Early ultraviolet signatures from the interaction of Type Ia supernova ejecta with a stellar companion

TL;DR

This paper models early ultraviolet emissions from Type Ia supernovae interacting with companion stars, aiming to identify progenitor systems by comparing predictions with observations like iPTF14atg.

Contribution

It provides theoretical luminosity distributions for UV signatures from SN Ia ejecta-companion interactions across different progenitor types.

Findings

The UV pulse of iPTF14atg likely originated from a red-giant donor system.

Main-sequence and helium-star donors are unlikely for iPTF14atg.

Models can help constrain SN Ia progenitors through early UV observations.

Abstract

The progenitors of SNe Ia are not yet fully understood. The two leading progenitor scenarios are the single-degenerate (SD) scenario and the double-degenerate scenario. In the SD scenario, the collision of the SN Ia ejecta with its companion star is expected to produce detectable ultraviolet (UV) emission in the first few days after the SN explosion within certain viewing angles. A strong UV flash has recently been detected in an SN 2002es-like peculiar SN Ia iPTF14atg by Cao et al., which is interpreted as evidence of an early-time UV signature due to SN ejecta interacting with its companion star, supporting the SD scenario. In this paper, we present the expected luminosity distributions of early-time UV emission arising from SN Ia ejecta-companion interaction by performing binary population synthesis calculations for different progenitor systems in the SD scenario. Our theoretical predictions will be helpful for future early-time observations of SNe Ia to constrain their possible progenitors. Assuming the observed strong UV pulse of iPTF14atg was indeed produced by the SN ejecta-companion interaction, our population synthesis model suggests that the progenitor system of iPTF14atg is most likely a red-giant donor binary system, and it is unlikely to have been a main-sequence or helium-star donor system.