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@ARTICLE{Aharonian:481249,
author = {Aharonian, F. and Benkhali, F. Ait and Anguner, E. O. and
Ashkar, H. and Backes, M. and Martins, V. Barbosa and
Batzofin, R. and Becherini, Y. and Berge, D. and Bernloehr,
K. and Boettcher, M. and Boisson, C. and Bolmont, J. and de
Lavergne, M. de Bony and Breuhaus, M. and Brose, R. and
Brun, F. and Bulik, T. and Bylund, T. and Cangemi, F. and
Caroff, S. and Casanova, S. and Cerruti, M. and Chand, T.
and Chen, A. and Chibueze, O. and Cotter, G. and Cristofari,
P. and Mbarubucyeye, Jean Damascene and Devin, J. and
Djannati-Atai, A. and Dmytriiev, A. and Egberts, K. and
Einecke, S. and Ernenwein, J.-P. and Feijen, K. and Fiasson,
A. and de Clairfontaine, G. Fichet and Fontaine, G. and
Funk, S. and Gabici, S. and Gallant, Y. A. and
Ghafourizadeh, S. and Giavitto, Gianluca and Giunti, L. and
Glawion, D. and Glicenstein, J. F. and Grondin, M.-H. and
Hoerbe, M. and Hofmann, W. and Holch, Tim Lukas and Holler,
M. and Horns, D. and Huang, Zhiqiu and Jamrozy, M. and
Joshi, V. and Jung-Richardt, I. and Kasai, E. and
Katarzynski, K. and Katz, U. and Khelifi, B. and Kluzniak,
W. and Komin, Nu. and Kosack, K. and Kostunin, D. and
Lemiere, A. and Lemoine-Goumard, M. and Lenain, J.-P. and
Leuschner, F. and Lohse, T. and Luashvili, A. and Lypova, I.
and Mackey, J. and Malyshev, D. and Marandon, V. and
Marchegiani, P. and Marcowith, A. and Marti-Devesa, G. and
Marx, R. and Maurin, G. and Meintjes, P. J. and Meyer, M.
and Mitchell, A. and Moderski, R. and Mohrmann, L. and
Montanari, A. and Moulin, E. and Muller, J. and Nakashima,
K. and de Naurois, M. and Nayerhoda, A. and Niemiec, J. and
Noel, A. Priyana and O'Brien, P. and Ohm, Stefan and
Olivera-Nieto, L. and Wilhelmi, E. de Ona and Ostrowski, M.
and Panny, S. and Panter, M. and Parsons, R. D. and Peron,
G. and Poireau, V. and Prokhorov, D. A. and Puehlhofer, G.
and Punch, M. and Quirrenbach, A. and Reichherzer, P. and
Reimer, A. and Reimer, O. and Renaud, M. and Reville, B. and
Rieger, F. and Rowell, G. and Rudak, B. and Ricarte, H.
Rueda and Sahakian, V. and Sailer, S. and Salzmann, H. and
Sanchez, D. A. and Santangelo, A. and Sasaki, M. and
Schafer, J. and Schussler, F. and Schutte, H. M. and
Schwanke, U. and Shapopi, J. N. S. and Simoni, R. and Sol,
H. and Specovius, A. and Spencer, S. and Stawarz, L. and
Steinmassl, S. and Steppa, C. and Sushch, I. and Takahashi,
T. and Tanaka, T. and Taylor, A. M. and Terrier, R. and
Tsirou, M. and Uchiyama, Y. and Unbehaun, T. and van Eldik,
C. and Veh, J. and Vink, J. and Voelk, H. J. and Wagner, S.
J. and Werner, F. and White, R. and Wierzcholska, A. and
Wong, Yu Wun and Yusafzai, A. and Zacharias, M. and
Zargaryan, D. and Zdziarski, A. A. and Zech, A. and Zhu,
Sylvia Jiechen and Zouari, S. and Zywucka, N.},
collaboration = {H. E. S. S.{ Collaboration}},
title = {{E}vidence for $\gamma$-ray emission from the remnant of
{K}epler’s supernova based on deep {H}.{E}.{S}.{S}.
observations},
journal = {Astronomy and astrophysics},
volume = {662},
issn = {0004-6361},
address = {Les Ulis},
publisher = {EDP Sciences},
reportid = {PUBDB-2022-04260, arXiv:2201.05839},
pages = {A65},
year = {2022},
abstract = {Observations with imaging atmospheric Cherenkov telescopes
(IACTs) have enhanced our knowledge of nearby supernova (SN)
remnants with ages younger than 500 yr by establishing
Cassiopeia A and the remnant of Tycho’s SN as
very-high-energy (VHE) γ-ray sources. The remnant of
Kepler’s SN, which is the product of the most recent
naked-eye SN in our Galaxy, is comparable in age to the
other two, but is significantly more distant. If the γ-ray
luminosities of the remnants of Tycho’s and Kepler’s SNe
are similar, then the latter is expected to be one of the
faintest γ-ray sources within reach of the current
generation IACT arrays. Here we report evidence at a
statistical level of 4.6σ for a VHE signal from the remnant
of Kepler’s SN based on deep observations by the High
Energy Stereoscopic System (H.E.S.S.) with an exposure of
152 h. The measured integral flux above an energy of 226 GeV
is $∼0.3\%$ of the flux of the Crab Nebula. The spectral
energy distribution (SED) reveals a γ-ray emitting
component connecting the VHE emission observed with H.E.S.S.
to the emission observed at GeV energies with Fermi-LAT. The
overall SED is similar to that of the remnant of Tycho’s
SN, possibly indicating the same nonthermal emission
processes acting in both these young remnants of
thermonuclear SNe.},
keywords = {gamma ray: emission (INSPIRE) / energy: high (INSPIRE) /
Cherenkov counter: atmosphere (INSPIRE) / supernova
(INSPIRE) / energy spectrum (INSPIRE) / VHE (INSPIRE) / HESS
(INSPIRE) / GeV (INSPIRE) / flux (INSPIRE) / spectral
(INSPIRE) / imaging (INSPIRE) / GLAST (INSPIRE) /
statistical (INSPIRE) / galaxy (INSPIRE) / gamma rays:
general (autogen) / supernovae: individual: Kepler (autogen)
/ gamma-rays: general (autogen) / supernovae: individual:
Kepler’s SN (autogen) / ISM: supernova remnants (autogen)
/ radiation mechanisms: non-thermal (autogen)},
cin = {ZEU-HESS},
ddc = {520},
cid = {I:(DE-H253)ZEU-HESS-20140213},
pnm = {613 - Matter and Radiation from the Universe (POF4-613)},
pid = {G:(DE-HGF)POF4-613},
experiment = {EXP:(DE-H253)HESS-20170101},
typ = {PUB:(DE-HGF)16},
eprint = {2201.05839},
howpublished = {arXiv:2201.05839},
archivePrefix = {arXiv},
SLACcitation = {$\%\%CITATION$ = $arXiv:2201.05839;\%\%$},
UT = {WOS:000851302600006},
doi = {10.1051/0004-6361/202243096},
url = {https://bib-pubdb1.desy.de/record/481249},
}
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