{"paper":{"title":"Characterising the VHE diffuse emission in the central 200 parsecs of our Galaxy 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. Chen, A. Djannati-Ata\\\"i, A. Donath, A. Fiasson, A. F\\\"orster, A.G. Akhperjaniany, A. Goyal, A. Ivascenko, A. Jacholkowska, A. Lemi\\`ere, A. Marcowith, A.M. Taylor, A.M.W. Mitchel, 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. Degrange, 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. Trichard, C. van Eldik, C. van Rensburg, C. Venter, D.A. Sanchez, D. Berge, D. Gottschall, D. Horns, D. Jankowsky, D.J. van der Walt, D. Kerszberg, D. Khangulyan, D. Klochkov, D. Kolitzus, D. Prokhorov, D. Salek, D. Tiziani, D. Wouters, D. Zaborov, E. Leser, E. Moulin, E.O. Ang\\\"uner, F. Aharonian, F. Ait Benkhali, F. Brun, F. Jankowsky, F. Niederwanger, F. Rieger, F. Sch\\\"ussler, F. Spanier, F. Spies, F. Voisin, F. Zefi, G. Cologna, G. Fontaine, G. Giavitto, G. Heinzelmann, G. Henri, G. Hermann, G. Lamanna, G. Maurin, G. Pelletier, G. P\\\"uhlhofer, G. Rowell, G. Spengler, G. Vasileiadis, H.E.S.S. Collaboration: H. Abdalla, H. Iwasaki, H.J. V\\\"olk, H. Laffon, 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. Carr, 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, K. Bernl\\\"ohr, K. Dutson, K. Egberts, K. Katarzynski, K. Kosack, K. Mor{\\aa}, K. Stycz, L. Dirson, L. Jouvin, L. Mohrmann, L. Oakes, L.O.C. Drury, 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. Coffaro, M. de Naurois, M. F\\\"u{\\ss}ling, M. Haupt, M.H. Grondin, M. Holler, M. Jamrozy, M. Janiak, 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. Tluczykont, 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. Eger, 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. Lopez-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. Casanova, S. Colafrancesco, S. Eschbach, S. Fegan, S. Funk, S. Gabici, S.J. Wagner, S. Klepser, S. Krakau1, S. Nakashima, S. Ohm, S. Pita, S. Raab, S. Richter, S. Saito, S. Schwemmer, T. Andersson, T. Bulik, T. Edwards, T. Garrigoux, T. Jogler, T. L. Holch, T. Lohse, T. Murach, T. Takahashi, T. Tavernier, T. Vuillaume, U. Katz, U. Schwanke, V. Lefranc, V. Marandon, V. Sahakian, W. Domainko, W. Hofmann, W. Kluzniak, Y.A. Gallant, Y. Becherini, Y. Cui, Y. Uchiyama, Z. Wadiasingh","submitted_at":"2017-06-14T15:29:16Z","abstract_excerpt":"The diffuse very high-energy (VHE, > 100 GeV) gamma-ray emission observed in the central 200 pc of the Milky Way by H.E.S.S. was found to follow the dense matter distribution in the Central Molecular Zone (CMZ) up to a longitudinal distance of about 130 pc to the Galactic Centre (GC), where the flux rapidly decreases. Recent sensitive H.E.S.S. analysis revealed that the cosmic-ray (CR) density profile drops with the distance to the centre, making data compatible with a steady cosmic PeVatron at the GC. In this paper, we extend this analysis to obtain for the first time a detailed characterisat"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1706.04535","kind":"arxiv","version":1},"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"}