Revealing the Large-Scale Structures of Interstellar Gas Associated with the Magellanic SNR N132D

TL;DR

This study investigates the large-scale distribution of interstellar gas around the Magellanic SNR N132D, revealing a cavity-like CO structure and providing new insights into its molecular environment.

Contribution

It presents preliminary large-scale mapping of interstellar gas around N132D, identifying a cavity-like structure and updating the estimated molecular gas mass.

Findings

Identified a cavity-like CO structure along the SNR's X-ray shell.

Estimated the molecular gas mass as approximately 10^4 solar masses.

Found the gas mass to be an order of magnitude smaller than previous estimates.

Abstract

We report preliminary results of large-scale distribution toward the Magellanic supernova remnant N132D using Mopra and Chandra archival datasets. We identified a cavity-like CO structure along the X-ray shell toward the southern half of it. The total mass of associating molecular gas is $\sim10^4 M_\odot$, which is smaller than the previous study by an order of magnitude. Further observations using ALMA, ASTE, and Mopra will reveal the detailed spatial structures and its physical conditions.