Maxted, N.I.Braiding, C.Wong, G.F.Rowell, G.P.Burton, M.G.Filipović, M.D.Voisin, F.Urošević, D.Vukotić, B.Pavlović, M.Z.Sano, H.Fukui, Y.2019-01-312019-01-312018Monthly Notices of the Royal Astronomical Society, 2018; 480(1):134-1480035-87111365-2966http://hdl.handle.net/2440/117522The Galactic supernova remnant HESSJ1534−571 (also known as G323.7 − 1.0) has a shell-like morphology in TeV gamma-ray emission and is a key object in the study of cosmic ray origin. Little is known about its distance and local environment. We examine Mopra 12CO/13CO(1–0) data, Australian Telescope Compact Array HI⁠, and Parkes HI data towards HESSJ1534−571⁠. We trace molecular clouds in at least five velocity ranges, including clumpy interstellar medium structures near a dip in HI emission at a kinematic velocity consistent with the Scutum–Crux arm at ∼3.5 kpc. This feature may be a cavity blown-out by the progenitor star, a scenario that suggests HESSJ1534−571 resulted from a core-collapse event. By employing parametrizations fitted to a sample of supernova remnants of known distance, we find that the radio continuum brightness of HESSJ1534−571 is consistent with the ∼3.5 kpc kinematic distance of the Scutum–Crux arm HI dip. Modelling of the supernova evolution suggests a ∼8–24 kyr age for HESSJ1534−571 at this distance.en© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical SocietyCosmic rays, ISM: molecules, ISM: supernova remnants, gamma-rays: ISMJournal article003009685610.1093/mnras/sty17970004425679000122-s2.0-85052575670435949Rowell, G.P. [0000-0002-9516-1581]