{"paper":{"title":"Population study of Galactic supernova remnants at very high $\\gamma$-ray energies with H.E.S.S.","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"A. Abramowski, A. A. Zdziarski, A. Balzer, A. Carosi, A. Chen, A. Djannati-Ata\\\"i, A. Donath, A. Fiasson, A. Ivascenko, A. Jacholkowska, A. Lemi\\`ere, A. Marcowith, A. M. Taylor, A. M. W. Mitchell, A. Quirrenbach, A. Reimer, A. Santangelo, A. Schulz, A. S. Seyffert, A. Viana, A. Wierzcholska, A. W\\\"ornlein, A. Zech, A. Ziegler, B. Condon, B. Giebels, B. Kh\\'elifi, B. Peyaud, B. Rudak, B. van Soelen, C. Boisson, C. B. Rulten, C. Deil, C. Farnier, C. Hoischen, C. Mariaud, C. Perennes, C. Romoli, C. Stegmann, C. Steppa, C. Trichard, C. van Eldik, C. van Rensburg, C. Venter, D. A. Sanchez, D. Berge, D. Fernandez, D. Glawion, D. Gottschall, D. Horns, D. Jankowsky, D. J. van der Walt, D. Kerszberg, D. Khangulyan, D. Klochkov, D. Malyshev, D. Prokhorov, D. Tiziani, D. Wouters, D. Zaborov, E. Leser, E. Moulin, E. O. Ang\\\"uner, F. Aharonian, F. Ait Benkhali, F. Brun, F. Gat\\'e, F. Jankowsky, F. Niederwanger, F. Rieger, F. Sch\\\"ussler, F. Spanier, F. Voisin, F. Zefi, G. Emery, G. Fontaine, G. Giavitto, G. Heinzelmann, G. Henri, G. Hermann, G. Lamanna, G. Maurin, G. Pelletier, G. P\\\"uhlhofer, G. Rowell, G. Vasileiadis, H.E.S.S. Collaboration: H. Abdalla, H. Iwasaki, H. J. V\\\"olk, H. Laffon, H. Ndiyavala, H. Odaka, H. Poon, H. Prokoph, H. Sol, I. D. Davids, I. Jung-Richardt, I. Lypova, I. Oya, I. Shilon, I. Sushch, J. A. Hinton, J. Becker Tjus, J. Bolmont, J. Bregeon, J. Chevalier, J. Conrad, J. Decock, J. Devin, J. Dyks, J. F. Glicenstein, J. Hahn, J. Hawkes, J. King, J. Lau, J. Lefaucheur, J. Niemiec, J. -P. Ernenwein, J. -P. Lees, J. -P. Lenain, J. -P. Tavernet, J. Veh, J. Vink, J. Zorn, K. Bernl\\\"ohr, K. Dutson, K. Egberts, K. Katarzy\\'nski, K. Kosack, K. Mor{\\aa}, K. Shiningayamwe, L. Dirson, L. Jouvin, L. Mohrmann, L. Oakes, L. O'C. Drury, L. Rinchiuso, \\L. Stawarz, L. Tibaldo, M. A. Kastendieck, M. Arakawa, M. Arrieta, M. Backes, M. Barnard, M. B\\\"ottcher, M. Bryan, M. B\\\"uchele, M. Capasso, M. Cerruti, M. deNaurois, M. F\\\"u{\\ss}ling, M. Haupt, M. -H. Grondin, M. Holler, M. Jamrozy, M. Jingo, M. Katsuragawa, M. Kraus, M. Lemoine-Goumard, M. Lorentz, M. Mayer, M. Meyer, M. Mohamed, M. Ostrowski, M. Padovani, M. Panter, M. Punch, M. Renaud, M. Sasaki, M. Seglar-Arroyo, M. Settimo, M. Spir-Jacob, M. Tluczykont, M. Tsirou, M. V. Fernandes, M. Zacharias, N. Chakraborty, N. Maxted, N. Shafi, N. Tsuji, Nu. Komin, N. W. Pekeur, N. \\.Zywucka, O. Reimer, P. Aubert, P. Bordas, P. Brun, P. deWilt, P. J. Meintjes, P. O\\'Brien, P. -O. Petrucci, P. P. Kr\\\"uger, P. Vincent, P. Wagner, P. Willmann, Q. Piel, R. Blackwell, R. C. G. Chaves, R. de los Reyes, R. D. Parsons, R. Liu, R. L\\'opez-Coto, R. Marx, R. Moderski, R. M. Wagner, R. Rauth, R. Schlickeiser, R. Simoni, R. Steenkamp, R. Terrier, R. Tuffs, R. White, R. Yang, R. Zanin, S. Bernhard, S. Bonnefoy, S. Caroff, S. Casanova, S. Colafrancesco, S. Eschbach, S. Fegan, S. Funk, S. Gabici, S. J. Wagner, S. Klepser, S. Krakau, S. Nakashima, S. Ohm, S. Pita, S. Raab, S. Safi-Harb, S. Saito, S. Schwemmer, T. Bulik, T. Edwards, T. Garrigoux, T. L. Holch, T. Lohse, T. Murach, T. Takahashi, T. Tavernier, T. Vuillaume, U. Katz, U. Schwanke, V. Marandon, V. Poireau, V. Sahakian, W. Hofmann, W. Klu\\'zniak, Y. A. Gallant, Y. Becherini, Y. Uchiyama, Z. Wadiasingh","submitted_at":"2018-02-14T15:56:45Z","abstract_excerpt":"Shell-type supernova remnants (SNRs) are considered prime candidates for the acceleration of Galactic cosmic rays (CRs) up to the knee of the CR spectrum at $\\mathrm{E} \\approx \\mathrm{3}\\times \\mathrm{10}^\\mathrm{15}$ eV. Our Milky Way galaxy hosts more than 350 SNRs discovered at radio wavelengths and at high energies, of which 220 fall into the H.E.S.S. Galactic Plane Survey (HGPS) region. Of those, only 50 SNRs are coincident with a H.E.S.S source and in 8 cases the very high-energy (VHE) emission is firmly identified as an SNR. The H.E.S.S. GPS provides us with a legacy for SNR population"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1802.05172","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}