Evidence for $\gamma$-ray emission from the remnant of Kepler’s supernova based on deep H.E.S.S. observations

Aharonian, F.; White, R.; Boisson, C.; Zhu, Sylvia Jiechen; H. E. S. S. Collaboration; Rowell, G.; Moulin, E.; Nayerhoda, A.; Unbehaun, T.; Kluzniak, W.; Rieger, F.; Khelifi, B.; Benkhali, F. Ait; Devin, J.; Simoni, R.; Shapopi, J. N. S.; Lemoine-Goumard, M.; Marx, R.; Bolmont, J.; Montanari, A.; Berge, D.; Einecke, S.; Schussler, F.; Lohse, T.; Martins, V. Barbosa; Schwanke, U.; Wong, Yu Wun; Grondin, M.-H.; Kostunin, D.; Meintjes, P. J.; Cristofari, P.; O'Brien, P.; Sanchez, D. A.; Chibueze, O.; Reichherzer, P.; Sushch, I.; Holler, M.; Backes, M.; Uchiyama, Y.; Steppa, C.; Punch, M.; Bernloehr, K.; Holch, Tim Lukas; Glawion, D.; Prokhorov, D. A.; Poireau, V.; Santangelo, A.; Peron, G.; Wagner, S. J.; Egberts, K.; Ghafourizadeh, S.; Yusafzai, A.; Marchegiani, P.; Marcowith, A.; Steinmassl, S.; Zywucka, N.; Chand, T.; Bulik, T.; Cotter, G.; Nakashima, K.; Rudak, B.; Katz, U.; Meyer, M.; Kasai, E.; Brose, R.; Lemiere, A.; Reimer, O.; Quirrenbach, A.; Takahashi, T.; Fontaine, G.; Sol, H.; Giunti, L.; Noel, A. Priyana; Tsirou, M.; Schutte, H. M.; Terrier, R.; Veh, J.; Katarzynski, K.; Funk, S.; Mbarubucyeye, Jean Damascene; Reimer, A.; Olivera-Nieto, L.; Jung-Richardt, I.; Feijen, K.; Salzmann, H.; Dmytriiev, A.; Huang, Zhiqiu; Zargaryan, D.; Taylor, A. M.; Anguner, E. O.; Muller, J.; de Naurois, M.; Giavitto, Gianluca; Parsons, R. D.; Moderski, R.; de Lavergne, M. de Bony; Vink, J.; Chen, A.; Casanova, S.; Hoerbe, M.; Sailer, S.; Ashkar, H.; Gallant, Y. A.; Mackey, J.; Zouari, S.; Joshi, V.; Hofmann, W.; Marandon, V.; Reville, B.; Panny, S.; Niemiec, J.; Ostrowski, M.; Ohm, Stefan; Sasaki, M.; Caroff, S.; Brun, F.; Fiasson, A.; Leuschner, F.; Komin, Nu.; Cangemi, F.; Schafer, J.; Ricarte, H. Rueda; de Clairfontaine, G. Fichet; Zech, A.; Batzofin, R.; Jamrozy, M.; van Eldik, C.; Maurin, G.; Voelk, H. J.; Werner, F.; Mohrmann, L.; Mitchell, A.; Malyshev, D.; Horns, D.; Ernenwein, J.-P.; Boettcher, M.; Lenain, J.-P.; Bylund, T.; Kosack, K.; Puehlhofer, G.; Breuhaus, M.; Zdziarski, A. A.; Wierzcholska, A.; Wilhelmi, E. de Ona; Becherini, Y.; Gabici, S.; Glicenstein, J. F.; Stawarz, L.; Specovius, A.; Cerruti, M.; Luashvili, A.; Spencer, S.; Renaud, M.; Zacharias, M.; Tanaka, T.; Sahakian, V.; Lypova, I.; Djannati-Atai, A.; Panter, M.; Marti-Devesa, G.

doi:10.1051/0004-6361/202243096

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000481249 0247_ $$2arXiv$$aarXiv:2201.05839
000481249 0247_ $$2datacite_doi$$a10.3204/PUBDB-2022-04260
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000481249 041__ $$aEnglish
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000481249 088__ $$2arXiv$$aarXiv:2201.05839
000481249 1001_ $$0F.Aharonian.1$$aAharonian, F.$$b0
000481249 245__ $$aEvidence for $\gamma$-ray emission from the remnant of Kepler’s supernova based on deep H.E.S.S. observations
000481249 260__ $$aLes Ulis$$bEDP Sciences$$c2022
000481249 3367_ $$2DRIVER$$aarticle
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000481249 520__ $$aObservations with imaging atmospheric Cherenkov telescopes (IACTs) have enhanced our knowledge of nearby supernova (SN) remnants with ages younger than 500 yr by establishing Cassiopeia A and the remnant of Tycho’s SN as very-high-energy (VHE) γ-ray sources. The remnant of Kepler’s SN, which is the product of the most recent naked-eye SN in our Galaxy, is comparable in age to the other two, but is significantly more distant. If the γ-ray luminosities of the remnants of Tycho’s and Kepler’s SNe are similar, then the latter is expected to be one of the faintest γ-ray sources within reach of the current generation IACT arrays. Here we report evidence at a statistical level of 4.6σ for a VHE signal from the remnant of Kepler’s SN based on deep observations by the High Energy Stereoscopic System (H.E.S.S.) with an exposure of 152 h. The measured integral flux above an energy of 226 GeV is ∼0.3% of the flux of the Crab Nebula. The spectral energy distribution (SED) reveals a γ-ray emitting component connecting the VHE emission observed with H.E.S.S. to the emission observed at GeV energies with Fermi-LAT. The overall SED is similar to that of the remnant of Tycho’s SN, possibly indicating the same nonthermal emission processes acting in both these young remnants of thermonuclear SNe.
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000481249 650_7 $$2INSPIRE$$agamma ray: emission
000481249 650_7 $$2INSPIRE$$aenergy: high
000481249 650_7 $$2INSPIRE$$aCherenkov counter: atmosphere
000481249 650_7 $$2INSPIRE$$asupernova
000481249 650_7 $$2INSPIRE$$aenergy spectrum
000481249 650_7 $$2INSPIRE$$aVHE
000481249 650_7 $$2INSPIRE$$aHESS
000481249 650_7 $$2INSPIRE$$aGeV
000481249 650_7 $$2INSPIRE$$aflux
000481249 650_7 $$2INSPIRE$$aspectral
000481249 650_7 $$2INSPIRE$$aimaging
000481249 650_7 $$2INSPIRE$$aGLAST
000481249 650_7 $$2INSPIRE$$astatistical
000481249 650_7 $$2INSPIRE$$agalaxy
000481249 650_7 $$2autogen$$agamma rays: general
000481249 650_7 $$2autogen$$asupernovae: individual: Kepler
000481249 650_7 $$2autogen$$agamma-rays: general
000481249 650_7 $$2autogen$$asupernovae: individual: Kepler’s SN
000481249 650_7 $$2autogen$$aISM: supernova remnants
000481249 650_7 $$2autogen$$aradiation mechanisms: non-thermal
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