Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20915619b&link_type=abstract
2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #156.19; Bulletin of the American Astronomical Society,
Astronomy and Astrophysics
Astronomy
Scientific paper
The brightest supernova remnant in the Magellanic Clouds, N132D, belongs to a rare class of oxygen-rich remnants, consisting of about a dozen objects which show emission from pure heavy-element ejecta in their optical spectra. They are generally thought to originate in explosions of massive stars which produce large amounts of O, although only a tiny fraction of that O is found to emit at optical wavelengths. We report detection of the "missing" O at X-ray wavelengths in a recent deep (100 ksec) Chandra ACIS observation of N132D. Ejecta spectra are dominated by strong lines of Heand H-like O, and Ne and Mg emission enhancements are also apparent. There is a good match between X-rayand optically-emitting ejecta, as shown by comparison between subarcsecond-resolution Chandra and Hubble images. Because optical ejecta are concentrated in a 5 pc radius elliptical expanding shell, most of ejecta X-ray emission also originates in this shell. We interpret these new Chandra observations in a framework of a core-collapse supernova explosion of a massive star within a wind-blown bubble, about 3000 yr ago. We discuss constraints on the initial main-sequence mass of the supernova progenitor posed by detection of large amounts of O in X-rays.
Borkowski Kazimierz J.
Hendrick Sean Patrick
Reynolds Stephen P.
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