2007/03/29 by Xiao Xiao, Yang Chen · 1 citation
Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Cosmic Phenomena #Galaxy #Gamma-ray bursts and supernovae #Large Magellanic Cloud #Materials science #Optics #Physics #Shell (structure) #Spectral line #Spectroscopy #Supernova #Supernova remnant #Synchrotron #Thermal #X-ray #X-ray spectroscopy #astro-ph
paper · pdf · doi:10.1016/j.asr.2007.03.071
published as Adv.SpaceRes.41:416-423,2008 · 14 pages (including 9 figures), accepted for publication in AdSpR
arxiv created 2007/03/29 · openalex publication_date 2007/04/25 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present the preliminary results of a Chandra X-ray study of N132D, a young shell-like supernova remnant (SNR) in the Large Magellanic Cloud. The equivalent width maps of emissions from O, Ne, Mg, Si, and S are provided. Spatially resolved spectral analysis for the small-scale regions were tentatively performed. The X-ray spectra of the interior can be described with a single-thermal model. The faint interior regions have lower density and higher temperature (above 1keV) than those of bright interior regions. The X-ray spectra along the shell can be phenomenally fitted with either a double-vpshock model or a vpshock + powerlaw model. If the non-thermal component is true, N132D would be listed as another X-ray synchrotron SNR.