%0 Journal Article
%A Aharonian, F.
%A Benkhali, F. Ait
%A Anguner, E. O.
%A Ashkar, H.
%A Backes, M.
%A Martins, V. Barbosa
%A Batzofin, R.
%A Becherini, Y.
%A Berge, D.
%A Bernloehr, K.
%A Boettcher, M.
%A Boisson, C.
%A Bolmont, J.
%A de Lavergne, M. de Bony
%A Breuhaus, M.
%A Brose, R.
%A Brun, F.
%A Bulik, T.
%A Bylund, T.
%A Cangemi, F.
%A Caroff, S.
%A Casanova, S.
%A Cerruti, M.
%A Chand, T.
%A Chen, A.
%A Chibueze, O.
%A Cotter, G.
%A Cristofari, P.
%A Mbarubucyeye, Jean Damascene
%A Devin, J.
%A Djannati-Atai, A.
%A Dmytriiev, A.
%A Egberts, K.
%A Einecke, S.
%A Ernenwein, J.-P.
%A Feijen, K.
%A Fiasson, A.
%A de Clairfontaine, G. Fichet
%A Fontaine, G.
%A Funk, S.
%A Gabici, S.
%A Gallant, Y. A.
%A Ghafourizadeh, S.
%A Giavitto, Gianluca
%A Giunti, L.
%A Glawion, D.
%A Glicenstein, J. F.
%A Grondin, M.-H.
%A Hoerbe, M.
%A Hofmann, W.
%A Holch, Tim Lukas
%A Holler, M.
%A Horns, D.
%A Huang, Zhiqiu
%A Jamrozy, M.
%A Joshi, V.
%A Jung-Richardt, I.
%A Kasai, E.
%A Katarzynski, K.
%A Katz, U.
%A Khelifi, B.
%A Kluzniak, W.
%A Komin, Nu.
%A Kosack, K.
%A Kostunin, D.
%A Lemiere, A.
%A Lemoine-Goumard, M.
%A Lenain, J.-P.
%A Leuschner, F.
%A Lohse, T.
%A Luashvili, A.
%A Lypova, I.
%A Mackey, J.
%A Malyshev, D.
%A Marandon, V.
%A Marchegiani, P.
%A Marcowith, A.
%A Marti-Devesa, G.
%A Marx, R.
%A Maurin, G.
%A Meintjes, P. J.
%A Meyer, M.
%A Mitchell, A.
%A Moderski, R.
%A Mohrmann, L.
%A Montanari, A.
%A Moulin, E.
%A Muller, J.
%A Nakashima, K.
%A de Naurois, M.
%A Nayerhoda, A.
%A Niemiec, J.
%A Noel, A. Priyana
%A O'Brien, P.
%A Ohm, Stefan
%A Olivera-Nieto, L.
%A Wilhelmi, E. de Ona
%A Ostrowski, M.
%A Panny, S.
%A Panter, M.
%A Parsons, R. D.
%A Peron, G.
%A Poireau, V.
%A Prokhorov, D. A.
%A Puehlhofer, G.
%A Punch, M.
%A Quirrenbach, A.
%A Reichherzer, P.
%A Reimer, A.
%A Reimer, O.
%A Renaud, M.
%A Reville, B.
%A Rieger, F.
%A Rowell, G.
%A Rudak, B.
%A Ricarte, H. Rueda
%A Sahakian, V.
%A Sailer, S.
%A Salzmann, H.
%A Sanchez, D. A.
%A Santangelo, A.
%A Sasaki, M.
%A Schafer, J.
%A Schussler, F.
%A Schutte, H. M.
%A Schwanke, U.
%A Shapopi, J. N. S.
%A Simoni, R.
%A Sol, H.
%A Specovius, A.
%A Spencer, S.
%A Stawarz, L.
%A Steinmassl, S.
%A Steppa, C.
%A Sushch, I.
%A Takahashi, T.
%A Tanaka, T.
%A Taylor, A. M.
%A Terrier, R.
%A Tsirou, M.
%A Uchiyama, Y.
%A Unbehaun, T.
%A van Eldik, C.
%A Veh, J.
%A Vink, J.
%A Voelk, H. J.
%A Wagner, S. J.
%A Werner, F.
%A White, R.
%A Wierzcholska, A.
%A Wong, Yu Wun
%A Yusafzai, A.
%A Zacharias, M.
%A Zargaryan, D.
%A Zdziarski, A. A.
%A Zech, A.
%A Zhu, Sylvia Jiechen
%A Zouari, S.
%A Zywucka, N.
%T Evidence for γ-ray emission from the remnant of Kepler’s supernova based on deep H.E.S.S. observations
%J Astronomy and astrophysics
%V 662
%N arXiv:2201.05839
%@ 0004-6361
%C Les Ulis
%I EDP Sciences
%M PUBDB-2022-04260
%M arXiv:2201.05839
%P A65 
%D 2022
%X 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
%K gamma ray: emission (INSPIRE)
%K energy: high (INSPIRE)
%K Cherenkov counter: atmosphere (INSPIRE)
%K supernova (INSPIRE)
%K energy spectrum (INSPIRE)
%K VHE (INSPIRE)
%K HESS (INSPIRE)
%K GeV (INSPIRE)
%K flux (INSPIRE)
%K spectral (INSPIRE)
%K imaging (INSPIRE)
%K GLAST (INSPIRE)
%K statistical (INSPIRE)
%K galaxy (INSPIRE)
%K gamma rays: general (autogen)
%K supernovae: individual: Kepler (autogen)
%K gamma-rays: general (autogen)
%K supernovae: individual: Kepler’s SN (autogen)
%K ISM: supernova remnants (autogen)
%K radiation mechanisms: non-thermal (autogen)
%F PUB:(DE-HGF)16
%9 Journal Article
%U <Go to ISI:>//WOS:000851302600006
%R 10.1051/0004-6361/202243096
%U https://bib-pubdb1.desy.de/record/481249