Massive stars dying alone: the remote environment of SN 2010jp and its associated late-time source
arXiv:2201.02657 · doi:10.1093/mnras/stab2892
Abstract
We present late-time images of the site of the peculiar jet-driven TypeIIn supernova SN2010jp, including HST images taken 2-5 yr post explosion and deep ground-based images over a similar time. These are used to characterise its unusually remote environment and to constrain the progenitor's initial mass and age. The position of SN2010jp is found to reside along a chain of diffuse starlight that is probably an outer spiral arm or tidal tail of the interacting galaxy pair NGC2207/IC2163. There is one bright HII region projected within 1 kpc, and there is faint extended Halpha emission immediately surrounding the continuum source at the position of SN2010jp, which has mag. In principle, the lingering light could arise from late-time circumstellar material (CSM) interaction, an evolved supergiant, a host star cluster, or some combination of these. Steady flux over 3 yr and a lack of strong, spatially unresolved Halpha emission make ongoing CSM interaction unlikely. If an evolved supergiant dominates, its observed luminosity implies an initial mass of roughly 22 and an age older than roughly 8 Myr. If the source is a star cluster, then its colour and absolute magnitude imply an age of 8-13 Myr and a modest cluster initial mass of log() = 3.6-3.8. Extended Halpha emission out to a radius of 30 pc reveals a faint evolved HII region, pointing to recent star formation with at least one late O-type star. Based on these various clues, we conclude that the progenitor of SN2010jp had a likely initial mass of 18-22 .
arXiv commentMNRAS accepted, 10 pages
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