to help more people appreciate the ongoing loss of a
dark night sky for much of the world's population and to raise public
knowledge about diverse impacts of excess artificial lighting on local
environments, the International Year of Astronomy's Dark Skies Working
Group has established six “Dark Skies” programs and six “Dark Skies”
resources. The Dark Skies programs include GLOBE at Night (with Earth
Hour), Astronomy Nights in the [National] Parks, Dark Skies Discovery
Sites, Quiet Skies, Good Neighbor Lighting, and a digital photography
contest. Resources include the light education toolkit, the “Let There
Be Night” DVD and planetarium program, the 6-minute video, online
interactions like Second Life, podcasts, and traveling exhibits. The
programs and resources are summarized here, as they were in a poster
for the June 2008 ASP/AAS conference. For more information on these
programs and resources, visit http://astronomy2009.us/darkskies/.
---------------------------------------------------------
Title: Supernova 2008ha in UGC 12682
Authors: Puckett, T.; Moore, C.; Newton, J.; Orff, T.
2008CBET.1567....1P Altcode: 2008CBET.1567A...1P
T. Puckett, Ellijay, GA, U.S.A.; C. Moore, Warwick, NY, U.S.A.; and
J. Newton, Portal, AZ, U.S.A., report the discovery of an apparent
supernova (mag 18.8) on unfiltered CCD images (limiting mag 19.4) taken
with a 0.40-m reflector at Portal on Nov. 7.17 UT in the course of the
Puckett Observatory Supernova Search. The new object was confirmed at
mag 18.2 on images (limiting mag 19.8) taken by T. Orff on Nov. 9.16
with a 0.60-m reflector at Ellijay. SN 2008ha is located at R.A. =
23h34m52s.69, Decl. = +18o13'35".4 (equinox 2000.0), which is about
12" west and 0".5 south of the center of UGC 12682. Nothing is visible
at this position on images taken by Puckett on Sept. 8 (limiting mag
19.4). The exact center of the apparent host galaxy was very hard
to measure, so its coordinates were taken from the Sinbad website
(position end figures 53s.55, 35".9), though Puckett's measurements
on the brightest nodule yield position end figures 53s.31, 38".0.
---------------------------------------------------------
Title: Automation - Recent Progress at Mt Stromlo SLR Station
Authors: Moore, C.
2008lara.workE..78M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Assessing Tracking Performance of High Satellites at Mt
Stromlo SLR Station
Authors: Moore, C.
2008lara.workE..42M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: On the Generation of SLR Output Files at Mt Stromlo
Authors: Moore, C.
2008lara.workE..82M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Effects of Ranging in Circular Polarization
Authors: Luck, J.; Moore, C.
2008lara.workE.111L Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Observing Earth from the Vantage Point of Venus Orbit
Authors: Grinspoon, David H.; Williams, D. M.; Piccioni, G.; Bertaux,
J.; Moore, C.
2008DPS....40.0105G Altcode: 2008BAAS...40Q.386G
Earth has been photographed as a single pixel - a "pale blue dot” -
by Voyager, Cassini, the Mars Exploration Rovers, and other spacecraft,
and studied spectroscopically with Galileo during an Earth fly-by. But
our planet has not been the subject of sustained spectroscopic
and photometric observations as an unresolved, disk-averaged,
time-variable single pixel object (at least not by humans). Disk
averaged observations of Earth have, however, been modeled extensively
as proxy for observations of extrasolar terrestrial planets which
will be possible in the future with instruments such as Darwin or
Terrestrial Planet Finder. Interplanetary observations of Earth can
mimic these planned observations of extrasolar planets. Features that
could potentially be observed include the "red edge” of vegetation,
seasonal albedo changes, photometric phase effects such as specular
reflection from oceans, rotation rate, spectral differences between
oceanic and terrestrial hemispheres, and the seasonal and secular
variations in CO2 abundance caused by the hemispheric distribution
of vegetation and by the industrial activities of "intelligent”
organisms. We have begun regular observations of Earth with the
Venus Express spacecraft, and will present some preliminary results,
and discuss how these observations can provide context for future
observations of Earth-like extrasolar planets.
---------------------------------------------------------
Title: First disk-resolved millimeter observations of Io's surface
and SO{2} atmosphere
Authors: Moullet, A.; Lellouch, E.; Moreno, R.; Gurwell, M. A.;
Moore, C.
2008A&A...482..279M Altcode:
Aims: In spite of considerable progress in the last two decades,
Io's atmosphere remains poorly understood. The goal of this work is to
improve our understanding of its spatial distribution, temperature and
dynamics. <BR />Methods: We present millimeter observations of Io's
surface and SO2 atmosphere at 1.4 mm obtained with the IRAM Plateau
de Bure Interferometer in January-February 2005. With a synthesized
beam of 0.5×1.5”, these observations resolve Io's ~1.0” disk in
the longitudinal / local time direction, and sample the leading and
trailing hemispheres of Io. <BR />Results: The measured continuum total
flux and visibilities show that continuum radiation originates from
a depth of at least 1 cm in Io's subsurface. On both the leading and
trailing sides, emission in the SO2 216.643 GHz line appears spatially
narrower than the continuum, and suggests that the atmosphere covers
~80% of the surface on the leading side and ~60% on the trailing. On the
leading side, disk-resolved spectra yield Doppler shift measurements,
indicating a beam-integrated limb-to-limb velocity difference of
330 ± 100 m/s in the prograde direction. Such a flow allows an
improved fit of disk-averaged SO2 spectra, but its origin remains
to be understood. Mean gas temperatures are in the range 130-180 K,
in agreement with estimates from IR measurements, and with a tendency
for higher trailing vs leading side gas temperatures. On the basis
of realistic plume models, we find that the contribution of isolated
volcanic plumes to the SO2 emission is small. <P />Appendix A is only
available in electronic form at http://www.aanda.org
---------------------------------------------------------
Title: Io's Surface and SO2 Atmosphere: First Disk-resolved
Millimetric Observations
Authors: Moullet, A.; Lellouch, E.; Moreno, R.; Gurwell, M.; Moore, C.
2007LPICo1357..102M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Numerical modeling of ionian volcanic plumes with entrained
particulates
Authors: Zhang, J.; Goldstein, D. B.; Varghese, P. L.; Trafton, L.;
Moore, C.; Miki, K.
2004Icar..172..479Z Altcode:
Volcanic plumes on Jupiter's moon Io are modeled using the direct
simulation Monte Carlo (DSMC) method. The modeled volcanic vent is
interpreted as a "virtual" vent. A parametric study of the "virtual"
vent gas temperature and velocity is performed to constrain the
gas properties at the vent by observables, particularly the plume
height and the surrounding condensate deposition ring radius. Also,
the flow of refractory nano-size particulates entrained in the gas is
modeled with "overlay" techniques which assume that the background gas
flow is not altered by the particulates. The column density along the
tangential line-of-sight and the shadow cast by the plume are calculated
and compared with Voyager and Galileo images. The parametric study
indicates that it is possible to obtain a unique solution for the vent
temperature and velocity for a large plume like Pele. However, for a
small Prometheus-type plume, several different possible combinations of
vent temperature and velocity result in both the same shock height and
peak deposition ring radius. Pele and Prometheus plume particulates are
examined in detail. Encouraging matches with observations are obtained
for each plume by varying both the gas and particle parameters. The
calculated tangential gas column density of Pele agrees with that
obtained from HST observations. An upper limit on the size of particles
that track the gas flow well is found to be ∼10 nm, consistent with
Voyager observations of Loki. While it is certainly possible for the
plumes to contain refractory dust or pyroclastic particles, especially
in the vent vicinity, we find that the conditions are favorable for SO
<SUB>2</SUB> condensation into particles away from the vent vicinity for
Prometheus. The shadow cast by Prometheus as seen in Galileo images is
also reproduced by our simulation. A time averaged frost deposition
profile is calculated for Prometheus in an effort to explain the
multiple ring structure observed around the source region. However,
this multiple ring structure may be better explained by the calculated
deposition of entrained particles. The possibility of forming a dust
cloud on Io is examined and, based on a lack of any such observed
clouds, a subsolar frost temperature of less than 118 K is suggested.
---------------------------------------------------------
Title: Matching Various Observations of Io with DSMC Modeling: Plume,
Plume Shadow, Sodium Field Around Pele
Authors: Zhang, J.; Goldstein, D. B.; Varghese, P. L.; Trafton, L.;
Moore, C.; Miki, K.
2004LPI....35.1972Z Altcode:
Volcanic plumes on Jupiter's moon Io are modeled using the direct
simulation Monte Carlo (DSMC) method. Numerical matches to various
observations of Io with DSMC Modeling: plume, plume shadow and Sodium
field around Pele are presented.
---------------------------------------------------------
Title: Monte Carlo Modeling of [O I] 630 nm Auroral Emission on Io
Authors: Moore, C.; Miki, K.; Goldstein, D. B.; Varghese, P. L.;
Trafton, L.; Zhang, J.
