Molecular environment of the thermal composite supernova remnant G352.7$-$0.1

TL;DR

This study investigates the molecular environment of supernova remnant G352.7$-$0.1 using CO spectroscopy, revealing interactions with molecular clouds, estimating shock properties, and analyzing gamma-ray data with no detected counterparts.

Contribution

First detailed spectroscopic mapping of G352.7$-$0.1 revealing its interaction with molecular clouds and environmental properties.

Findings

Interaction with molecular clouds at ~-51 km/s

Estimated shock momentum and energy

No gamma-ray counterparts detected

Abstract

Galactic supernova remnants (SNRs) play an important role in our understanding of supernovae and their feedback on the interstellar environment. SNR G352.7$-$0.1 is special for its thermal composite morphology and double-ring structure. We have performed spectroscopic mapping in $^{12}$CO and $^{13}$CO $J=2$-1 lines toward G352.7$-$0.1 with the Atacama Pathfinder Experiment telescope. Broad $^{12}$CO lines are found in the northeastern ring at a local-standard-of-rest velocity range of $\sim-50$-$-30$ km s$^{-1}$, suggesting that the remnant is interacting with molecular clouds (MCs) at $\sim-51$ km s$^{-1}$. Thus, we adopt a distance of $\sim10.5$ kpc for this SNR. The momentum and kinetic energy of the shocked gas along the line of sight are estimated to be $\sim10^2{\rm M_{sun}}$ km s$^{-1}$ and $\sim10^{46}$ erg, respectively. We also find an expanding structure around the remnant, which is possibly related to the wind-blown bubble of the progenitor star. From the Fermi-LAT data in an energy range of 0.1-500 GeV, we find no gamma-ray counterparts of G352.7$-$0.1.