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ABSTRACT With Gaia parallaxes, it is possible to study the stellar populations associated with individual Galactic supernova remnants (SNRs) to estimate the mass of the exploding star. Here, we analyse the luminous stars near the Vela pulsar and SNR to find that its progenitor was probably ($$\mathrel {\raise.3ex\rm{\gt }\lower0.6ex\rm{\sim }}90\rm \,per\,cent$$) low mass (8.1–$$10.3\, {\rm M}_\odot$$). The presence of the O star γ2 Vel a little over 100 pc from Vela is the primary ambiguity, as including it in the analysis volume significantly increases the probability (to 5 per cent) of higher mass ($$\gt 20\, {\rm M}_\odot$$) progenitors. However, to be a high-mass star associated with γ2 Vel’s star cluster at birth, the progenitor would have to be a runaway star from an unbound binary with an unusually high velocity. The primary impediment to analysing large numbers of Galactic SNRs in this manner is the lack of accurate distances. This can likely be solved by searching for absorption lines from the SNR in stars as a function of distance, a method which yielded a distance to Vela in agreement with the direct pulsar parallax. If Vela was a $$10\, {\rm M}_\odot$$ supernova in an external galaxy, the 50-pc search region used in extragalactic studies would contain only $$\simeq 10\rm \,per\,cent$$ of the stars formed in a 50-pc region around the progenitor at birth and $$\simeq 90\rm \,per\,cent$$ of the stars in the search region would have been born elsewhere.
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On the progenitor of the Crab Pulsar
ABSTRACT We investigate the progenitor of the Crab supernova by examining the remnant’s surrounding stellar population. The Crab is interesting because of the apparently low energy and mass of the supernova remnant. We also know it was not a binary at death and that the explosion formed a neutron star. Using Gaia EDR3 parallaxes and photometry, we analyse stars inside a cylinder with a projected radius of 100 pc and spanning distances from $$\sim 1600$$ to 2300 pc set by the $$2\sigma$$ uncertainties in the Crab’s parallax. We also individually model the most luminous stars local to the Crab. The two most luminous stars are blue, roughly main sequence stars with masses of $$\sim 11\, {\rm M}_{\odot }$$. We estimate the stellar population’s age distribution using solar metallicity PARSEC isochrones. The estimated age distribution of the 205 $$M_{\mathrm{ G}} < 0$$ stars modestly favour lower mass stars, consistent with an AGB star or a lower mass binary merger as the progenitor, but statistically we cannot rule out higher masses. This may be driven by contamination due to the $$\sim 700$$ pc span of the cylinder in distance.
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- Award ID(s):
- 2307385
- PAR ID:
- 10628084
- Publisher / Repository:
- Oxford University Press
- Date Published:
- Journal Name:
- Monthly Notices of the Royal Astronomical Society
- Volume:
- 538
- Issue:
- 2
- ISSN:
- 0035-8711
- Page Range / eLocation ID:
- 745 to 754
- Format(s):
- Medium: X
- Sponsoring Org:
- National Science Foundation
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- Free Publicly Accessible Full Text
-
Accepted Manuscript
- Journal Article:
- https://doi.org/10.1093/mnras/staf333
