Abstract
The Galactic supernova remnant HESS J1534-571 (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 HESS J1534-571. 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 HESS J1534-571 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 HESS J1534-571 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 HESS J1534-571 at this distance.
Original language | English |
---|---|
Pages (from-to) | 134-148 |
Number of pages | 15 |
Journal | Monthly Notices of the Royal Astronomical Society |
Volume | 480 |
Issue number | 1 |
DOIs | |
Publication status | Published - 2018 |
Keywords
- cosmic rays
- gamma rays
- interstellar matter
- supernova remnants