XRF 100316D / SN 2010bh and the Nature of Gamma Ray Burst Supernovae

TL;DR

This study presents detailed optical and infrared observations of SN 2010bh associated with XRF 100316D, revealing its unique properties, explosion parameters, and comparing its light curve evolution with other GRB-SNe, contributing to understanding their diversity.

Contribution

It provides the first detailed analysis of SN 2010bh's light curves, estimates its explosion parameters, and investigates correlations among GRB-SNe properties, highlighting its faintness and shock break-out origin.

Findings

SN 2010bh has the fastest optical light curve evolution among GRB-SNe.

It is the faintest spectroscopically-confirmed GRB-SN in V-band.

No significant correlation between stretch and luminosity factors in GRB-SNe.

Abstract

We present ground-based and HST optical and infrared observations of XRF 100316D / SN 2010bh. It is seen that the optical light curves of SN 2010bh evolve at a faster rate than the archetype GRB-SN 1998bw, but at a similar rate to SN 2006aj, a supernova that was spectroscopically linked with XRF 060218, and at a similar rate to non-GRB associated type Ic SN 1994I. We estimate the rest-frame extinction of this event from our optical data to be E(B-V)=0.18 +/- 0.08 mag. We find the V-band absolute magnitude of SN 2010bh to be M_{V}=-18.62 +/- 0.08, which is the faintest peak V-band magnitude observed to-date for a spectroscopically-confirmed GRB-SNe. When we investigate the origin of the flux at t-t_{o}=0.598 days, it is shown that the light is not synchrotron in origin, but is likely coming from the supernova shock break-out. We then use our optical and infrared data to create a quasi-bolometric light curve of SN 2010bh which we model with a simple analytical formula. The results of our modeling imply that SN 2010bh synthesized a nickel mass of M_{Ni} \approx 0.10 M_{sun}, ejected M_{ej} \approx 2.2 M_{sun} and has an explosion energy of E_{k} \approx 1.4 x 10^{52} erg. Finally, for a sample 22 GRB-SNe we check for a correlation between the stretch factors and luminosity factors in the R band and conclude that no statistically-significant correlation exists.