Revisiting the progenitor of the low-luminosity type II-plateau supernova, SN 2008bk. (arXiv:2012.00592v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+ONeill_D/0/1/0/all/0/1">D. O'Neill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kotak_R/0/1/0/all/0/1">R. Kotak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fraser_M/0/1/0/all/0/1">M. Fraser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mattila_S/0/1/0/all/0/1">S. Mattila</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pietrzynski_G/0/1/0/all/0/1">G. Pietrzyński</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prieto_J/0/1/0/all/0/1">J. L. Prieto</a>
The availability of updated model atmospheres for red supergiants and
improvements in single and binary stellar evolution models, as well as
previously unpublished data prompted us to revisit the progenitor of
low-luminosity type II-Plateau supernova, SN 2008bk. Using mid-IR data in
combination with dust models, we find that high temperature (4250-4500 K), high
extinction (E(B-V)>0.7) solutions are incompatible with the data. We therefore
favour a cool (~3500-3700 K) progenitor with a luminosity of log(L/Lsun)~4.53.
Comparing with evolutionary tracks, we infer progenitor masses in the 8-10 Msun
range in agreement with some previous studies. This mass is consistent with the
observed pattern of low-luminosity Type IIP SNe coming from the explosion of
RSGs at the lower extremum for core-collapse. We also present multi-epoch data
of the progenitor, but do not find clear evidence of variability.
The availability of updated model atmospheres for red supergiants and
improvements in single and binary stellar evolution models, as well as
previously unpublished data prompted us to revisit the progenitor of
low-luminosity type II-Plateau supernova, SN 2008bk. Using mid-IR data in
combination with dust models, we find that high temperature (4250-4500 K), high
extinction (E(B-V)>0.7) solutions are incompatible with the data. We therefore
favour a cool (~3500-3700 K) progenitor with a luminosity of log(L/Lsun)~4.53.
Comparing with evolutionary tracks, we infer progenitor masses in the 8-10 Msun
range in agreement with some previous studies. This mass is consistent with the
observed pattern of low-luminosity Type IIP SNe coming from the explosion of
RSGs at the lower extremum for core-collapse. We also present multi-epoch data
of the progenitor, but do not find clear evidence of variability.
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