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

Author:

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

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 steadyγ-ray flux from HESS J1826−130, which appears extended with a half-width of 0.21° ± 0.02stat° ± 0.05sys°. The source spectrum is best fit with either a power-law function with a spectral index Γ = 1.78 ± 0.10stat± 0.20sysand an exponential cut-off at 15.2−3.2+5.5TeV, or a broken power-law with Γ1= 1.96 ± 0.06stat± 0.20sys, Γ2= 3.59 ± 0.69stat± 0.20sysfor energies below and aboveEbr= 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.

Publisher

EDP Sciences

Subject

Space and Planetary Science,Astronomy and Astrophysics

Cited by 17 articles. 订阅此论文施引文献 订阅此论文施引文献,注册后可以免费订阅5篇论文的施引文献,订阅后可以查看论文全部施引文献

同舟云学术

1.学者识别学者识别

2.学术分析学术分析

3.人才评估人才评估

"同舟云学术"是以全球学者为主线,采集、加工和组织学术论文而形成的新型学术文献查询和分析系统,可以对全球学者进行文献检索和人才价值评估。用户可以通过关注某些学科领域的顶尖人物而持续追踪该领域的学科进展和研究前沿。经过近期的数据扩容,当前同舟云学术共收录了国内外主流学术期刊6万余种,收集的期刊论文及会议论文总量共计约1.5亿篇,并以每天添加12000余篇中外论文的速度递增。我们也可以为用户提供个性化、定制化的学者数据。欢迎来电咨询!咨询电话:010-8811{复制后删除}0370

www.globalauthorid.com

TOP

Copyright © 2019-2024 北京同舟云网络信息技术有限公司
京公网安备11010802033243号  京ICP备18003416号-3