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Type: Journal article
Title: Probing the local environment of the supernova remnant HESS J1731-347 with CO and CS observations
Author: Maxted, N.
Burton, M.
Braiding, C.
Rowell, G.
Sano, H.
Voisin, F.
Capasso, M.
Puehlhofer, G.
Fukui, Y.
Citation: Monthly Notices of the Royal Astronomical Society, 2018; 474(1):662-676
Publisher: Oxford University Press
Issue Date: 2018
ISSN: 0035-8711
Statement of
N. Maxted, M. Burton, C. Braiding, G. Rowell, H. Sano, F. Voisin, M. Capasso, G. Pühlhofer and Y. Fukui
Abstract: 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× 10²² cm⁻². Assuming standard X-factor values and that most of the HI/CO emission seen towards HESS J1731 − 347 is on the near-side of the Galaxy, X-ray absorption column densities are consistent with HI+CO-derived column densities foreground to, but not beyond, the Scutum–Crux Galactic arm, suggesting a kinematic distance of ∼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 HII 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.
Rights: © 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI: 10.1093/mnras/stx2727
Grant ID: ARC
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