2004LPI....35.1983M Altcode:
A three-dimensional Monte Carlo model for the motion of electrons and
excited oxygen atoms is used to simulate the electron flow around Io,
electron-neutral collisions, and the resulting [O I] 630 nm emission.
---------------------------------------------------------
Title: Modeling of Particulates and Condensates in Io's Pele-type
Volcanic Plumes
Authors: Moore, C.; Zhang, J.; Goldstein, D. B.; Varghese, P. L.;
Trafton, L.
2003LPI....34.2102M Altcode:
DSMC is used to model dust flow and condensate formation in Io's
Pele-Type Plumes. It is found that particles up to .1 micron in diamter
can reach the shock front.
---------------------------------------------------------
Title: BooNE
Authors: McKenney, S.; Smith, D.; Koutsoliotas, S.; Church, E.;
Stancu, I.; Vandalen, G. J.; Johnson, R. A.; Bugel, L.; Conrad, J. M.;
Formaggio, J.; Shaevitz, M. H.; Tamminga, B.; Zimmerman, E.; Bhat,
C.; Brown, B. C.; Ford, R.; Kasper, P.; Kourbanis, I.; Malensek, A.;
Marsh, W.; Martin, P.; Mills, F.; Moore, C.; Russell, A.; Stefanski,
R.; Eitel, K.; Garvey, G. T.; Hawker, E.; Louis, W. C.; Mills,
G. B.; Sandberg, V.; Sapp, B.; Tayloe, R.; White, D. H.; Imlay, R.;
Kim, H. J.; Malik, A.; Metcalf, W.; Sung, M.; Azemoon, T.; Ball, R.;
Berbeco, R.; Riles, K.; Roe, B. P.; Wadia, N.; Yamamoto, J.; Bazarko,
A. O.; Meyers, P. D.; Shoemaker, F. C.
2000APS..DNP.AS046M Altcode:
The phenomenon of neutrino oscillations, where a neutrino of one type
spontaneously transforms into a neutrino of another type, has important
and far-reaching consequences for particle physics and cosmology. For
this phenomenon to occur, at least one neutrino must be massive
and the heretofore observed lepton flavor conservation law must be
violated. There are, at present, several results that indicate neutrino
oscillations and it is not clear how and if these experimental results
are indicative of the situation that actually obtains in Nature. There
is evidence for a deficit of electrons neutrinos observed emanating
from the sun. There is evidence for a deficit of electron neutrinos
compared to muon neutrinos created in the upper atmosphere. And, there
is an excess of electron antineutrinos observed in a beam of muon
antineutrinos by the LSND experiment. The Booster Neutrino Experiment
(BooNE) will focus on the final observation by definitely testing the
LSND result. BooNE has been approved to run at Fermilab and is currently
under construction. If the LSND result is due to oscillations, the
first stage of the experiment (miniBooNE) will observe approximately
1000 oscillation events in the first calendar year of operation.
---------------------------------------------------------
Title: Possible Radio Counterpart of MXB 1730-335
Authors: Rutledge, R.; Moore, C.; Fox, D.; Lewin, W.; van Paradijs, J.
1998ATel....8....1R Altcode:
Contemporaneous observations with RXTE All-Sky Monitor (2-10 keV) and
the VLA at 4.9 and 8.4 GHz reveal a transient radio point-source, the
intensity of which is correlated with the X-ray flux of MXB 1730-335
(The Rapid Burster; RB).
---------------------------------------------------------
Title: Outburst of MXB 1730-335
Authors: Fox, D.; Guerriero, R.; Lewin, W.; Rutledge, R.; Moore, C.;
van der Klis, M.; van Paradijs, J.
1998ATel....9....1F Altcode:
The Rapid Burster (MXB 1730-335) has been detected by the All-Sky
Monitor of the Rossi X-ray Timing Explorer in three consecutive
90-second dwells over the course of the last 28 hours (beginning
28 Jan 1998 22:20 UT). The source was detected at fitted count
rates of 14, 11, and 15 cts/sec (per SSC), with uncertainties of
~2 cts/sec. During quiescence fitted count rates are generally <
6 cts/sec and consistent with zero (3 sigma).
---------------------------------------------------------
Title: MXB 1730-335
Authors: Guerriero, R.; Fox, D.; Lewin, W.; Rutledge, R.; Moore, C.;
van der Klis, M.; van Paradijs, J.
1998IAUC.6815....2G Altcode: 1998IAUC.6815R...1G; 1998IAUC.6815B...1G
R. Guerriero, D. Fox and W. Lewin, Massachusetts Institute of
Technology; R. Rutledge, University of California at Berkeley;
C. Moore, Kapteyn Institute; M. van der Klis, Astronomical Institute
'Anton Pannekoek', University of Amsterdam (UA); and J. van Paradijs,
University of Alabama in Huntsville and UA, report: "The All-Sky Monitor
of the Rossi X-ray Timing Explorer indicates the beginning of a new
x-ray outburst of this rapid burster. Discovery of a likely radio
counterpart (IAUC 6813) makes timely radio and infrared observations
extremely valuable."
---------------------------------------------------------
Title: MXB 1730-335
Authors: Rutledge, R.; Moore, C.; Fox, D.; Lewin, W.; van Paradijs, J.
1998IAUC.6813....2R Altcode: 1998IAUC.6813B...1R; 1998IAUC.6813R...1R
R. Rutledge, University of California at Berkeley; C. Moore,
Kapteyn Institute; D. Fox and W. Lewin, Massachusetts Institute
of Technology; and J. van Paradijs, University of Amsterdam and
University of Alabama at Huntsville, report the discovery of a
radio transient with flux density correlated with the RXTE/ASM x-
ray flux of the rapid burster MXB 1730-335 (cf. IAUC 6409, 6506),
in five observations at the Very Large Array at 8.0 GHz during the
Dec. 1996 and June/July 1997 outbursts. The position of the radio
source is R.A. = 17h33m24s.61, Decl. = -33o23'19".8 (equinox 2000.0;
uncertainty 0".1). Details for a proposed radio campaign during the
next outburst (expected in the next few months) will be given at
http://astron.berkeley.edu/~rutledge/rb.html.
---------------------------------------------------------
Title: Identification of a Likely Radio Counterpart to the Rapid
Burster (MXB 1730-335)
Authors: Rutledge, R.; Moore, C.; Fox, D.; Lewin, W. H. G.; van
Paradijs, J.
1997AAS...19110005R Altcode: 1997BAAS...29.1370R
We have identified a likely radio counterpart to the X-ray
low-mass-X-ray-binary MXB 1730-335 (The Rapid Burster; RB). The
counterpart, which is between 4-5.6sigma away from the X-ray position,
has during our five observations shown radio on/off behavior correlated
with the X-ray on/off behavior as observed by the RXTE/ASM -- the
chance probabilty of an unrelated background source duplicating this
is 1.6%. If the radio and X-ray flux are correlated on ~ seconds
timescales, then observations of radio bursts are well within current
instrumentation capability.
---------------------------------------------------------
Title: Systematic Collection and Analysis of Meteoritic Materials
from Meteor Crater, Arizona
Authors: Kargel, J. S.; Coffin, P.; Kraft, M.; Lewis, J. S.; Moore,
C.; Roddy, D.; Shoemaker, E. M.; Wittke, J. H.
1996LPI....27..645K Altcode:
We have started a systematic collection and analysis of meteoritic
materials from Meteor Crater, Arizona. Since our earlier report
(Kargel, J.S., Kraft, M.D., Roddy, D.J., Wittke, J.H., and Lewis,
J.S., 1995, Eos, v. 76, p. F337), we have found 47 small fragments
of the Canyon Diablo iron meteorite. We also have collected impactite
lapilli; oxidized meteorite fragments; and materials we call amalgamated
meteoritic/lithic fragments (AMLs), which consist of target rocks fused
with and impregnated by oxidized meteoritic iron. The composition of
the impactite lapilli is consistent with admixture of about 3 parts
Kaibab Formation (siliceous dolomitic limestone) and 1 part oxidized
meteorite. In addition, the lapilli contain microscopic spherules of
Ni-rich metal (up to 90% Ni), which can only be explained by partial
oxidation of Canyon Diablo metal. Our interpretation of the lapilli
is that the impact event melted and devolatilized rocks of the Kaibab
Formation (siliceous limestone and dolomite), which mixed with molten
meteoritic metal. If impact heated metal droplets or vapor condensates
attained about 3500 K, then CO2 released from the Kaibab Formation may
have thermally decomposed to CO and O2 and caused partial oxidation
of the metal.
---------------------------------------------------------
Title: A Search for HI Absorption against Gravitational Lenses
Authors: McMahon, P. M.; Moore, C.; Hewitt, J. N.; Rupen, M. P.;
Carilli, C.
