The Oxygen-Rich SNR N132D: Ejecta Detection and Chemical Abundances

Details The Oxygen-Rich SNR N132D: Ejecta Detection and Chemical Abundances The Oxygen-Rich SNR N132D: Ejecta Detection and Chemical Abundances

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004cxo..prop.1698b&link_type=abstract

Chandra Proposal ID #06500305

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Chandra Proposal Id #06500305

Scientific paper

N132D is the brightest supernova remnant in the Large Magellanic Cloud, with oxygen-rich filamentary ejecta detected in the optical at its center. O-rich remnants originate in explosions of massive stars, in this case 30-35 solar masses. Several solar masses of O-rich ejecta are then expected, and indeed available Chandra data hint at the central O overabundance. We propose a deep 100 ksec ACIS-S/S3 observation in order to detect and study supernova ejecta, and determine their chemical composition. An equally important objective is to study chemical abundances in the ambient shocked interstellar medium. The X-ray derived chemical abundances will be useful in modeling X-ray spectra of other supernova remnants in the LMC, and they will be of general interest to the astronomical community.

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