SN2017ein: bolometric light curve and physical parameters

TL;DR

This paper presents photometric analysis and bolometric light curve reconstruction of supernova SN2017ein, estimating key physical parameters and highlighting its unusually low luminosity compared to typical supernovae.

Contribution

It introduces a method to reconstruct the bolometric light curve from photometric data and estimates physical parameters for SN2017ein using simple models, providing new insights into this peculiar supernova.

Findings

Reconstructed peak luminosity of $3.3\times 10^{41}$ erg/s, lower than typical supernovae.

Estimated nickel-56 mass of 0.037 solar masses.

Estimated ejected mass of 1.246 solar masses.

Abstract

Apparent stellar magnitudes observed at Maidanak observatory for SN2017ein - peculiarly faint core-collapse supernova rumored to have images of progenitor - are processed to get exact photometric data. Technique of photometry is described and the data itself is presented. Based on photometric data of B and R bands we used the regressional equation proposed by Lyman and Bersier to reconstruct the quasi-bolometric light curve. Reconstructed light curve has a peak luminosity of $3.3\cdot 10^{41} \rm{erg/s}$ which is almost an order of magnitude lower than typical values for such supernovae. Further, we used reconstructed bolometric values to estimate physical parameters using simple one-component models for photospheric and nebular phases. Fitting the models to reconstructed quasi-bolometric light curve allows us to estimate physical parameters. Such estimation yields $0.037 M_{\odot}$ for nickel-56 mass, $1.246 M_{\odot}$ for ejected mass and $1.641\cdot 10^{51}$ erg for final kinetic energy of ejecta. Ejecta mass looks very small for proposed progenitor candidate, but some explanations for such discrepancy are already proposed.