1993AAS...183.1203M Altcode: 1993BAAS...25S1307M
We observed the radio spectrum of two gravitationally lensed sources,
MG 0414+0534 and PKS 1830-211, to search for neutral hydrogen absorption
associated with the foreground lensing galaxies. The primary purpose of
these observations is to determine the redshift of the lensing galaxies,
which are both extremely faint, making optical determinations difficult
at best. The observations were performed on the Greenbank 140' telescope
using the spectral processor. The observed frequency range extends from
750 to 1000 MHz, corresponding to a redshift range of 0.42 <= z <=
0.9, and covers most of the range in redshifts predicted by lensing
models. The main difficulty with observations in this frequency range
is severe interference from a variety of sources. We discuss several
methods of minimizing the effects of such interference and present our
results in terms of optical depth limits as a function of wavelength.
---------------------------------------------------------
Title: Tambo Quemado: Extraordinary Concentrations of REE and
Refractory Trace Elements Caused by Artificial Heating
Authors: Olsen, E.; Hutcheon, I.; Moore, C.
1993LPI....24.1103O Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Tables of Spectra of Hydrogen, Carbon, Nitrogen, and Oxygen
Atoms and Ions
Authors: Moore, C. E.
1993tshc.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Atmospheric-lithospheric interactions on Venus: experimental
investigations.
Authors: Tucker, D. W.; Marshall, J. R.; Greeley, R.; Moore, C.;
Pollack, J.
1988NASTM4041..119T Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Book-Review - the Solar Spectrum 3069A - 2095A from the
Echelle Spectrograph Flown in 1961 and 1964 - an Extension from
Rowland's Preliminary Table of Solar Spectrum Wavelengths
Authors: Moore, C. E.; Tousey, R.; Brown, D. M.
1984Sci...223R.584M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Selected tables of atomic spectra - A: Atomic energy levels
- Second edition - B: Multiplet table; O IV. Data derived from the
analyses of optical spectra
Authors: Moore, Charlotte E.
1983stas.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The solar spectrum 3069 A - 2095 A. From the Echelle
Spectrograph flown in 1961 and 1964
Authors: Moore, C. E.; Tousey, R.; Brown, C. M.
1982sses.book.....M Altcode: 1982QB501.S95......
The final listing of solar lines recorded in the NRL echelle
spectra photographed at high resolution from Aerobee rockets flown
in 1961 and 1964 is presented. The wavelength range covered is
3059A to 2095A. It is intended to accompany NRL report no. 7788,
An Atlas of the Solar Spectrum Between 2226 and 2922 Argstroms,
which presents the solar irradiance at 0.03 A resolution as derived
from the echelle spectra. Solar wavelengths are given to 0.01 A,
and estimated solar intensities are listed on a visual scale of 1 to
9. Laboratory wavelengths, multiplet numbers, and references are cited
for each line. Approximately 6150 lines are reported, of which 80%
are identified.
---------------------------------------------------------
Title: New Analyses of Antarctic Carbonaceous Chondrites
Authors: Moore, C.; Cronin, J.; Pizzarello, S.; Ma, M. -S.; Schmitt, R.
1981PolRe.......29M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Solar Spectrum 3069Å - 2095Å - Extension of Rowland's
Preliminary Table of Solar Spectrum Wavelengths
Authors: Moore, C. E.; Tousey, R.; Brown, C. M.
1981BAAS...13R.879M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Selected tables of atomic spectra - A: Atomic energy levels
- Second edition - B: Multiplet table; O V. Data derived from the
analyses of optical spectra
Authors: Moore, Charlotte E.
1980stas.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Selected tables of atomic spectra - A: Atomic energy levels
- Second edition - B: Multiplet tables O VI, O VII, O VIII. Data
derived from the analyses of optical spectra
Authors: Moore, Charlotte E.
1979stas.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The presence of Si I series in the ultraviolet solar spectrum:
3000 to 1200 Å.
Authors: Moore, C. E.; Brown, C. M.; Sandlin, G. D.; Tilford, S. G.;
Tousey, R.
1977ApJS...33..393M Altcode:
Laboratory and solar data are presented which form the basis for
identifying chromospheric Si I absorption lines in UV rocket spectra
of the solar limb. Prints of the Si I laboratory spectrum between 1520
and 1570 A are matched with those of the chromospheric spectrum, and a
striking line-to-line coincidence is observed. Individual absorption
series of Si I covering the 3p(2), 3P, 1D, and 1S ground terms are
tabulated in multiplet form over the wavelength range from 1517 to
3069 A. It is noted that many of the solar lines are blended with both
other Si I lines and lines of other spectra.
---------------------------------------------------------
Title: Leading atomic lines present in solar spectra: H through Ca.
Authors: Moore, C. E.
1977OPurA..10..131M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: XUV spectrum of CI observed from Skylab during a solar flare.
Authors: Feldman, U.; Brown, C. M.; Doschek, G. A.; Moore, C. E.;
Rosenberg, F. D.
1976JOSA...66..853F Altcode: 1976OSAJ...66..853F
A list of 193 neutral carbon lines observed in the XUV spectrum
of a solar flare between 100 and 2000 A using the normal incidence
spectrograph flown on Skylab is presented. Of these, 69 are newly
identified lines arising from transitions from upper levels of
high quantum number where the quantum number is not less than
six. The new lines have allowed the determination of 63 new energy
levels. Wavelengths for an additional 109 transitions were calculated
by polynomial fitting using reference wavelengths of unblended neutral
carbon, Si, N, and S lines emitted in the same atmospheric regions of
the flare. The calculated lines falling between 1102 and 1140 A were not
observed due to low instrumental efficiency at these wavelengths. The
calculated wavelengths are in excellent agreement with those of
Johansson (1965). It appears that in solar spectra recombination
processes are dominant, enhancing the populations of the high quantum
levels relative to the populations of levels with small quantum numbers.
---------------------------------------------------------
Title: Selected tables of atomic spectra - A: Atomic energy levels
- Second edition - B: Multiplet tables; O I. Data derived from the
analyses of optical spectra
Authors: Moore, Charlotte E.
1976stas.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The first spectrum of hafnium (Hf_I).
Authors: Meggers, W. F.; Moore, C. E.
1976fsh..book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Ultraviolet Solar Identifications Based on Extended Absorption
Series Observed in the Laboratory Spectrum of SI I
Authors: Moore, C. E.; Tousey, R.; Sandlin, G. D.; Brown, C. M.;
Ginter, M. L.; Tilford, S. G.
1975Ap&SS..38..359M Altcode: 1975IAUCo..27..359M
The absorption spectrum of Si i in the wavelength region 1500 1900
Å has been photographed at high resolution. The silicon vapour was
produced in a 122 cm long King furnace at 1800 2300°C. Forty-two
Rydberg series have been observed from the ground state terms 3p
<SUP>2</SUP> <SUP>3</SUP> P and<SUP>1</SUP> D to terms associated
with the 3pns and 3pnd configurations. All of the series from
these configurations withJ<4 have been extended with the 3pnd
<SUP>3</SUP> D {<SUB>3</SUB>/<SUP>o</SUP>} levels reachingn=56. Numerous
perturbations have been observed. This laboratory work has provided the
basis for extending the identification of silicon lines in the solar
spectrum. Nearly all lines found in the laboratory spectrum are also
found in rocket spectrograms of the solar chromosphere. More than 300
lines have been attributed to Si i. The excellent correlation between
laboratory and solar Si i lines will be illustrated.
---------------------------------------------------------
Title: Selected tables of atomic spectra - A: Atomic energy levels -
Second edition - B: Multiplet table; N I, N II, N III. Data derived
from the analyses of optical spectra
Authors: Moore, Charlotte E.
1975stas.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A multiplet table of astrophysical interest - Pt.1: Table
of multiplets - Pt.2: Finding list of all lines in the table of
multiplets
Authors: Moore, Charlotte E.
1972mtai.book.....M Altcode: 1972QB465.M6.......
No abstract at ADS
---------------------------------------------------------
Title: Erratum: Lithium in chondritic meteorites. W. Nichiporuk and
Moore, Earth Planet. Sci. Letters 9 (1970) 280-286 W. Nichiporuk
and Moore, Earth Planet. Sci. Letters 9 (1970) 280-286
Authors: Nichiporuk, W.; Moore
1971E&PSL..10..380N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: National Bureau of Standards, Washington, D.C. Report
1969-1970.
Authors: Moore, C. E.
1971BAAS....3..154M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Nsrds-Nbs 35
Authors: Moore, C. E.
1971nsnb.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Selected tables of atomic spectra - A: Atomic energy levels -
Second edition - B: Multiplet tables; N IV, N V, N VI, N VII. Data
derived from the analyses of optical spectra
Authors: Moore, Charlotte E.
1971stas.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: National Bureau of Standards, Washington, D.C. Report
1968-1969.
Authors: Moore, C. E.
