X-ray Doppler Velocities and 3D Structure Of The Supernova Remnant N132D

Details X-ray Doppler Velocities and 3D Structure Of The Supernova Remnant N132D X-ray Doppler Velocities and 3D Structure Of The Supernova Remnant N132D

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008head...10.3103d&link_type=abstract

American Astronomical Society, HEAD meeting #10, #31.03

Astronomy and Astrophysics

Astronomy

Scientific paper

The oxygen-rich supernova remnant N132D in the Large Magellanic Cloud was observed with the High Energy Transmission Grating Spectrometer onboard the Chandra X-ray Observatory. Individual emission lines of oxygen, neon, magnesium, and silicon are observed and Doppler shifts have been measured. We find Doppler velocities of knots and filaments of only a few hundred km/s supporting previous abundance studies that concluded that the X-ray emission is mostly swept-up ISM and not ejecta. We have also begun to model the 3-dimensional structure of the X-ray emission using both the zeroth-order image and individual dispersed images of the remnant.

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