by Nigel I Maxted (UNSW)

HESS J1731-347 is shell-type supernova remnant seen in TeV γ-rays, and is a potential accelerator of cosmic ray protons. Mopra CO(1-0) data may trace molecular gas associated with the supernova remnant, which may also be involved in γ-ray production. We derive a distance of ~3.2 kpc to the supernova remnant by comparing gas observations with X-ray absorption, and investigate the ISM structure at this distance.

Figure captions: – Left – A plot of Mopra CO(1-0) emission as a function of line of sight velocity and Galactic Longitude. Blue and pink dotted lines indicate the longitudinal extent of HESS J1731-347 (supernova remnant) and HESS J1729-345 (unidentified γ-ray source), respectively. – Right – Velocity-integrated CO(1-0) emission for three velocity-range slices corresponding to a kinematic distance of ~3.2 kpc, the distance for the supernova remnant derived in our analysis.

Reference: N. Maxted, M. Burton, C. Braiding, G. Rowell, H. Sano, F. Voisin, M. Capasso, G. Pühlhofer, and Y. Fukui, MNRAS, in press ( astro-ph:1710.06101 ).