1970BAAS....2...98M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Silicon in the sun
Authors: Moore, Charlotte E.
1970VA.....12..307M Altcode:
A brief survey is given of silicon lines in the spectra of the solar
photosphere, chromosphere and corona. These lines arise not only from
the spectrum of the neutral atom, but also from the ionic spectra of
every stage of ionization, i.e. Si I through Si XIV. The ionization
potentials range from 8 to 2673 eV, and the wavelengths of the solar
identifications span the interval from 6 Å to 25129 Å. The wide range
of excitation and ionization thus represented makes silicon a suitable
element for detailed study of solar models, fluxes, abundances and
the like.
---------------------------------------------------------
Title: Ionization potentials and ionization limits derived from the
analyses of optical spectra
Authors: Moore, Charlotte E.
1970ipil.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Selected tables of atomic spectra
Authors: Moore, Charlotte E.
1970stas.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Bibliography on the analyses of optical atomic
spectra. Sect. 1: 1H - 23V; Sect.2: 24[W] - 41[Nb]; Sect.3: 42[Mo]
- 57[La], 72[Hf] - 89[Ac]; Sect.4: 57[La] - 71[Lu], 89[Ac] - 99[Es]
Authors: Moore, Charlotte E.
1969baoa.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: National Bureau of Standards, Washington, D.C. Report
1967-1968.
Authors: Moore, C. E.
1969BAAS....1...84M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Partial Grotrian Diagrams of Astrophysical Interest
Authors: Moore, Charlotte E.; Merrill, Paul W.
1968pgda.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Bibliography on the analyses of optical atomic spectra -
Sect.1: 1[H] - 23[V]
Authors: Moore, Charlotte E.
1968baoa.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Selected tables of atomic spectra - A: Atomic energy levels -
Second edition; B: Multiplet tables - SI I. Data derived from the
analyses of optical spectra
Authors: Moore, Charlotte E.
1967stas.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Future spectroscopy for late-type stars
Authors: Moore, C. E.
1967lts..conf...15M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Elements in the Sun
Authors: Moore, Charlotte E.
1966ossg.book...44M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The solar spectrum 2935 A to 8770 A
Authors: Moore, Charlotte E.; Minnaert, M. G. J.; Houtgast, J.
1966sst..book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Selected tables of atomic spectra - A: Atomic energy levels
- Second edition; B: Multiplet tables - SI II, SI III, SI IV. Data
derived from the analyses of optical spectra
Authors: Moore, Charlotte E.
1965stas.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: National Bureau of Standards Report
Authors: Moore, Charlotte E.; Branscomb, Lewis M.
1963AJ.....68..657M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Extensive Cosmic Ray Air Showers at 4200 m
Authors: Clark, G.; Moore, C.; Escobar, I.; Hersil, J.; Olbert, S.;
Scott, D.
1962JPSJS..17C.243C Altcode: 1962PSJaP..17C.243C; 1962JPSJ...17C.243C; 1962ICRC....7C.243C
No abstract at ADS
---------------------------------------------------------
Title: An ultraviolet multiplet table
Authors: Moore, C. E.
1962aumt.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: An ultraviolet multiplet table
Authors: Moore, Charlotte E.
1961aumt.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Faint lines in the arc spectrum of Iron (Fe1)
Authors: Kiess, Carl C.; Rubin, Vera C.; Moore, Charlotte E.
1961flas.book.....K Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Solar Spectrum from 2635 TO 2085A.
Authors: Malitson, H. H.; Purcell, J. D.; Tousey, R.; Moore, C. E.
1960ApJ...132..746M Altcode:
Solar ultraviolet spectra obtained from rockets flown on December
15,1952, February 21,1955, and June 4, 1956, are presented and analyzed
over the wave-length range 2635-2085 A, together with an absolute
spectral intensity-distribution-curve. In all, 538 absorption features
were observed, and 949 atomic lines are listed as contributing to the
observed spectrum.
---------------------------------------------------------
Title: A multiplet table of astrophysical interest. Part 1
Authors: Moore, Charlotte E.
1959mtai.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Identification list of lines in stellar spectra.
Authors: Moore, C. E.
1959NBSTN..36....1M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Obituary: Henry Norris Russell
Authors: Moore, C. E.
1957Obs....77...67M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Rotational Lines of Ch, OH, and CN in the Solar Spectrum
Authors: Moore, Charlotte E.; Broida, Herbert P.
1957LIACo...7..252M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Molecules in the Solar Spectrum. Introductory Report
Authors: Broida, Herbert P.; Moore, Charlotte E.
1957LIACo...7..217B Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Atomic spectra—Their rôle in astrophysics
Authors: Moore, Charlotte E.
1956VA......2.1209M Altcode:
This paper deals with the use of atomic spectra as a connecting
link between stars and atoms, illustrated by the spectrum of the
Sun, our nearest star. The importance of the multiplets found from
the analyses of laboratory spectra, in the identification of solar
lines is exemplified by selected lines of P I, S I, Si I, Mg I, and
Fe I. Solar lines identified from predicted wavelengths, calculated
from the energy levels, are found among these spectra. The elements
represented in the Sun only in compounds or by only one atomic line
are discussed in some detail. A second revision of Rowland's Table of
Solar Spectrum Wavelengths, including measured equivalent widths and
revised identifications, provides an excellent example of the rôle
of atomic spectra in astrophysics.
---------------------------------------------------------
Title: Spectroscopy
Authors: Moore, Charlotte E.
1956SCoA....1...13M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Revised Analysis of the Solar Spectrum from 2990 TO 2635 A.
Authors: Wilson, N. L.; Tousey, R.; Purcell, J. D.; Johnson, F. S.;
Moore, C. E.
1954ApJ...119..590W Altcode:
New solar spectra from 2990 to 2635 A, obtained from spectrographs
flown in rockets on February 9, 1950, September 3, 1952, and December
15,1952, are presented and analyzed. Lines as close as 0.3 A were
observed. Nearly 500 lines are recorded and are attributed to 1054
atomic lines. The detailed spectral-intensity distribution-curve is
presented instead of the customary visual-intensity estimates. The
effect of instrumental blending is illustrated by comparing a
long-wave-length region of the rocket spectrum with the high-resolution
Utrecht Atlas curve, after averaging the latter over appropriate
wavelength intervals.
---------------------------------------------------------
Title: The Identification of Solar Lines
Authors: Moore, Charlotte E.
1953sun..book..186M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: An ultraviolet multiplet table
Authors: Moore, Charlotte E.
1952aumt.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Predicted lines of Fe I in the arc and in the sun.
Authors: Kiess, C. C.; Moore, Charlotte E.
1950AJ.....55..173K Altcode:
In their analysis of the arc spectrum of iron, Professor Russell and
Miss Moore present a list of 1254 Fe I lines, calculated from term
combinations, that are present in the sun's spectrum but have not been
reported in laboratory descriptions of the iron spectrum. They state,
"It is evident that the spectrum of the iron arc is very far from
being fully observed." An opportunity to test this statement was found
recently, at the National Bureau of Standards, on some spectrograms
on which the iron comparison-spectrum was over-exposed. One set
of plates, taken with a Rowland grating, ruled with 20,000 lines
per inch, covered the region from 66ooA to 868oA; the other set,
taken with a grating ruled by R. W. Wood with 30,000 lines per inch,
covered the region 3600A to 4300A. All the faint lines appearing
on the plates have been measured and com- pared with the published
list of predicted iron lines in the sun's spectrum, with gratifying
results. In the regions covered by our observations, there are 231
solar lines in the red, identified by prediction as Fe I, and 268
in the violet a total of 499. Of these predicted lines 28 per cent
have now been observed in the arc. The percentages of observed lines,
arranged by solar intensity, are distributed as follows: Percentage of
Lines Observed Solar Int. Red Violet Total 42 46 0 55 22 34 -I 28 19
22 -2 30 13 23 -3 4 0 4 In addition, there are 18 unclassified iron
lines in the red and 131 in the violet list that coincide with solar
lines that have heretofore been wholly or partially unidentified. As
soon as the laboratory measurements have been confirmed by additional
observations with different gratings, doubtless many of these new
lines will be classified, and definitively identified in the solar
spectrum. National Bureau of Standards, W)ishington, D. C.
---------------------------------------------------------
Title: An ultraviolet multiplet table - Sect. 1-2
Authors: Moore, C. E.
1950aumt.book.....M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Erratum: The Ultraviolet Solar Spectrum λλ2935-3060
Authors: Babcock, H. D.; Moore; Coffeen
1949ApJ...110..104B Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Ultraviolet Solar Spectrum, λλ 2935-3060.
Authors: Babcock, Harold D.; Moore, Charlotte E.; Coffeen, Mary F.
