H.E.S.S. ToO program on nearby core-collapse Supernovae : search for very-high energy γ-ray emission towards the SN candidate AT2019krl in M74
- 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, Anna
- 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, Marek
- 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.
- 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, Angel
- O'Brien, P.
- Oberholzer, L. L.
- Ohm, S.
- Olivera-Nieto, L.
- Ona-Wilhelmi (de), E.
- Ostrowski, Michał
- 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, Łukasz
- 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, Alicja
- 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.
DOIAbstract
While the youngest known supernova remnants (SNRs), such as Cassiopeia A (Cas A), have been proven to be able to accelerate cosmic rays (CRs) only up to ∼ 10$^{14}$ eV at their present evolutionary stages, recent studies have shown that particle energies larger than a few PeV (10$^{15}$ eV) could be reached during the early stages of a core-collapse Supernova (cc-SN), when the high-velocity forward shock expands into the dense circumstellar medium (CSM) 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$_{\bigodot}$ yr$^{-1}$, could thus lead to γ-ray emission from $\pi ^{0}$ decay in hadronic interactions, potentially detectable with ...
Add to ORKG