Two shell- and wing-shaped supernova remnants. Investigating the molecular environments around VRO 42.05.01 and G 350.0-2.0

TL;DR

This study investigates the molecular environments of two similar-shaped supernova remnants, VRO 42.05.01 and G 350.0-2.0, revealing different environmental interactions despite their morphological similarities.

Contribution

It provides the first detailed molecular environment analysis of these two SNRs, showing that their shell and wing shapes are not caused by similar ambient molecular conditions.

Findings

VRO 42.05.01 interacts with its molecular environment, showing broadened CO lines and shock features.

G 350.0-2.0 shows no such molecular interaction features.

Both SNRs have similar radio spectral steepening at low frequencies.

Abstract

Supernova remnants (SNRs) are profoundly affected by their ambient medium. We present carbon monoxide (CO) observations around two mixed morphology SNRs, VRO 42.05.01 and G 350.0-2.0, that look remarkably similar in continuum radio emission, showing what we refer to as a shell and wing shape. It has been proposed that the shell and wing shape is the result of environmental effects, in the form of a sharp density gradient or discontinuity. Our motivation for studying these two sources jointly is that if the dense molecular environment causes the development of these sources' shell and wing shape, then these two sources' environments must be similar. This is contrary to what we observe. In the case of VRO 42.05.01, we have found direct evidence of an interaction with its molecular environment, in the form of broadened $^{12}$CO line profiles, high $(J=2-1)$ to $(J=1-0)$ line ratios, and arc features in position-velocity space. We interpret some of these features to be associated with the SNR shock, and some of them to be due to the presence of a pre-supernova stellar wind. We have found no such features in the abundant molecular gas surrounding G 350.0-2.0. We have also made a spectral index map of G 350.0-2.0, and we see that the radio spectrum of G 350.0-2.0 steepens significantly at frequencies $<200$~MHz, much like that of VRO 42.05.01. In spite of their spectral and morphological similarities, these two sources look substantially different in their optical and infrared emission. The lack of large-scale correspondence between the radio continuum and the molecular material, as well as the differences in the excitation and morphological properties of the molecular gas surrounding both sources, lead us to conclude that the shell and wing morphology of these two sources is not due to interactions with a similar ambient molecular ISM.