Progenitor candidate for the type II-P supernova SN 2018aoq in NGC 4151. (arXiv:1812.04988v1 [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:+Sim_S/0/1/0/all/0/1">S. A. Sim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benetti_S/0/1/0/all/0/1">S. Benetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smartt_S/0/1/0/all/0/1">S. J. Smartt</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:+Ashall_C/0/1/0/all/0/1">C. Ashall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Callis_E/0/1/0/all/0/1">E. Callis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elias_Rosa_N/0/1/0/all/0/1">N. Elias-Rosa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gromadzki_M/0/1/0/all/0/1">M. Gromadzki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prentice_S/0/1/0/all/0/1">S. J. Prentice</a>
We present our findings based on pre- and post-explosion data of the type
II-Plateau SN 2018aoq that exploded in NGC 4151. As distance estimates to NGC
4151 vary by an order of magnitude, we utilised the well-known correlation
between ejecta velocity and plateau brightness, i.e. the standard candle
method, to obtain a distance of 18.2$pm$1.2 Mpc, which is in very good
agreement with measurements based on geometric methods. The above distance
implies a mid-plateau absolute magnitude of $M_{V}^{50}=-15.76pm$0.14
suggesting that it is of intermediate brightness when compared to IIP SNe such
as SN 2005cs at the faint end, and more typical events such as SN 1999em. This
is further supported by relatively low expansion velocities (Fe II
$lambda$5169 $sim$3000 km s$^{-1}$ at +42 d). Using archival HST/WFC3 imaging
data, we find a point source coincident with the supernova position in the
F350LP, F555W, F814W, and F160W filters. This source shows no significant
variability over the $sim$2 month time span of the data. From fits to the
spectral energy distribution of the candidate progenitor, we find
$logleft(L/L_odotright)sim 4.7$ and $T_{mathrm{eff}}sim 3.5$ kK,
implying an M-type red supergiant progenitor. From comparisons to single and
binary star models, we find that both favour the explosion of a star with a
zero-age main sequence mass of $sim$$10 M_odot$.
We present our findings based on pre- and post-explosion data of the type
II-Plateau SN 2018aoq that exploded in NGC 4151. As distance estimates to NGC
4151 vary by an order of magnitude, we utilised the well-known correlation
between ejecta velocity and plateau brightness, i.e. the standard candle
method, to obtain a distance of 18.2$pm$1.2 Mpc, which is in very good
agreement with measurements based on geometric methods. The above distance
implies a mid-plateau absolute magnitude of $M_{V}^{50}=-15.76pm$0.14
suggesting that it is of intermediate brightness when compared to IIP SNe such
as SN 2005cs at the faint end, and more typical events such as SN 1999em. This
is further supported by relatively low expansion velocities (Fe II
$lambda$5169 $sim$3000 km s$^{-1}$ at +42 d). Using archival HST/WFC3 imaging
data, we find a point source coincident with the supernova position in the
F350LP, F555W, F814W, and F160W filters. This source shows no significant
variability over the $sim$2 month time span of the data. From fits to the
spectral energy distribution of the candidate progenitor, we find
$logleft(L/L_odotright)sim 4.7$ and $T_{mathrm{eff}}sim 3.5$ kK,
implying an M-type red supergiant progenitor. From comparisons to single and
binary star models, we find that both favour the explosion of a star with a
zero-age main sequence mass of $sim$$10 M_odot$.
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