Revisiting the PeVatron candidate MGRO J1908+06 with an updated H.E.S.S. analysis
On behalf of the Hess Collaboration,
H. Abdalla,
F. Aharonian,
F. Ait-Benkhali,
O. Anguener,
C. Arcaro,
C. Armand, T. Armstrong, H. Ashkar, M. Backes, V. Baghmanyan, V. Barbosa Martins, A. Barnacka, M. Barnard, R.W. Batzofin, Y. Becherini, D. Berge, K. Bernloehr, B. Bi, M. Böttcher, C. Boisson, J. Bolmont, M. Bony (de), M. Breuhaus, R. Brose, F. Brun, T. Bulik, T. Bylund, F. Cangemi, S. Caroff, S. Casanova, J. Catalano, P. Chambery, T.B. Chand, A. Chen, G. Cotter, M. Curlo, H. Dalgleish, J. Damascene Mbarubucyeye, I.D. Davids, J. Davies, J. Devin, A. Djannati-Ataï, A. Dmytriiev, A. Donath, V. Doroshenko, L. Dreyer, L. Du Plessis, C. Duffy, K. Egberts, S. Einecke, J.P. Ernenwein, S. Fegan, K. Feijen, A. Fiasson, G. Fichet de Clairfontaine, G. Fontaine, L. Frans, M. Fuessling, S. Funk, S. Gabici, Y. Gallant, G. Giavitto, L. Giunti, D. Glawion, J.F. Glicenstein, M.H. Grondin, S. Hattingh, M. Haupt, G. Hermann, J. Hinton, W. Hofmann, C. Hoischen, T. Holch, M. Holler, D. Horns, Z.Q. Huang, D. Huber, M. Hörbe, M. Jamrozy, F. Jankowsky, V. Joshi, I. Jung, E. Kasai, K. Katarzynski, U. Katz, D. Khangulyan, B. Khelifi, S. Klepser, W. Kluzniak, N. Komin, R. Konno, K. Kosack, D. Kostunin*, M. Kreter, G. Kukec Mezek, A. Kundu, G. Lamanna, S. Le Stum, A. Lemiere, M. Lemoine-Goumard, J.P. Lenain, F. Leuschner, C. Levy, T. Lohse, A. Luashvili, I. Lypova, J. Mackey, J. Majumdar, D. Malyshev, D. Malyshev, V. Marandon, P. Marchegiani, A. Marcowith, A. Mares, G. Martí-Devesa, R. Marx, G. Maurin, P. Meintjes, M. Meyer, A. Mitchell, R. Moderski, L. Mohrmann, A. Montanari, C. Moore, P. Morris, E. Moulin, J. Muller, T. Murach, K. Nakashima, M. Naurois (de), A. Nayerhoda, H. Davids, J. Niemiec, A. Noel, P. O'Brien, L.L. Oberholzer, S. Ohm, L. Olivera-Nieto, E. Ona-Wilhelmi (de), M. Ostrowski, S. Panny, M. Panter, D. Parsons, G. Peron, S. Pita, V. Poireau, D.A. Prokhorov, H. Prokoph, G. Puehlhofer, M. Punch, A. Quirrenbach, P. Reichherzer, A. Reimer, O. Reimer, Q. Remy, M. Renaud, B. Reville, F. Rieger, C. Romoli, G.P. Rowell, B. Rudak, H. Rueda Ricarte, E. Ruiz Velasco, V. Sahakian, S. Sailer, H. Salzmann, D. Sanchez, A. Santangelo, M. Sasaki, J. Schaefer, H. Schutte, U. Schwanke, F. Schüssler, M. Senniappan, A. Seyffert, J.N.S. Shapopi, K. Shiningayamwe, R. Simoni, A. Sinha, H. Sol, H. Spackman, A. Specovius, S.T. Spencer, M. Spir-Jacob, L. Stawarz, R. Steenkamp, C. Stegmann, S. Steinmassl, C. Steppa, L. Sun, T. Takahashi, T. Tanaka, T. Tavernier, A. Taylor, R. Terrier, H. Thiersen, C. Thorpe-Morgan, M. Tluczykont, L. Tomankova, M. Tsirou, N. Tsuji, R. Tuffs, Y. Uchiyama, J. van der Walt, C. van Eldik, C. van Rensburg, B. van Soelen, G. Vasileiadis, J. Veh, C. Venter, P. Vincent, J. Vink, H.J. Völk, S. Wagner, J.J. Watson, F. Werner, R. White, A. Wierzcholska, Y.W. Wong, H.M. Yassin, A. Yusafzai, M. Zacharias, R. Zanin, D. Zargaryan, A. Zdziarski, A. Zech, S. Zhu, A. Zmija, S. Zouari and N. Żywuckaet al. (click to show)*: corresponding author
Pre-published on:
July 30, 2021
Published on:
March 18, 2022
Abstract
Detecting and studying galactic gamma-ray sources emitting very-high energy photons sheds light on the acceleration and propagation of cosmic rays presumably created in these sources. Currently, there are few sources emitting photons with energies exceeding 100 TeV. In this work we revisit the unidentified source MGRO J1908+06, initially detected by Milagro, using an updated H.E.S.S. dataset and analysis pipeline. The vicinity of the source contains a supernova remnant and pulsars as well as molecular clouds. This makes the identification of the primary source(s) of galactic cosmic rays as well as the nature of the gamma-ray emission challenging, especially in light of the recent HAWC and LHAASO detection of the high energy tail of its spectrum. Exploiting the better angular resolution as compared to particle detectors, we investigate the morphology of the source as well as its spectral properties.
DOI: https://doi.org/10.22323/1.395.0779
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