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An extreme particle accelerator in the Galactic plane: HESSJ1826-130


Angüner, EO; Casanova, S; Bordas, P; Oya, I; Ziegler, A; Mitchell, A M W; Takahashi, T A (2020). An extreme particle accelerator in the Galactic plane: HESSJ1826-130. Astronomy and Astrophysics, 644:A112.

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 extendedwith 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 indexΓ =1.78±0.10stat±0.20sysand an exponential cut-offat 15.2+5.5−3.2TeV, or a broken power-law withΓ1=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 ofthe bright, nearby pulsar wind nebula (PWN), HESS J1825−137, particularly at the low end of the energy spectrum. Leptonic scenarios for theorigin of HESS J1826−130 VHE emission related to PSR J1826−1256 are confronted by our spectral and morphological analysis. In a hadronicframework, taking into account the properties of dense gas regions surrounding HESS J1826−130, the source spectrum would imply an astrophysicalobject capable of accelerating the parent particle population up to&200 TeV. Our results are also discussed in a multiwavelength context, accountingfor both the presence of nearby supernova remnants (SNRs), molecular clouds, and counterparts detected in radio, X-rays, and TeV energies

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 extendedwith 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 indexΓ =1.78±0.10stat±0.20sysand an exponential cut-offat 15.2+5.5−3.2TeV, or a broken power-law withΓ1=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 ofthe bright, nearby pulsar wind nebula (PWN), HESS J1825−137, particularly at the low end of the energy spectrum. Leptonic scenarios for theorigin of HESS J1826−130 VHE emission related to PSR J1826−1256 are confronted by our spectral and morphological analysis. In a hadronicframework, taking into account the properties of dense gas regions surrounding HESS J1826−130, the source spectrum would imply an astrophysicalobject capable of accelerating the parent particle population up to&200 TeV. Our results are also discussed in a multiwavelength context, accountingfor both the presence of nearby supernova remnants (SNRs), molecular clouds, and counterparts detected in radio, X-rays, and TeV energies

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Item Type:Journal Article, refereed, original work
Communities & Collections:07 Faculty of Science > Physics Institute
Dewey Decimal Classification:530 Physics
Uncontrolled Keywords:Space and Planetary Science, Astronomy and Astrophysics
Language:English
Date:1 December 2020
Deposited On:05 Nov 2020 16:22
Last Modified:08 Dec 2020 02:17
Publisher:EDP Sciences
ISSN:0004-6361
OA Status:Green
Free access at:Publisher DOI. An embargo period may apply.
Publisher DOI:https://doi.org/10.1051/0004-6361/202038851

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