A Search for Infrared Emission from Core-Collapse Supernovae at the Transitional Phase

TL;DR

This study investigates infrared emissions from core-collapse supernovae during the transitional phase (10-100 years post-explosion) using satellite data, detecting IR emission from SN 1978K and exploring dust formation and circumstellar environments.

Contribution

It provides the first observational search for IR emission in supernovae during the transitional phase and identifies shocked circumstellar dust as a key emission source in SN 1978K.

Findings

IR emission detected from SN 1978K with 1.3 x 10^{-3} Msun of silicate dust.

IR emission not detected in 5 other supernovae, constraining dust and mass-loss rates.

Shocked circumstellar dust likely explains IR emission in SN 1978K.

Abstract

Most of the observational studies of supernova (SN) explosions are limited to early phases (< a few yr after the explosion) of extragalactic SNe and observations of SN remnants (> 100 yr) in our Galaxy or very nearby galaxies. SNe at the epoch between these two, which we call "transitional" phase, have not been explored in detail except for several extragalactic SNe including SN 1987A in the Large Magellanic Cloud. We present theoretical predictions for the infrared (IR) dust emissions by several mechanisms; emission from dust formed in the SN ejecta, light echo by circumstellar and interstellar dust, and emission from shocked circumstellar dust. We search for IR emission from 6 core-collapse SNe at the transitional phase in the nearby galaxies NGC 1313, NGC 6946, and M101 by using the data taken with the AKARI satellite and Spitzer. Among 6 targets, we detect the emission from SN 1978K in NGC 1313. SN 1978K is associated with 1.3 x 10^{-3} Msun of silicate dust. We show that, among several mechanisms, the shocked circumstellar dust is the most probable emission source to explain the IR emission observed for CSM-rich SN 1978K. IR emission from the other 5 objects is not detected. Our current observations are sensitive to IR luminosity of > 10^{38} erg s^{-1}, and the non-detection of SN 1962M excludes the existence of the shocked circumstellar dust for a high gas mass-loss rate of sim 10^{-4} Msun yr^{-1}. Observations of SNe at the transitional phase with future IR satellites will fill the gap of IR observations of SNe with the age of 10-100 years, and give a new opportunity to study the circumstellar and interstellar environments of the progenitor, and possibly dust formation in SNe.