LMC N132D: A mature supernova remnant with a power-law gamma-ray spectrum extending beyond 8 TeV
Creators: name: Collaboration, H. E. S. S.
name: :
name: Abdalla, H.
name: Aharonian, F.
name: Benkhali, F. Ait
name: Angüner, E. O.
name: Arcaro, C.
name: Armand, C.
name: Armstrong, T.
name: Ashkar, H.
name: Backes, M.
name: Baghmanyan, V.
name: Martins, V. Barbosa
name: Barnacka, A.
name: Barnard, M.
name: Becherini, Y.
name: Berge, D.
name: Bernlöhr, K.
name: Bi, B.
name: Böttcher, M.
name: Boisson, C.
name: Bolmont, J.
name: de Lavergne, M. de Bony
name: Breuhaus, M.
name: Brun, F.
name: Brun, P.
name: Bryan, M.
name: Büchele, M.
name: Bulik, T.
name: Bylund, T.
name: Caroff, S.
name: Carosi, A.
name: Casanova, S.
name: Chand, T.
name: Chandra, S.
name: Chen, A.
name: Cotter, G.
name: Curyło, M.
name: Mbarubucyeye, J. Damascene
name: Davids, I. D.
name: Davies, J.
name: Deil, C.
name: Devin, J.
name: Dirson, L.
name: Djannati-Atai, A.
name: Dmytriiev, A.
name: Donath, A.
name: Doroshenko, V.
name: Dreyer, L.
name: Duffy, C.
name: Dyks, J.
name: Egberts, K.
name: Eichhorn, F.
name: Einecke, S.
name: Emery, G.
name: Ernenwein, J. -P.
name: Feijen, K.
name: Fegan, S.
name: Fiasson, A.
name: de Clairfontaine, G. Fichet
name: Fontaine, G.
name: Funk, S.
name: Füßling, M.
name: Gabici, S.
name: Gallant, Y. A.
name: Giavitto, G.
name: Giunti, L.
name: Glawion, D.
name: Glicenstein, J. F.
name: Grondin, M. -H.
name: Hahn, J.
name: Haupt, M.
name: Hermann, G.
name: Hinton, J. A.
name: Hofmann, W.
name: Hoischen, C.
name: Holch, T. L.
name: Holler, M.
name: Hörbe, M.
name: Horns, D.
name: Huber, D.
name: Jamrozy, M.
name: Jankowsky, D.
name: Jankowsky, F.
name: Jardin-Blicq, A.
name: Joshi, V.
name: Jung-Richardt, I.
name: Kasai, E.
name: Kastendieck, M. A.
name: Katarzynski, K.
name: Katz, U.
name: Khangulyan, D.
name: Khélifi, B.
name: Klepser, S.
name: Kluźniak, W.
name: Komin, Nu.
name: Konno, R.
name: Kosack, K.
name: Kostunin, D.
name: Kreter, M.
name: Lamanna, G.
name: Lemière, A.
name: Lemoine-Goumard, M.
name: Lenain, J. -P.
name: Leuschner, F.
name: Levy, C.
name: Lohse, T.
name: Lypova, I.
name: Mackey, J.
name: Majumdar, J.
name: Malyshev, D.
name: Malyshev, D.
name: Marandon, V.
name: Marchegiani, P.
name: Marcowith, A.
name: Mares, A.
name: Martí-Devesa, G.
name: Marx, R.
name: Maurin, G.
name: Meintjes, P. J.
name: Meyer, M.
name: Mitchell, A.
name: Moderski, R.
name: Mohrmann, L.
name: Montanari, A.
name: Moore, C.
name: Morris, P.
name: Moulin, E.
name: Muller, J.
name: Murach, T.
name: Nakashima, K.
name: Nayerhoda, A.
name: de Naurois, M.
name: Ndiyavala, H.
name: Niemiec, J.
name: Oakes, L.
name: O'Brien, P.
name: Odaka, H.
name: Ohm, S.
name: Olivera-Nieto, L.
name: Wilhelmi, E. de Ona
name: Ostrowski, M.
name: Panny, S.
name: Panter, M.
name: Parsons, R. D.
