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An extreme particle accelerator in the Galactic plane: HESS J1826−130

H. Abdalla R. Adam 1 F. Aharonian F. Ait Benkhali E.O. Angüner 2 C. Arcaro C. Armand 3 T. Armstrong H. Ashkar M. Backes V. Baghmanyan V. Barbosa Martins A. Barnacka M. Barnard Y. Becherini D. Berge K. Bernlöhr B. Bi M. Böttcher C. Boisson 4 J. Bolmont 1 M. de Bony de Lavergne 3 P. Bordas M. Breuhaus F. Brun P. Brun M. Bryan M. Büchele T. Bulik T. Bylund S. Caroff 1 A. Carosi 3 S. Casanova T. Chand S. Chandra A. Chen G. Cotter M. Curyło J. Damascene Mbarubucyeye I. Davids J. Davies C. Deil J. Devin 5 P. Dewilt L. Dirson A. Djannati-Ataï 6 A. Dmytriiev 4 A. Donath V. Doroshenko C. Duffy J. Dyks K. Egberts F. Eichhorn S. Einecke G. Emery 1 J.-P. Ernenwein 2 K. Feijen S. Fegan 1 A. Fiasson 3 G. Fichet de Clairfontaine 4 G. Fontaine 1 S. Funk M. Füßling S. Gabici 6 Y. Gallant 7 G. Giavitto L. Giunti D. Glawion J. Glicenstein D. Gottschall M.-H. Grondin 5 J. Hahn M. Haupt G. Hermann J. Hinton W. Hofmann C. Hoischen T. Holch M. Holler M. Hörbe D. Horns D. Huber M. Jamrozy D. Jankowsky F. Jankowsky A. Jardin-Blicq V. Joshi I. Jung-Richardt E. Kasai M. Kastendieck K. Katarzyński U. Katz D. Khangulyan B. Khélifi 6 S. Klepser W. Kluźniak Nu. Komin R. Konno K. Kosack D. Kostunin M. Kreter G. Lamanna 3 A. Lemière 6 M. Lemoine-Goumard 5 J.-P. Lenain 1 C. Levy 1 T. Lohse I. Lypova J. Mackey J. Majumdar D. Malyshev V. Marandon ¶. Marchegiani Alexandre Marcowith 7 A. Mares 5 G. Martí-Devesa R. Marx G. Maurin 3 P. Meintjes M. Meyer A. Mitchell R. Moderski M. Mohamed L. Mohrmann A. Montanari C. Moore P. Morris E. Moulin J. Muller 1 T. Murach K. Nakashima A. Nayerhoda M. de Naurois 1 H. Ndiyavala F. Niederwanger J. Niemiec L. Oakes P. O’brien H. Odaka S. Ohm L. Olivera-Nieto E. de Ona Wilhelmi M. Ostrowski I. Oya M. Panter S. Panny R. Parsons G. Peron B. Peyaud Q. Piel 3 S. Pita 6 V. Poireau 3 A. Priyana Noel D. Prokhorov H. Prokoph G. Pühlhofer M. Punch 6 A. Quirrenbach S. Raab R. Rauth P. Reichherzer A. Reimer O. Reimer Q. Remy Matthieu Renaud 7 F. Rieger L. Rinchiuso C. Romoli G. Rowell B. Rudak E. Ruiz-Velasco V. Sahakian S. Sailer D. Sanchez 3 A. Santangelo M. Sasaki M. Scalici F. Schüssler H. Schutte U. Schwanke S. Schwemmer M. Seglar-Arroyo M. Senniappan A. Seyffert N. Shafi K. Shiningayamwe R. Simoni A. Sinha 6 H. Sol 4 A. Specovius S. Spencer M. Spir-Jacob 6 Ł. Stawarz L. Sun R. Steenkamp C. Stegmann S. Steinmassl C. Steppa T. Takahashi T. Tavernier A. Taylor R. Terrier 6 D. Tiziani M. Tluczykont L. Tomankova C. Trichard 1 M. Tsirou 7 R. Tuffs Y. Uchiyama D. van der Walt C. van Eldik C. van Rensburg B. van Soelen George Vasileiadis 7 J. Veh C. Venter P. Vincent 1 J. Vink H. Völk T. Vuillaume 3 Z. Wadiasingh S. Wagner J. Watson F. Werner R. White A. Wierzcholska Yu Wun Wong A. Yusafzai M. Zacharias 4 R. Zanin D. Zargaryan A. Zdziarski A. Zech 4 S. Zhu A. Ziegler J. Zorn S. Zouari 6 N. Żywucka
Abstract : 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.
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H. Abdalla, R. Adam, F. Aharonian, F. Ait Benkhali, E.O. Angüner, et al.. An extreme particle accelerator in the Galactic plane: HESS J1826−130. Astronomy and Astrophysics - A&A, EDP Sciences, 2020, 644, pp.A112. ⟨10.1051/0004-6361/202038851⟩. ⟨hal-03371639⟩

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