1948ApJ...107..287B Altcode:
Solar spectrograms, obtained with a 21-foot concave grating, show
better detail below X 3100 than has been reported previously. New
measurements of wave length and visual estimates of intensity have
been made for 665 lines, XX 2935-3060. Solar standards of wave length
near X 4500 were observed in the second order for fixing the scale
in the overlapping third order. Final measurements were made in the
second-order ultraviolet. The new intensities are consistent with
those found in the region of greater wave lengths; many of them differ
widely from the early values. From a thorough study of laboratory data,
identifications have been found for three-fourths of the tabulated
lines. The lower E.P. is given for every classified line. Additional
measurements (500 lines, XX 3060-3150), not presented in detail, show
that differences be- tween our interpretation of solar spectrograms and
that made by Jewell from Rowland's plates occur even where it is easy
to obtain excellent spectrograms. The text is accompanied by tables
and reproductions of spectra
---------------------------------------------------------
Title: No. 745. The ultraviolet solar spectrum, λλ 2835-3060.
Authors: Babcock, Harold D.; Moore, Charlotte E.; Coffeen, Mary F.
1948CMWCI.745....1B Altcode: 1948QB4.M93n745....
No abstract at ADS
---------------------------------------------------------
Title: A Multiplet Table of Astrophysical Interest
Authors: Moore, Charlotte E.
1946C&T....62Q.420M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Neutral barium in the Sun
Authors: Moore, Charlotte E.; Russell, Norris
1946PAAS...10...64M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The solar spectrum lambda 2914-lambda 3060.
Authors: Babcock, Harold D.; Moore, Charlotte E.
1946AJ.....52Q..41B Altcode:
From spectrograms (i .25 A/mm) obtained with the second order of a
~i-foot concave grating a new description of the spectrum between
~29I4 and X3060 has been prepared, giving improved wave lengths
and intensities for 550 lines. Since most of these are blends, the
observational data are subject to greater difficulties of interpretation
than in more open regions of the spectrum. By the method of overlapping
orders the wave lengths were referred to adopted solar standards in
the blue region. Intensities were obtained by estimation, on a scale
intended to correspond to Rowland's intensities in the violet and
near ultraviolet. By comparison with the Revised Multiplet Table1
and other laboratory data fairly definitive identifications have
been found for 380 lines, 200 of which are associated with singly
ionized atoms. Among the latter, members of the iron group are
especially prominent. Lines of Zr ii, Cd ii, Sc ii, Y ii, Cb ii,
and Eu ii are also present. Our results confirm the reality and
the identification of most of the principal features described by
Cornu2 and by Fabry and Buisson,3 but differ in respect to numerous
finer details because of the greater dispersion and resolving power
which we have used. Comparison with Rowland's data4 shows that the
wave lengths in this part of the Revised Rowland require only small
corrections, but we add some weak lines not recorded by him, reject
some which he included, and extensively revise the intensities and the
identifications. Intense lines of Fe and Ni which characterize this
region of the solar spectrum have extensive wings when observed in the
central part of the disk. Rowland described some of these as weak lines,
doubtless because, with inadequate filtering, his spectrograms were
affected by false light. At the solar limb, and indeed well inside
it, we find these wings suppressed, leaving narrow dark cores. Such
effects are more conspicuous in the ultraviolet than elsewhere in
the spectrum. To remove overlapping spectral orders and reduce the
scattering of intense radiation in adjacent parts of the order in use,
filters were mounted in front of the slit. Best results were obtained
with 50 mm of concentrated aqueous solution of NiSO4 in conjunction
with 5 mm of Corning glass number 986. Exposure times extended up to
6 hours. We are indebted to Dr. J. C. Duncan and to Mrs. H. A. Coffeen
for valuable aid in obtaining and reducing the spectrograms. I.Charlotte
E. Moore, A Multiplet Tahle of Astrophysical Interest. Revised Edition,
Princeton Contr. No. 20, 1945. 2.C. R. 86, 103, 1878. 3.J. Phys. Radium,
6th ser., 2, 197 and 297, 1921; Ap. J. 54, 297, 1921. 4.St. John and
others, Revision of Rowland's Preliminary Tahle of Solar Spectrum ~Vave
Lengths. Pub. Carnegie Instn. No. 396, 1928. Mount Wilson Observatory,
Pasadena, Cal~., and National Bureau of Standards, Washington, D. C.
---------------------------------------------------------
Title: Progress on the revision of the multiplet table
Authors: Moore, Charlotte E.
1946PAAS...10..256M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Series Lines of Magnesium in the Solar Spectrum.
Authors: Babcock, Harold D.; Moore, Charlotte E.
1945ApJ...101..374B Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Multiplet Table of Astrophysical Interest. Revised
Edition. Part I - Table of Multiplets. General Arrangement of the
Multiplet Table
Authors: Moore, Charlotte E.
1945CoPri..20D...6M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Multiplet Table of Astrophysical Interest. Revised
Edition. Part I - Table of Multiplets. Forbidden Lines
Authors: Moore, Charlotte E.
1945CoPri..20D..21M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Multiplet Table of Astrophysical Interest. Revised
Edition. Part I - Table of Multiplets. Arrangement of the Multiplets
of Each Spectrum
Authors: Moore, Charlotte E.
1945CoPri..20D...9M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Multiplet Table of Astrophysical Interest. Revised
Edition. Part I - Table of Multiplets. The Multiplet Table-General
Considerations
Authors: Moore, Charlotte E.
1945CoPri..20D...4M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Multiplet Table of Astrophysical Interest. Revised
Edition. Part I - Table of Multiplets. Basis of Selection
Authors: Moore, Charlotte E.
1945CoPri..20D...5M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Multiplet Table of Astrophysical Interest. Revised
Edition. Part I - Table of Multiplets
Authors: Moore, Charlotte E.
1945CoPri..20....1M Altcode: 1945QB4.P94n20.....
No abstract at ADS
---------------------------------------------------------
Title: A Multiplet Table of Astrophysical Interest. Revised
Edition. Part II - Finding List of All Lines in the Table
of Multiplets. Contents of Section on Forbidden Lines. Index
Card. Errata. Finding List
Authors: Moore, Charlotte E.
1945CoPri..21D...3M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Multiplet Table of Astrophysical Interest. Revised
Edition. Part I - Table of Multiplets. Details of
Publication. Bibliography-Description
Authors: Moore, Charlotte E.
1945CoPri..20D..23M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Multiplet Table of Astrophysical Interest. Revised
Edition. Part II - Finding List of All Lines in the Table of
Multiplets. Body of Multiplet Table
Authors: Moore, Charlotte E.
1945CoPri..21....1M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Multiplet Table of Astrophysical Interest. Revised
Edition. Part I - Table of Multiplets. Spectra Omitted from the R M T
Authors: Moore, Charlotte E.
1945CoPri..20D..20M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Multiplet Table of Astrophysical Interest. Revised
Edition. Part I - Table of Multiplets. Spectroscopic Notation
Authors: Moore, Charlotte E.
1945CoPri..20D..16M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Multiplet Table of Astrophysical Interest. Revised
Edition. Part II - Finding List of All Lines in the Table of
Multiplets. Blends. Scope. Part B-Forbidden Lines
Authors: Moore, Charlotte E.
1945CoPri..21D...2M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Multiplet Table of Astrophysical Interest. Revised
Edition. Part II - Finding List of All Lines in the Table of
Multiplets. Part A-Observed and Permitted Predicted Lines
Authors: Moore, Charlotte E.
1945CoPri..21D...1M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Multiplet Table of Astrophysical Interest. Revised
Edition. Part I - Table of Multiplets. Columns of the Table of
Multiplets
Authors: Moore, Charlotte E.
1945CoPri..20D..13M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Multiplet Table of Astrophysical Interest. Revised
Edition. Part I - Table of Multiplets. Special Notes on Individual
Spectra
Authors: Moore, Charlotte E.
1945CoPri..20D..18M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Multiplet Table of Astrophysical Interest. Revised
Edition. Part II - Finding List of All Lines in the Table of
Multiplets. Forbidden Lines
Authors: Moore, Charlotte E.
1945CoPri..21...87M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Arc Spectrum of Iron (Fe 1)
Authors: Russel, Henry Norris; Moore, Charlotte E.; Weeks, Dorothy W.
1944asif.book.....R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Elements in the Sun
Authors: Moore, Charlotte E.
1943S&T.....2R...3M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Stronger Lines of Singly Ionized Dysprosium and
Identifications in the Solar Spectrum.
Authors: King, Arthur S.; Moore, Charlotte E.
1943ApJ....98...33K Altcode:
Table 1 lists 527 of the stronger lines of Dy n in the spectral
range XX 2970-8280. A large proportion of these lines appear in the
high-temperature furnace; and their furnace intensities, supplementing
those in the arc and spark, indicate, in the absence of term-analysis,
the relative levels from which the lines arise. The solar spectrum was
examined for the presence of 95 selected lines whose laboratory behavior
indicated a low-level origin. Of these, 57 were identified in the sun,
in part as members of blends. Of the others, 20 are masked and 18 absent
---------------------------------------------------------
Title: The Presence of Gold in the Sun
Authors: Moore, Charlotte E.; King, Arthur S.
