R. Seitenzahl , Ashley J. Ruiter & Parviz Ghavamian
title: |
    Shocked Interstellar clouds and dust grain destruction\
    in the LMC Supernova Remnant N132D
---

Introduction {#intro}
============

The supernova remnant (SNR) N132D in the Large Magellanic Cloud (LMC) is the brightest X-ray emitting SNR in this galaxy [@Hwang93; @Favata97; @Hughes98; @Borkowski07; @Xiao08]. Located within the stellar bar of the LMC, N132D was first identified as a SNR by @Westerlund66 on the basis of the association of a non-thermal radio source with a \[\]– bright optical structure. @Danziger76 discovered high-velocity \[\] and \[\] material ejected [ in the supernova explosion]{}, which established N132D as a relatively young SNR [ in which the reverse shock has not yet reached the centre of the remnant, marking the formal transition to the Sedov phase of evolution. This would imply that the swept-up interstellar medium (ISM) is less than a few times the mass ejected in the supernova event, a result which is in apparent contradiction to the swept-up mass derived from X-ray observations [@Hughes98].]{} From the dynamics of the fast-moving O and Ne material, @Danziger76 derived a maximum age of 3440yr for the SNR, and a probable age of $\sim 1350$yr. Subsequent analyses 