Dust masses for SN 1980K, SN1993J and Cassiopeia A from red-blue emission line asymmetries

TL;DR

This study uses Monte Carlo line transfer models to analyze dust effects on late-time emission line spectra of supernovae SN 1980K, SN 1993J, and Cassiopeia A, estimating their dust masses and properties.

Contribution

It introduces detailed modeling of dust influence on emission line asymmetries to estimate dust masses in supernova remnants, advancing understanding of dust formation in such environments.

Findings

Dust masses estimated: 0.08-0.15 M$_\ m\odot$ for SN 1993J

Dust masses estimated: 0.12-0.30 M$_\ m\odot$ for SN 1980K

Dust mass for Cas A approximately 1.1 M$_\ m\odot$

Abstract

We present Monte Carlo line transfer models that investigate the effects of dust on the very late time emission line spectra of the core collapse supernovae SN 1980K and SN 1993J and the young core collapse supernova remnant Cassiopeia A. Their blue-shifted emission peaks, resulting from the removal by dust of redshifted photons emitted from the far sides of the remnants, and the presence of extended red emission wings are used to constrain dust compositions and radii and to determine the masses of dust in the remnants. We estimate dust masses of between 0.08 - 0.15 M$_\odot$ for SN 1993J at year 16, 0.12 - 0.30 M$_\odot$ for SN 1980K at year 30 and $\sim$1.1 M$_\odot$ for Cas A at year $\sim$330. Our models for the strong oxygen forbidden lines of Cas A require the overall modelled profiles to be shifted to the red by between 700 - 1000 km s$^{-1}$, consistent with previous estimates for the shift of the dynamical centroid of this remnant.