1943PASP...55..109M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Thorium in the Sun
Authors: Moore, Charlotte E.; King, Arthur S.
1943PASP...55...36M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: No. 681. The stronger lines of singly ionized dysprosium and
identifications in th solar spectrum.
Authors: King, Arthur S.; Moore, Charlotte E.
1943CMWCI.681....1K Altcode: 1943QB4.M93n681....
No abstract at ADS
---------------------------------------------------------
Title: Book Reviews: The Masses of the Stars
Authors: Russell, Henry Norris; Moore, Charlotte E.
1940PA.....48..285R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Neutral Barium in the Sun
Authors: Moore, Charlotte E.; Russell, H. N.
1940PASP...52..373M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Systematic and Accidental Errors of Spectroscopic
Parallaxes.
Authors: Russell, Henry Norris; Moore, Charlotte E.
1940ApJ....92..354R Altcode:
I. The stars for which trigonometric and spectroscopic parallaxes are
available were divided into eight groups of approximately equal number,
in order of the "reduced" spectroscopic parallaxes and of the reduced
proper motions, and the mean reduced spectroscopic and trigonometric
parallaxes were compared. Tue deviations from linear correlation
between the two are no larger than can be attributed to the accidental
and sampling errors-both for the biased and impartial groupings and
also for four ranges of spectral class among main-sequence stars,
for all these together, and for giants. To distinguish between the
results of the assumptions of linear correlation between the absolute
mag- nitudes and between the reduced parallaxes would demand several
times the observa- tional data now available (i 140 stars). For stars
differing greatly in absolute magni- tude from the general mean (such as
Groombridge 1830), these linear correlations are probably invalid; and
the data are at present insufficient for a reliable calibration. II. The
dispersion constants for the reduced parallaxes have been redetermined
by analysis of these mean values (Table 4) and compared with those
obtained by our earlier correlation analysis (Table 5). The factor
i/i, by which the differences of the tabular spectroscopic absolute
magnitude from the mean for the spectral subclass must be multiplied
in order to obtain an impartial calibration, comes out consistently
larger by the latter method. III. The correlation between the reduced
parallaxes and proper motions (which is equivalent to that between the
absolute magnitude M and H = in + 5 log j~) shows that, for groups
brighter and fainter than the normal for the spectral subclass, =
0.74 for main-sequence stars and o.66 for giants. Comparison of giants
and dwarfs gives ~M/~H = 0.69; of stars in different parts of the main
sequence, o.8o. IV. Unavoidable deviations of spectroscopic absolute
magnitudes from the true values may arise from physical causes within
the stars, such as differeiices in the relative abundance of hydrogen
and heavy elements, either in the interior or in the atmosphere,
and differences in the contribulion of negative hydrogen ions to the
general opacity. These differences may account for a considerable
portion of the apparent "errors" of spectroscopic parallaxes. V. These
effects, combined with a correlation between the masses and the space-
velocities of the stars, may cause grouping by H to be systematically
different from one by M; but this appears inadequate to account for
the systematic differences mentioned above. VI. Since no conclusive
reasons have been found for preferring one of the sets of con- stants
described in (II) to the other, weighted means have been taken, and
the remain- ing dispersion constants have been determined with the
aid of these. Results for the reduced parallaxes appear in Table 9;
and the corresponding constants for the absolute magnitudes (derived
on the assumption that these have a normal distribution), in Table
io. The mean-square difference 0 between the spectroscopic absolute
magnitudes, M~, as published in Mt. W. Contr. No. 511, and the true
values is ±o'~'48 for main-sequence stars as a whole and ± o~ for
giants. Joy's values, derived from double stars and clusters, are in
substantial agreement with this. To obtain an impartial calibration, *
Contributions from the Mount Wilson Observatory, Carnegie Institution of
Wash- ington, No. 636. `Research associate of the Carnegie Institution
of Washington
---------------------------------------------------------
Title: A Comparison of spectroscopic and trigonometric parallaxes
Authors: Russell, Henry Norris; Moore, Charlotte E.
1939PAAS....9..133R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: New identifications of solar lines
Authors: Moore, Charlotte E.
1939PAAS....9...15M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The spectrum of ionized vanadium
Authors: Meggers, W. F.; Moore, Charlotte E.
1939PAAS....9Q.225M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Comparison of Spectroscopic and Trigonometric Parallaxes
Authors: Russell, Henry Norris; Moore, Charlotte E.
1938ApJ....87..389R Altcode:
The calibration of spectroscofric absolute magnitudes has been made
by selecting groups of stars with similar intensities for pairs of
"sensitive" lines and adjusting the calibration-curves so that the
absolute magnitudes which these lines give for each group shall agree
with those determined for the same stars from other data (trigo-
nometric parallaxes, proper motions, etc.). Since the spectroscopic
data are affected by accidental errors, this practically unavoidable
process gives a regressioii-curve which inevitably underestimates the
deviations of the individual absolute magnitudes from the general mean
for the spectral class concerned, while giving an accurate value I
or this mean. The magnitude of this effect can be determined by the
comparison of the spectro- scopic and trigonometric parallaxes of
the same stars, provided that the accidental errors of the latter
are known. Formulae are developed for the determination of the
constants involved in this problem, and of the statistical errors of
the constants derived from samples of finite size. The spectroscopic
parallaxes of Mo~unt Wilson Contribution No. 511 are then com- pared
with the trigonometric parallaxes given in Schlesinger's General
Catalogue (Yale, 1936). For the 1140 stars of the main sequence which
are available, the real dispersion in absolute magnitude about the
mean for the subclass of the Draper classification corresponds to a
standard deviation of ±34 per cent in the parallax, while the errors
of the spectroscopic determination (including the effects of real
differences between stars whose sensitive lines appear the same) give
a standard deviation of ±38 per cent. The means for all the stars of a
given subclass are accurate within 5 per cent, except for a few faint M
dwarfs. The differences between the individual spectroscopic absolute
magnitudes and the mean for the subclass should be multiplied by 1.19
to give an im- proved calibration for groups selected according to
the spectroscopic criteria, but by 2.6 in order to give values which
wifi be correct in the mean for groups of stars selected by criteria
independent of the spectroscopic data. When these stars are divided
into seven groups according to spectral type, the results for all
are similar, although with some- what larger fluctuations than would
be anticipated from errors of sampling. Comparison of the mean for
groups of stars selected by spectroscopic absolute magnitude and by
proper motion fully confirms the anticipated differences. For the
giant stars, 732 in number, the parallaxes are smaller; but good
mean results can be obtained. The standard deviation in parallax,
corresponding to real dispersion in absolute magnitude, is ± 52 per
cent (increased by the inclusion of supergiants and subgiants), while
that arising from the spectroscoJ~ic errors is ± 38 per cent. The
general means of the spectroscopic and trigonometric parallaxes agree
perfectly. The differences from the mean require no correction for
grouping according to spectroscopic criteria, but a factor of 1.6
when the criteria are independent. A special discussion of ~7 stars
of great absolute brightness shows that the probable errors assigned
in "Schlesinger's Catalogue" represent correctly the true accidental
errors of the determinations. Formulae and tables are given (sec. 13)
for the rapid application of the corrections to the spectroscopic
parallaxes. These are important for only a small fraction of the whole
number of stars. Their applicabifity to supergiants is doubtful. *
Contributions from the Mount Wilson Observatory, Carnegie Institution of
Wash- ington, No. 589. `Research Associate, Mount Wilson Observatory. 38
---------------------------------------------------------
Title: Orbit of the binary 20 Persei
Authors: Moore, Charlotte E.
1937AJ.....46..162M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: New Identifications of Solar Lines
Authors: Moore, Charlotte E.
1937ApJ....85...79M Altcode:
A summary of elements present in the solar spectrum-is discussed. The 92
chemical elements are divided into five groups as follows: 61 present;
3 possibly present (Sn, Ta, Tb); 2 having insufficient solar data
(Ne, Cs); 7 having insufficient laboratory data; 19 absent. Over 400
faint new lines have been measured between X 66oo and X 7330 as part of
Mr. Babcock's work on the infrared solar spectrum. Among these, the two
Li lines at X 6707, previously found only in the spot spectrum, have
been measured in the spec- trum of the disk (intensity -3). Similarly,
the stronger Rb line X 7800 is also present in the disk spectrum. Os and
Ir may now be classified as present without question. Their presence
has previously been suspected but not confirmed. Tu has been detected
for the first time. It occurs only in the ionized state, like most
of the rare earths. Laboratory material has been lacking for this
element until recently. Three elements, Sn, Ta, and Tb, must remain as
doubtfully present. Laboratory measures are needed for Sn and Tb. The
three strongest Ta lines agree with faint solar lines recorded by
Rowland, but the reality of two of the solar lines is somewhat ques-
tionable. The strongest accessible line of Ne is suspected to be present
in the chromosphere, but further measures are needed for confirmation of
its presence. For Cs, the infrared sun-spot spectrum must be adequately
photographed before any statement can be made as to its presence
or absence. Of the 7 elements with insufficient laboratory data,
the spectra of Th, U, and Ho may be observed in the near future. The
remaining 4 elements Ma, 85, 87, and Ii, have not been isolated in
sufficient quantity, if at all, to make this possible. The 19 absent
elements are listed in order of excitation potential of the accessible
lines, except for the radioactive elements, which are not to be expected
---------------------------------------------------------
Title: Measures and dynamical parallaxes of 108 A double stars
Authors: Aitken, Robert Grant; Moore, Charlotte Emma
1937LicOB..18...53A Altcode: 1937LicOB.485...53A; 1936LicOB..18...53A
No abstract at ADS
---------------------------------------------------------
Title: No. 565. New identifications of solar lines.
