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

Abstract

Most of the observational studies of supernova (SN) explosions are limited to early phases (<a few years 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 the "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 (CS) and interstellar (IS) dust, and emission from shocked CS dust. We search for IR emission from six 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 six targets, we detect the emission from SN 1978K in NGC 1313. SN 1978K is associated with 1.3 × 10 −3 M of silicate dust. We show that, among several mechanisms, the shocked CS dust is the most probable emission source to explain the IR emission observed for SN 1978K. IR emission from the other five 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 CS dust for a high gas mass-loss rate of ∼10 −4 M 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 yr, and give a new opportunity to study the CS and IS environments of the progenitor, and possibly dust formation in SNe.

First detection of X-ray line emission from Type IIn supernova 1978K with XMM-Newton’s RGS

“…Substituting these values into above Lx-Ṁ relation, we obtained the mass-loss rate to bė M l = 19.5 × 10 −4 M⊙ yr −1 andṀ h = 6.2 × 10 −4 M⊙ yr −1 for the low-and high-temperature components, respectively. This result is well within the range of mass-loss rates estimated in preceeding works (e.g., Ryder et al 1993;Chugai et al 1995;Schlegel et al 1999;Tanaka et al 2012;Kuncarayakti et al 2016). According to Kiewe et al (2012), such a high mass-loss rate can be best explained by LBV stars whose mass-loss rates are measured to bė M = 10 −4 − 10 M⊙ yr −1 .…”

Stardusts in Supernova Remnants Seen by Akari

“…A result on the dusts in SNRs in an earlier stage has been recently reported by Tanaka et al (2012). They have searched IR emission associated with six extragalactic SNRs.…”

ALMA, ATCA, and Spitzer Observations of the Luminous Extragalactic Supernova SN 1978K

“…The strong X-ray and UV energization in SN 1978K suggests it might not be a good place to create long-lasting dust. However, SN 1978K does currently have a significant emission from warm dust: it was the only supernova in the transitional phase detected by Tanaka et al (2012).…”

“…Thus the contribution from synchrotron radiation to the infrared emission is much smaller than assumed by Tanaka et al (2012). Tanaka et al (2012) preferred a model that used 1.3× 10 −3 M ⊙ of silicate dust at T = 230 K. This gives a double-peaked spectrum similar to the Spitzer IRS one shown in Figure 4. Removing the synchrotron component, the increase in the peak flux that needs to come from warm dust is relatively small, 10%.…”

“…The Spitzer IRS mid-infrared spectrum is shown in Figure 4; see also van Dyk (2011). The double-peaked spectrum is broadly consistent with the AKARI observations and modeling shown in Tanaka et al (2012). 55749 12099 42193408 0.04475 ± 0.00188 0.07783 ± 0.00132 · · · · · · 2012-02-01 55959 12309 42193152 0.04169 ± 0.00195 0.07623 ± 0.00126 · · · · · · 2014-02-12 56701 13051 50504704 · · · 0.07168 ± 0.00205 · · · · · · 2016-08-05 57606 13956 52691456 0.03138 ± 0.00083 · · · · · · · · · 2017-01-02 57755 14105 60812544 · · · 0.05311 ± 0.00063 · · · · · · 2018-02-09 58158 14508 60813568 · · · 0.05132 ± 0.00065 · · · · · · 2018-08-24 58355 14705 66130688 0.02500 ± 0.00068 0.04858 ± 0.00058 · · · · · · a Age based on the adopted explosion date of 1978-05-22 (MJD 43650).…”