Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 474, Issue 1, Pages 662-676Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stx2727
Keywords
cosmic rays; ISM: clouds; ISM: supernova remnants; gamma-rays: ISM
Categories
Funding
- Commonwealth of Australia
- Australian Research Council
- University of New South Wales
- University of Sydney
- Monash University
- CSIRO
- Australian Research Council through a Linkage Infrastructure, Equipment and Facilities (LIEF) [LE16010094]
- Grants-in-Aid for Scientific Research [15H05694, 16K17664] Funding Source: KAKEN
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The shell-type supernova remnant HESS J1731 - 347 emits TeV gamma-rays, and is a key object for the study of the cosmic ray acceleration potential of supernova remnants. We use 0.5-1 arcmin Mopra CO/CS(1-0) data in conjunction with HI data to calculate column densities towards the HESS J1731 - 347 region. We trace gas within at least four Galactic arms, typically tracing total (atomic+molecular) line-of-sight H column densities of 2-3 x 10(22) cm(-2). Assuming standard X-factor values and that most of the H I/CO emission seen towards HESS J1731 - 347 is on the near-side of the Galaxy, X-ray absorption column densities are consistent with H I+CO-derived column densities foreground to, but not beyond, the Scutum-Crux Galactic arm, suggesting a kinematic distance of similar to 3.2 kpc for HESS J1731 - 347. At this kinematic distance, we also find dense, infrared-dark gas traced by CS(1-0) emission coincident with the north of HESS J1731 - 347, the nearby H II region G353.43-0.37 and the nearby unidentified gamma-ray source HESS J1729 - 345. This dense gas lends weight to the idea that HESS J1729 - 345 and HESS J1731 - 347 are connected, perhaps via escaping cosmic-rays.
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