Authors: Moore, Charlotte E.
1937CMWCI.565....1M Altcode: 1937QB4.M93n565....
No abstract at ADS
---------------------------------------------------------
Title: A Scale of Wave-Lengths in the Infra-Red Solar Spectrum
Authors: Babcock, Harold D.; Moore, Charlotte E.; Hoge, Wendell P.
1936ApJ....83..103B Altcode:
Interferometer measurements made in 1927 have in some cases been
slightly improved in relative value without systematic change of
scale. Similar new observations extend the scale to X 10603. Standards
of reference have been chosen from the A band of atmospheric oxygen as
previously determined from neon standards. With the concave grating
alone provisional standards have been measured as far as A 12103 in
terms of adopted solar standards in the visual region by the method of
over- lapping orders. Methods of reduction are described, and tables
for finding the correction due to observer's motion relative to the
sun are given. Resulis, in Table VT, include 249 lines, of which 142
are telluric. The accuracy of the wave-lengths in Table VT, when tested
indirectly by means of a much larger collection of data based on these
standards, is found to be decidedly higher than that of most laboratory
data in the infra-red, and even well beyond X ioooo our wave-lengths
appear to be reliable to about i part in a rniffion
---------------------------------------------------------
Title: Identifications of infra-red solar lines
Authors: Moore, Charlotte E.; Babcock, H. D.
1936PAAS....8..120M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: No. 534. A scale of wave-lengths in the infra-red solar
spectrum.
Authors: Babcock, Harold D.; Moore, Charlotte E.; Hoge, Wendell P.
1936CMWCI.534....1B Altcode: 1936QB4.M93n534....
No abstract at ADS
---------------------------------------------------------
Title: Recent identifications of solar lines
Authors: Moore, Charlotte E.
1936PAAS....8R.218M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Presence of Phosphorus in the Sun
Authors: Moore, Charlotte E.; Babcock, Harold D.; Kiess, C. C.
1934ApJ....80...59M Altcode:
On the basis of specroscopic evidence phosphorus may with some assurance
be added to the long list of elements present in the sun. Three
infra-red solar lines are attributed without question to phosphorus,
and two with some doubt. The laboratory spectrum is discussed and a
table gives the observable multiplets and corresponding solar data
from which the results are derived.
---------------------------------------------------------
Title: The Presence of Sulphur in the Sun
Authors: Moore, Charlotte E.; Babcock, Harold D.
1934ApJ....79..492M Altcode:
With the aid of new laboratory material on analysis, and unpublished
infra-red solar wave-lengths, the spectroscopic evidence of the presence
of sulphur in the sun is discussed. Meissner's identifications are
revised and extended. Seventeen sulphur lines are identified in the
solar spectrum without question and six with some doubt. The observable
lines of ionized sulphur have such high excitation potentials that they
could not be expected to appear in the sun. The coincidence of a few
solar and laboratory wave-lengths is probably due to chance. Tables
give the laboratory and solar data on which the results are based
---------------------------------------------------------
Title: A multiplet table of astrophysical importance
Authors: Moore, Charlotte E.
1933PAAS....7Q..97M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Measures and dynamical parallaxes of 323 A double stars
Authors: Aitken, Robert Grant; Moore, Charlotte Emma
1933LicOB..16...96A Altcode: 1933LicOB.451...96A; 1932LicOB..16...96A
No abstract at ADS
---------------------------------------------------------
Title: Atomic lines in the sun-spot spectrum
Authors: Moore, Charlotte E.
1933alss.book.....M Altcode: 1933QB525.M58......
No abstract at ADS
---------------------------------------------------------
Title: A multiplet table of astrophysical interest
Authors: Moore, Charlotte Emma
1933mtai.book.....M Altcode: 1933QB465.M6.......
No abstract at ADS
---------------------------------------------------------
Title: On the masses of giant stars
Authors: Russell, H. N.; Moore, Charlotte E.
1933PAAS....7..184R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Atomic lines in the sun-spot spectrum
Authors: Moore, Charlotte E.
1933PAAS....7R..10M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Presence of Ytterbium in the Sun
Authors: Moore, Charlotte E.; Meggers, William F.
1932PASP...44..175M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Some Results from a Study of the Atomic Lines in the Sun-Spot
Spectrum
Authors: Moore, Charlotte E.
1932ApJ....75..298M Altcode:
A detailed study of the atomic lines in the sun-spot spectrum has
resulted in a deter- mination of the effective temperature of sun-spots
and the pressure and amount of material above them. Intensities for
6312 lines of atomic origin in the spot spectrum have been estimated
on the Rowland scale on original negatives and on prints made from
them. The plates were those taken with the 150-foot tower telescope and
75-foot spectrograph for the Mount Wilson map of the spot spectrum. The
third order was used from X39oo to X 5400, the second order from X
5400 to X óooo. The spectrum of the disk appears on each side of
the spot spectrum. The use of a quarter-wave plate and Nicol prism
gives the lines subject to Zeeman effect a dentate appearance in the
spectrum of the spot, which makes it possible to select the atomic
lines. Intensities estimated from the prints agree systematically
with those from the plates. The identifications of lines in the
solar spectrum from X 2975 to X 6635 and in the spot spectrum from X
3894 to A 6635 have been revised and extended. Lines of Lu~ have been
identified for the first time. The principal criteria employed have been
labora- tory wave-lengths and intensities, the multiplet relations and
excitation potentials, which are now available for almost all elements
except the rare earths, and the behavior of the lines in the spectrum of
`y Cygni, a giant star of class F8. Nine hundred and thirty-six faint
solar lines not previously identified and 21 spot lines have been
recog- nized as faint members of multiplets not yet observed in the
laboratory, but accurately predictable. Of these, 437 are due to Fe,
122 to Cr, 89 to Ni, 73 to Cr~, 67 to Ti, 50 to Fe+, 43 to Ti+, 21 to
Co, 20 to Zr+, 12 to V, 9 to V+, 7 to Sc+, and 7 to Mn. Three hun-
dred and ninety-six new atomic lines which appear oniy in the spot
spectrum have been measured and 193 identified. A quantitative study
of the composition of the atmosphere above sun-spots has been based on
the calibration of the Rowland intensity scale. This gives a quantity
V which is the logarithm of the ratio of the number of atoms producing
a line in the spot spec- trum to that effective in the formation of
the same line in the solar spectrum. From thermodynamic theory, V =
Y0+SE~, where V0 is the logarithm of the ratio of the num- bers of
neutral atoms above equal areas of the photospheres of spot and disk,
E~ the excitation potential, and S= 5040 (i/T- i/T'). T and T' are the
effective temperatures of disk and spot, respectively. For enhanced
lines, V0 must be replaced by Y1, the corre- sponding quantity for
ionized atoms. The observed data from 6 elements give a weighted mean
value of S equal to -0.190±0.010. Taking T= 574Q0 K, T'=472o° ±
400 K, where the probable error is a measure of the accordance of
the observations. From the observed values of V0 and V1 and the Saha
equation as modified by Pannekoek and Fowler, the ratio of the electron
pressures P~ (spot) and ~e (disk) can be found. Eight elements have a
sufficient number of arc and spark lines present in both solar and spot
spectra to be used. The weighted mean value of log (P~/Pe) iS -0.22 ±
0.07, i.e., the electron pressure over the spot is o.6o ± 0.10 times
that over the disk. Russell has defined the "level of ionization" as
the ionization potential of an atom which would be just 50 per cent
ionized under given conditions. For the spot this level is 7.0±0.1
volts, as compared with 8.5±0.1 for the disk. From these quantities
the percentages of ionization for disk and spot were calculated for
28 elements. By compar- ing these percentages with V0 and Y1, it
was found that the amount of material per unit `Contributions from
the Mount Wilson Observatory, Carnegie Institution of Washing- ton,
No. 446; continued from this Journal, April, 1932. 29
---------------------------------------------------------
Title: Some Results from a Study of the Atomic Lines in the Sun-Spot
Spectrum
Authors: Moore, Charlotte E.
