E-viri
PDF
Recenzirano
Odprti dostop
-
Aharonian, F.; Angüner, E.O.; Armand, C.; Barbosa Martins, V.; Barnacka, A.; Barnard, M.; Becherini, Y.; Boisson, C.; Bordas, P.; Breuhaus, M.; Bryan, M.; Caroff, S.; Carosi, A.; Chand, T.; Chandra, S.; Damascene Mbarubucyeye, J.; Davids, I. D.; Davies, J.; Deil, C.; Devin, J.; Dirson, L.; Donath, A.; Egberts, K.; Eichhorn, F.; Emery, G.; Fichet de Clairfontaine, G.; Füßling, M.; Gabici, S.; Giavitto, G.; Holch, T. L.; Hörbe, M.; Horns, D.; Huber, D.; Jamrozy, M.; Jankowsky, F.; Jardin-Blicq, A.; Joshi, V.; Kasai, E.; Katarzyński, K.; Katz, U.; Khélifi, B.; Klepser, S.; Komin, Nu; Lamanna, G.; Levy, C.; Lohse, T.; Malyshev, D.; Marcowith, A.; Mares, A.; Meyer, M.; Mitchell, A.; Moderski, R.; Moore, C.; de Naurois, M.; Niederwanger, F.; Niemiec, J.; Oakes, L.; O’Brien, P.; Olivera-Nieto, L.; de Ona Wilhelmi, E.; Parsons, R. D.; Peron, G.; Pita, S.; Priyana Noel, A.; Prokhorov, D. A.; Quirrenbach, A.; Renaud, M.; Sailer, S.; Santangelo, A.; Schüssler, F.; Schwanke, U.; Schwemmer, S.; Seyffert, A. S.; Simoni, R.; Sinha, A.; Spir-Jacob, M.; Steinmassl, S.; Steppa, C.; Takahashi, T.; Tavernier, T.; Terrier, R.; Tiziani, D.; Tomankova, L.; van Eldik, C.; van Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Venter, C.; Vincent, P.; Völk, H. J.; Vuillaume, T.; Wagner, S. J.; White, R.; Wierzcholska, A.; Zanin, R.; Zargaryan, D.; Zech, A.; Zhu, S. J.; Zorn, J.; Żywucka, N.
Astronomy and astrophysics (Berlin), 12/2020, Letnik: 644Journal Article
The unidentified very-high-energy (VHE; E > 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° ± 0.02 stat ° ± 0.05 sys °. The source spectrum is best fit with either a power-law function with a spectral index Γ = 1.78 ± 0.10 stat ± 0.20 sys and an exponential cut-off at 15.2 −3.2 +5.5 TeV, or a broken power-law with Γ 1 = 1.96 ± 0.06 stat ± 0.20 sys , Γ 2 = 3.59 ± 0.69 stat ± 0.20 sys for energies below and above E br = 11.2 ± 2.7 TeV, respectively. The VHE flux from HESS J1826−130 is contaminated by the extended emission of the bright, nearby pulsar wind nebula, 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 ≳200 TeV. Our results are also discussed in a multiwavelength context, accounting for both the presence of nearby supernova remnants, molecular clouds, and counterparts detected in radio, X-rays, and TeV energies.
