Strongly lensed SN Refsdal: refining time delays based on the supernova explosion models. (arXiv:2007.04106v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Baklanov_P/0/1/0/all/0/1">Petr Baklanov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lyskova_N/0/1/0/all/0/1">Natalia Lyskova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blinnikov_S/0/1/0/all/0/1">Sergei Blinnikov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nomoto_K/0/1/0/all/0/1">Ken&#x27;ichi Nomoto</a>

We explore the unique supernova (SN) “Refsdal” – the first discovered
gravitationally lensed SN with multiple images. A large magnification provided
by the galactic-scale lens, augmented by the cluster lens, gave us the
opportunity to perform a detailed modelling of a distant SN at $z simeq 1.5$.
% We present results of radiation hydrodynamics modelling of snref. According
to our calculations, the snref progenitor is likely to be a more massive and
energetic version of sna, i.e. a blue supergiant star with a radius of ${rm
R} = 50 R_{odot}$ before an explosion and a total mass of ${rm M}= 26
M_{odot}$. The total energy release is ${rm E}=5times10^{51}$ erg.
Reconstruction of SN light curves allowed us to obtain time delays and
magnifications for the images S2-S4 relative to S1 with higher accuracy than
previous estimates of Rodney et al. We estimate the Hubble constant $H_0 =
68.6^{+13.6}_{-9.7}$ km s$^{-1}$ Mpc$^{-1}$ via re-scaling the time delays
predicted by different lens models to match the values obtained in this work.
With more photometric data on the fifth image SX, we will be able to further
refine the time delay and magnification estimates for SX and obtain competitive
constraints on $H_0$.

We explore the unique supernova (SN) “Refsdal” – the first discovered
gravitationally lensed SN with multiple images. A large magnification provided
by the galactic-scale lens, augmented by the cluster lens, gave us the
opportunity to perform a detailed modelling of a distant SN at $z simeq 1.5$.
% We present results of radiation hydrodynamics modelling of snref. According
to our calculations, the snref progenitor is likely to be a more massive and
energetic version of sna, i.e. a blue supergiant star with a radius of ${rm
R} = 50 R_{odot}$ before an explosion and a total mass of ${rm M}= 26
M_{odot}$. The total energy release is ${rm E}=5times10^{51}$ erg.
Reconstruction of SN light curves allowed us to obtain time delays and
magnifications for the images S2-S4 relative to S1 with higher accuracy than
previous estimates of Rodney et al. We estimate the Hubble constant $H_0 =
68.6^{+13.6}_{-9.7}$ km s$^{-1}$ Mpc$^{-1}$ via re-scaling the time delays
predicted by different lens models to match the values obtained in this work.
With more photometric data on the fifth image SX, we will be able to further
refine the time delay and magnification estimates for SX and obtain competitive
constraints on $H_0$.

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