1932ApJ....75..222M Altcode:
A detailed study of the atomic lines in the sun-spot spectrum has
resulted in a deter- mination of the effective temperature of sun-spots
and the pressure and amount of material above them. Intensities for
6312 lines of atomic origin in the spot spectrum have been estimated
on the Rowland scale on original negatives and on prints made from
them. The plates were those taken with the 150-foot tower telescope and
75-foot spectrograph for the Mount Wilson map of the spot spectrum. The
third order was used from X39oo to X 5400; the second order from X
5400 to X óooo. The spectrum of the disk appears on each side of
the spot spectrum. The use of a quarter-wave plate and Nicol prism
gives the lines subject to Zeeman effect a dentate appearance in the
spectrum of the spot, which makes it possible to select the atomic
lines. Intensities estimated from the prints agree systematically
with those from the plates. The identifications of lines in the
solar spectrum from X 2975 to X 6635 and in the spot spectrum from X
3894 to X 6635 have been revised and extended. Lines of Lu~ have been
identified for the first time. The principal criteria employed have been
labora- tory wave-lengths and intensities, the multiplet relations and
excitation potentials, which are now available for almost all elements
except the rare earths, and the behavior of the lines in the spectrum of
`y Cygni, a giant star of class F8. Nine hundred and thirty-six faint
solar lines not previously identified and 21 spot lines have been recog-
nized as faint members of mattiplets not yet observed in the laboratory,
but accurately predictable. Of these, 437 are due to Fe, 122 to Cr,
89 to Ni, 73 to Cr~, 67 to Ti, 50 to F&, 43 to Ti+, 21 to Co, 20
to Zr+, 12 to V, 9 to V~, 7 to Sc+, and 7 to Mn. Three hun- dred and
ninety-six new atomic lines which appear only in the spot spectrum
have been measured and 193 identified. A quantitative study of the
composition of the atmosphere above sun-spots has been based on the
calibration of the Rowland intensity scale. This gives a quantity Y,
which is the logarithm of the ratio of the number of atoms producing
a line in the spot spec- trum to that effective in the formation of
the same line in the solar spectrum. From thermodynìamic theory Y =
Y0+SE~, where V0 is the logarithm of the ratio of the num- bers of
neutral atoms above equal areas of the photospheres of spot and disk,
E~ the excitation potential, and S=5o4o (i/T- i/T'). Tand T' are the
effective temperatures of disk and spot, respectively. For enhanced
lines, Y0 must be replaced by Y1, the corre- sponding quantity for
ionized atoms. The observed data from 6 elements give a weighted mean
value of S equal to -0.190 ± 0.010. Taking T= 57400 K, T' = 47200
± 4Q0 K, where the probable error is a measure of the accordance
of the observations. From the observed values of V0 and V1 and the
Saha equation as modified by Pannekoek and Fowler, the ratio of the
electron pressures P~ (spot) and Fe (disk) can be found. Eight elements
have a sufficient number of arc and spark lines present in both solar
and spot spectra to be used. The weighted mean value of log (P~/Pe)
iS -0.22 ± 0.07, i.e., the electron pressure over the spot is o.6o
± 0.10 times that over the disk. Russell has defined the "level of
ionization" as the ionization potential of an atom which would be just
50 per cent ionized under given conditions. For the spot this level
is 7.0 ± o.i volts, as compared with 8.5 ± o.i for the disk. From
these quantities the percentages of ionization for disk and spot were
calculated for 28 elements. By compar- ing these percentages with F0
and Y1, it was found that the amount of material per uni
---------------------------------------------------------
Title: No. 446. Some results from a study of the atomic lines in
the Sun-spot spectrum.
Authors: Moore, Charlotte E.
1932CMWCI.446....1M Altcode: 1932QB4.M93n446....
No abstract at ADS
---------------------------------------------------------
Title: The Absence of Rhenium from the Solar Spectrum
Authors: Moore, Charlotte E.; Meggers, W. F.
1931PASP...43..345M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Some Results from a Recent Study of the Atomic Lines in the
Sun-Spot Spectrum
Authors: Moore, Charlotte E.
1931PASP...43..272M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: New Comet
Authors: Shapley, H.; van Maanen; Moore; Nagata, M.
1931IAUC..327....1S Altcode:
A telegram from Professor Shapley announces that van Maanen has
telegraphed the photographic confirmation by Moore, Mt. Wilson, of
a comet found by Nagata. The following position was given: 1931 UT
R.A. Decl. July 17 16h26m 10 41 + 9 48
---------------------------------------------------------
Title: Atomic Lines in the Sun-Spot Spectrum.
Authors: Moore, Charlotte Emma
1931PhDT.........2M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The relation between the degree of anomalous dispersion and
line intensity (abstract)
Authors: Moore, Charlotte E.
1931PAAS....6..234M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A calibration of Rowland's intensity scale for solar lines
(abstract)
Authors: Russell, Henry Norris; Adams, Walter S.; Moore, Charlotte E.
1931PAAS....6..117R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Presence of Ionized Lutecium in the Sun
Authors: Moore, Charlotte E.
1930PASP...42..346M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Elements and ephemeris of Comet B 1930 (Beyer)
Authors: Bower, Ernest Clare; Moore, Charlotte Emma
1930LicOB..15...16B Altcode: 1930LicOB.423...16B
No abstract at ADS
---------------------------------------------------------
Title: Photographic determinations of the position of the moon
Authors: Moore, Charlotte Emma; Shapley, Harlow
1930AnHar..85..169M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Observations of Comet B 1929 (Neujmin) and of minor planets
Authors: Krieger, Charles John; Bobrovnikoff, Nicholas Theodore;
Whipple, Fred Lawrence; Moore, Charlotte Emma; Hayford, Phyllis
1930LicOB..15...20K Altcode: 1930LicOB.424...20K
No abstract at ADS
---------------------------------------------------------
Title: Dynamical parallaxes of 1777 double stars
Authors: Russell, H. N.; Moore, C. E.
1929AJ.....39..165R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The relation between the degree of anomalous dispersion and
line intensity (abstract)
Authors: Moore, Charlotte E.
1929PA.....37..273M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Presence of Predicted Iron Lines in the Solar Spectrum
and the Terms in the Arc Spectrum of Iron
Authors: Moore, Charlotte E.; Russell, Henry Norris
1928ApJ....68..151M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Calibration of Rowland's Scale of Intensities for Solar Lines
Authors: Russell, Henry Norris; Adams, Walter S.; Moore, Charlotte E.
1928ApJ....68....1R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: On the Presence of the Rare-Earth Elements in the Sun
Authors: St. John, Charles E.; Moore, Charlotte E.
1928ApJ....68...93S Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Predicted lines of CrII in the spectra of the Sun and of
alpha Persei.
Authors: Dunham, T., Jr.; Moore, C. E.
1928ApJ....68...37D Altcode:
No abstract at ADS
---------------------------------------------------------
Title: No. 364. On the presence of the rare-earth elements in the Sun.
Authors: St. John, Charles E.; Moore, Charlotte E.
1928CMWCI.364....1S Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A calibration of Rowland's intensity scale for solar lines
(abstract)
Authors: Russell, Henry Norris; Adams, Walter S.; Moore, Charlotte E.
1928PA.....36..295R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: No. 365. The presence of predicted iron lines in the solar
spectrum and the terms in the arc spectrum of iron.
Authors: Moore, Charlotte E.; Russell, Henry Norris.
1928CMWCI.365....1M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: No. 360. Predicted lines of Cr II in the spectra of the Sun
and of alpha Persei.
Authors: Dunham, Theodore, Jr.; Moore, Charlotte E.
1928CMWCI.360....1D Altcode:
No abstract at ADS
---------------------------------------------------------
Title: No. 358. A calibration of Rowland's scale of intensities for
solar lines.
Authors: Russell, Henry Norris; Adams, Walter S.; Moore, Charlotte E.
1928CMWCI.358....1R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: As to Cadmium in the Sun
Authors: St. John, C. E.; Moore, Charlotte E.
1927PASP...39..314S Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Laboratory Evidence on the Presence in the Sun of Ionized
Praseodymium, Neodymium and Samarium
Authors: King, A. S.; Moore, Charlotte E.
1927PASP...39..238K Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Probable Occurrence of Doubly-Ionized Cerium in the Sun
Authors: King, A. S.; Moore, Charlotte E.
1927PASP...39..240K Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Laboratory Evidence on the Presence of Ionized Cerium in
the Sun
Authors: King, A. S.; Moore, Charlotte E.
1927PASP...39...47K Altcode:
No abstract at ADS
---------------------------------------------------------
Title: On the Winged Lines in the Solar Spectrum
Authors: Moore, Charlotte E.; Russell, Henry Norris
1926ApJ....63....1M Altcode:
No abstract at ADS
