An Archival XMM-Newton Study of the Large Magellanic Cloud Supernova Remnant N132D

Details An Archival XMM-Newton Study of the Large Magellanic Cloud Supernova Remnant N132D An Archival XMM-Newton Study of the Large Magellanic Cloud Supernova Remnant N132D

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21923916p&link_type=abstract

American Astronomical Society, AAS Meeting #219, #239.16

Astronomy and Astrophysics

Astrophysics

Scientific paper

We present the results of an analysis of the archival XMM-Newton EPIC data (totaling more than 500ks) of the brightest X-ray supernova remnant (SNR) in the Large Magellanic Cloud (LMC) N132D. N132D has been routinely observed by XMM-Newton over its 11 year mission as a calibration target. We have combined the data from all calibration observations suitable for scientific analysis to create the deepest X-ray images of N132D. N132D has been classified as an ``Oxygen-rich'' remnant based on the UV and optical spectra which show emission from
C, O, Ne, Mg, and Si. These spectra of the bright optical knots do not show any emission from elements with higher Z than Si, yet the nucleosynthesis models predict significant quantities of these higher Z elements. Our preliminary analysis of the deep XMM data clearly shows emission lines from S, Ar, Ca, and Fe, with indications of other possible lines between Ca and Fe. We compare the estimated amount of these high Z elements to various nucleosynthesis models to constrain the possible progenitor.
This research was supported by the NASA Astrophysics Data Analysis Program (ADAP) through grant number NNX11AD17G.

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