HESS J1741−302: a hidden accelerator in the Galactic plane

Author:

,Abdalla H.,Abramowski A.,Aharonian F.,Ait Benkhali F.,Angüner E. O.,Arakawa M.,Armand C.,Arrieta M.,Backes M.,Balzer A.,Barnard M.,Becherini Y.,Becker Tjus J.,Berge D.,Bernhard S.,Bernlöhr K.,Blackwell R.,Böttcher M.,Boisson C.,Bolmont J.,Bonnefoy S.,Bordas P.,Bregeon J.,Brun F.,Brun P.,Bryan M.,Büchele M.,Bulik T.,Capasso M.,Caroff S.,Carosi A.,Casanova S.,Cerruti M.,Chakraborty N.,Chaves R. C. G.,Chen A.,Chevalier J.,Colafrancesco S.,Condon B.,Conrad J.,Davids I. D.,Decock J.,Deil C.,Devin J.,deWilt P.,Dirson L.,Djannati-Ataï A.,Donath A.,Drury L.O’C.,Dyks J.,Edwards T.,Egberts K.,Emery G.,Ernenwein J.-P.,Eschbach S.,Farnier C.,Fegan S.,Fernandes M. V.,Fiasson A.,Fontaine G.,Funk S.,Füßling M.,Gabici S.,Gallant Y. A.,Garrigoux T.,Gaté F.,Giavitto G.,Glawion D.,Glicenstein J. F.,Gottschall D.,Grondin M.-H.,Hahn J.,Haupt M.,Hawkes J.,Heinzelmann G.,Henri G.,Hermann G.,Hinton J. A.,Hofmann W.,Hoischen C.,Holch T. L.,Holler M.,Horns D.,Ivascenko A.,Iwasaki H.,Jacholkowska A.,Jamrozy M.,Jankowsky D.,Jankowsky F.,Jingo M.,Jouvin L.,Jung-Richardt I.,Kastendieck M. A.,Katarzyński K.,Katsuragawa M.,Katz U.,Kerszberg D.,Khangulyan D.,Khélifi B.,King J.,Klepser S.,Klochkov D.,Kluźniak W.,Komin Nu.,Kosack K.,Krakau S.,Kraus M.,Krüger P. P.,Laffon H.,Lamanna G.,Lau J.,Lefaucheur J.,Lemière A.,Lemoine-Goumard M.,Lenain J.-P.,Leser E.,Lohse T.,Lorentz M.,Liu R.,López-Coto R.,Lypova I.,Malyshev D.,Marandon V.,Marcowith A.,Mariaud C.,Marx R.,Maurin G.,Maxted N.,Mayer M.,Meintjes P. J.,Meyer M.,Mitchell A. M. W.,Moderski R.,Mohamed M.,Mohrmann L.,Morå K.,Moulin E.,Murach T.,Nakashima S.,de Naurois M.,Ndiyavala H.,Niederwanger F.,Niemiec J.,Oakes L.,O’Brien P.,Odaka H.,Ohm S.,Ostrowski M.,Oya I.,Padovani M.,Panter M.,Parsons R. D.,Pekeur N. W.,Pelletier G.,Perennes C.,Petrucci P.-O.,Peyaud B.,Piel Q.,Pita S.,Poireau V.,Prokhorov D. A.,Prokoph H.,Pühlhofer G.,Punch M.,Quirrenbach A.,Raab S.,Rauth R.,Reimer A.,Reimer O.,Renaud M.,de los Reyes R.,Rieger F.,Rinchiuso L.,Romoli C.,Rowell G.,Rudak B.,Rulten C. B.,Sahakian V.,Saito S.,Sanchez D. A.,Santangelo A.,Sasaki M.,Schlickeiser R.,Schüssler F.,Schulz A.,Schwanke U.,Schwemmer S.,Seglar-Arroyo M.,Seyffert A. S.,Shafi N.,Shilon I.,Shiningayamwe K.,Simoni R.,Sol H.,Spanier F.,Spir-Jacob M.,Stawarz Ł.,Steenkamp R.,Stegmann C.,Steppa C.,Sushch I.,Takahashi T.,Tavernet J.-P.,Tavernier T.,Taylor A. M.,Terrier R.,Tibaldo L.,Tiziani D.,Tluczykont M.,Trichard C.,Tsirou M.,Tsuji N.,Tuffs R.,Uchiyama Y.,van der Walt D. J.,van Eldik C.,van Rensburg C.,van Soelen B.,Vasileiadis G.,Veh J.,Venter C.,Viana A.,Vincent P.,Vink J.,Voisin F.,Völk H. J.,Vuillaume T.,Wadiasingh Z.,Wagner S. J.,Wagner P.,Wagner R. M.,White R.,Wierzcholska A.,Willmann P.,Wörnlein A.,Wouters D.,Yang R.,Zaborov D.,Zacharias M.,Zanin R.,Zdziarski A. A.,Zech A.,Zefi F.,Ziegler A.,Zorn J.,Żywucka N.,Enokiya R.,Fukui Y.,Hayakawa T.,Okuda T.,Torii K.,Yamamoto H.,

Abstract

The H.E.S.S. Collaboration has discovered a new very high energy (VHE, E > 0.1 TeV) γ-ray source, HESS J1741−302, located in the Galactic plane. Despite several attempts to constrain its nature, no plausible counterpart has been found so far at X-ray and MeV/GeV γ-ray energies, and the source remains unidentified. An analysis of 145-h of observations of HESS J1741−302 at VHEs has revealed a steady and relatively weak TeV source (~1% of the Crab Nebula flux), with a spectral index of Γ = 2.3 ± 0.2stat ± 0.2sys, extending to energies up to 10 TeV without any clear signature of a cut-off. In a hadronic scenario, such a spectrum implies an object with particle acceleration up to energies of several hundred TeV. Contrary to most H.E.S.S. unidentified sources, the angular size of HESS J1741−302 is compatible with the H.E.S.S. point spread function at VHEs, with an extension constrained to be below 0.068° at a 99% confidence level. The γ-ray emission detected by H.E.S.S. can be explained both within a hadronic scenario, due to collisions of protons with energies of hundreds of TeV with dense molecular clouds, and in a leptonic scenario, as a relic pulsar wind nebula, possibly powered by the middle-aged (20 kyr) pulsar PSR B1737−30. A binary scenario, related to the compact radio source 1LC 358.266+0.038 found to be spatially coincident with the best fit position of HESS J1741−302, is also envisaged.

Publisher

EDP Sciences

Subject

Space and Planetary Science,Astronomy and Astrophysics

Cited by 4 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

1. Exploring the possible gluon condensation signature in gamma-ray emission from pulsars;Journal of Cosmology and Astroparticle Physics;2021-08-01

2. VERITAS Observations of the Galactic Center Region at Multi-TeV Gamma-Ray Energies;The Astrophysical Journal;2021-06-01

3. Second AGILE catalogue of gamma-ray sources;Astronomy & Astrophysics;2019-06-25

4. The H.E.S.S. Galactic plane survey;Astronomy & Astrophysics;2018-04

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