An extreme particle accelerator in the Galactic plane: HESS J1826$-$130
Creators: name: Collaboration, H. E. S. S.
name: Abdalla, H.
name: Adam, R.
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: Bordas, P.
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: deWilt, P.
name: Dirson, L.
name: Djannati-Ataï, A.
name: Dmytriiev, A.
name: Donath, A.
name: Doroshenko, V.
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: Gottschall, D.
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: Katarzyński, 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: 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: Mohamed, M.
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: Niederwanger, F.
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: Oya, I.
name: Panter, M.
name: Panny, S.
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: Sanchez, D. A.
name: Santangelo, A.
name: Sasaki, M.
name: Scalici, M.
name: Schüssler, F.
name: Schutte, H. M.
name: Schwanke, U.
name: Schwemmer, S.
name: Seglar-Arroyo, M.
name: Senniappan, M.
name: Seyffert, A. S.
name: Shafi, N.
name: Shiningayamwe, K.
name: Simoni, R.
name: Sinha, A.
name: Sol, H.
name: Specovius, A.
name: Spencer, S.
name: Spir-Jacob, M.
name: Stawarz, Ł.
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: 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: Vuillaume, T.
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: Ziegler, A.
name: Zorn, J.
name: Zouari, S.
name: Żywucka, N.
Publisher: name: arXiv
Year: 2020
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: The unidentified very-high-energy (VHE; E $&gt;$ 0.1 TeV) $γ$-ray source, HESS J1826$-$130, was discovered with the High Energy Stereoscopic System (HESS) in the Galactic plane. The analysis of 215 h of HESS data has revealed a steady $γ$-ray flux from HESS J1826$-$130, which appears extended with a half-width of 0.21$^{\circ}$ $\pm$ 0.02$^{\circ}_{\text{stat}}$ $\pm$ 0.05$^{\circ}_{\text{sys}}$. The source spectrum is best fit with either a power-law function with a spectral index $Γ$ = 1.78 $\pm$ 0.10$_{\text{stat}}$ $\pm$ 0.20$_{\text{sys}}$ and an exponential cut-off at 15.2$^{+5.5}_{-3.2}$ TeV, or a broken power-law with $Γ_{1}$ = 1.96 $\pm$ 0.06$_{\text{stat}}$ $\pm$ 0.20$_{\text{sys}}$, $Γ_{2}$ = 3.59 $\pm$ 0.69$_{\text{stat}}$ $\pm$ 0.20$_{\text{sys}}$ for energies below and above $E_{\rm{br}}$ = 11.2 $\pm$ 2.7 TeV, respectively. The VHE flux from HESS J1826$-$130 is contaminated by the extended emission of the bright, nearby pulsar wind nebula (PWN), HESS J1825$-$137, particularly at the low end of the energy spectrum. Leptonic scenarios for the origin of HESS J1826$-$130 VHE emission related to PSR J1826$-$1256 are confronted by our spectral and morphological analysis. In a hadronic framework, taking into account the properties of dense gas regions surrounding HESS J1826$-$130, the source spectrum would imply an astrophysical object capable of accelerating the parent particle population up to $\gtrsim$200 TeV. Our results are also discussed in a multiwavelength context, accounting for both the presence of nearby supernova remnants (SNRs), molecular clouds, and counterparts detected in radio, X-rays, and TeV energies.
description: 9 Pages, 5 Figures