name: Peron, G.
name: Peyaud, B.
name: Piel, Q.
name: Pita, S.
name: Poireau, V.
name: Noel, A. Priyana
name: Prokhorov, D. A.
name: Prokoph, H.
name: Pühlhofer, G.
name: Punch, M.
name: Quirrenbach, A.
name: Raab, S.
name: Rauth, R.
name: Reichherzer, P.
name: Reimer, A.
name: Reimer, O.
name: Remy, Q.
name: Renaud, M.
name: Rieger, F.
name: Rinchiuso, L.
name: Romoli, C.
name: Rowell, G.
name: Rudak, B.
name: Ruiz-Velasco, E.
name: Sahakian, V.
name: Sailer, S.
name: Salzmann, H.
name: Sanchez, D. A.
name: Santangelo, A.
name: Sasaki, M.
name: Scalici, M.
name: Schäfer, J.
name: Schüssler, F.
name: Schutte, H. M.
name: Schwanke, U.
name: Seglar-Arroyo, M.
name: Senniappan, M.
name: Seyffert, A. S.
name: Shafi, N.
name: Shapopi, J. N. S.
name: Shiningayamwe, K.
name: Simoni, R.
name: Sinha, A.
name: Sol, H.
name: Specovius, A.
name: Spencer, S.
name: Spir-Jacob, M.
name: Stawarz, L.
name: Sun, L.
name: Steenkamp, R.
name: Stegmann, C.
name: Steinmassl, S.
name: Steppa, C.
name: Takahashi, T.
name: Tavernier, T.
name: Taylor, A. M.
name: Terrier, R.
name: Thiersen, J. H. E.
name: Tiziani, D.
name: Tluczykont, M.
name: Tomankova, L.
name: Trichard, C.
name: Tsirou, M.
name: Tuffs, R.
name: Uchiyama, Y.
name: van der Walt, D. J.
name: van Eldik, C.
name: van Rensburg, C.
name: van Soelen, B.
name: Vasileiadis, G.
name: Veh, J.
name: Venter, C.
name: Vincent, P.
name: Vink, J.
name: Völk, H. J.
name: Wadiasingh, Z.
name: Wagner, S. J.
name: Watson, J.
name: Werner, F.
name: White, R.
name: Wierzcholska, A.
name: Wong, Yu Wun
name: Yusafzai, A.
name: Zacharias, M.
name: Zanin, R.
name: Zargaryan, D.
name: Zdziarski, A. A.
name: Zech, A.
name: Zhu, S. J.
name: Zorn, J.
name: Zouari, S.
name: Żywucka, N.
Publisher: name: arXiv
Year: 2021
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We analyzed 252 hours of High Energy Stereoscopic System (H.E.S.S.) observations towards the supernova remnant (SNR) LMC N132D that were accumulated between December 2004 and March 2016 during a deep survey of the Large Magellanic Cloud, adding 104 hours of observations to the previously published data set to ensure a &gt; 5 sigma detection. To broaden the gamma-ray spectral coverage required for modeling the spectral energy distribution, an analysis of Fermi-LAT Pass 8 data was also included. We unambiguously detect N132D at very high energies (VHE) with a significance of 5.7 sigma. We report the results of a detailed analysis of its spectrum and localization based on the extended H.E.S.S. data set. The joint analysis of the extended H.E.S.S and Fermi-LAT data results in a spectral energy distribution in the energy range from 1.7 GeV to 14.8 TeV, which suggests a high luminosity of N132D at GeV and TeV energies. We set a lower limit on a gamma-ray cutoff energy of 8 TeV with a confidence level of 95%. The new gamma-ray spectrum as well as multiwavelength observations of N132D when compared to physical models suggests a hadronic origin of the VHE gamma-ray emission. SNR N132D is a VHE gamma-ray source that shows a spectrum extending to the VHE domain without a spectral cutoff at a few TeV, unlike the younger oxygen-rich SNR Cassiopeia A. The gamma-ray properties of N132D may be affected by an interaction with a nearby molecular cloud that partially lies inside the 95% confidence region of the source position. [Abridged]
description: Accepted for publication in Astronomy &amp; Astrophysics