SN 2015bq: A Luminous Type Ia Supernova with Early Flux Excess

TL;DR

SN 2015bq is a luminous Type Ia supernova exhibiting an early flux excess likely caused by radioactive decay of surface-embedded $^{56}$Ni, providing insights into supernova diversity and explosion mechanisms.

Contribution

This study presents detailed optical and UV observations of SN 2015bq, revealing the role of surface $^{56}$Ni in early flux excess and linking its properties to known subclasses.

Findings

Early flux excess observed in UV bands.

High surface $^{56}$Ni mass (~0.97 M_sun) inferred.

SN 2015bq properties between SN 1991T and SN 1999aa.

Abstract

We present optical and ultraviolet (UV) observations of a luminous type Ia supernova (SN Ia) SN 2015bq characterized by the early flux excess. This SN reaches a B-band absolute magnitude at $M_B = -19.68 \pm 0.41$ mag and a peak bolometric luminosity at $L = (1.75 \pm 0.37) \times 10^{43}$ erg s$^{-1}$, with a relatively small post-maximum decline rate [$\Delta m_{15}(B) = 0.82 \pm 0.05$ mag]. The flux excess observed in the light curves of SN 2015bq a few days after the explosion, especially seen in the UV bands, might be due to the radioactive decay of $^{56}$Ni mixed into the surface. The radiation from the decay of the surface $^{56}$Ni heats the outer layer of this SN. It produces blue $U-B$ color followed by monotonically reddening in the early phase, dominated iron-group lines, and weak intermediate-mass elements absorption features in the early spectra. The scenario of enhanced $^{56}$Ni in the surface is consistent with a large amount of $^{56}$Ni ($M_{ \rm ^{56}{\rm Ni}}$ = 0.97 $\pm 0.20$ $M_{\odot}$) synthesized during the explosion. The properties of SN 2015bq are found to locate between SN 1991T and SN 1999aa, suggesting the latter two subclasses of SNe Ia may have a common origin.