Can Ejecta-Dominated Supernova Remnants be Typed from their X-ray Spectra? The Case of G337.2-0.7

Details Can Ejecta-Dominated Supernova Remnants be Typed from their X-ray Spectra? The Case of G337.2-0.7 Can Ejecta-Dominated Supernova Remnants be Typed from their X-ray Spectra? The Case of G337.2-0.7

2006-04-11

arxiv.org/abs/astro-ph/0604246v1

Astrophys.J.646:982-1000,2006

Astronomy and Astrophysics

Astrophysics

21 pages emulateapj including 9 figures, 5 tables, accepted for publication in the Astrophysical Journal

Scientific paper

10.1086/505018

In this paper we use recent X-ray and radio observations of the ejecta-rich Galactic supernova remnant (SNR) G337.2-0.7 to determine properties of the supernova (SN) explosion that formed this source. H I absorption measurements from the Australia Telescope Compact Array (ATCA) constrain the distance to G337.2-0.7 to lie between 2.0 +/- 0.5 and 9.3 +/- 0.3 kpc. Combined with a clear radio image of the outer blast-wave, this distance allows us to estimate the dynamical age (between 750 and 3500 years) from the global X-ray spectrum obtained with the XMM-Newton and Chandra observatories. The presence of ejecta is confirmed by the pattern of fitted relative abundances, which show Mg, Ar and Fe to be less enriched (compared to solar) than Si, S or Ca, and the ratio of Ca to Si to be 3.4 +/- 0.8 times the solar value (under the assumption of a single electron temperature and single ionization timescale). With the addition of a solar abundance component for emission from the blast-wave, these abundances (with the exception of Fe) resemble the ejecta of a Type Ia, rather than core-collapse, SN. Comparing directly to models of the ejecta and blast-wave X-ray emission calculated by evolving realistic SN Ia explosions to the remnant stage allows us to deduce that one-dimensional delayed detonation and pulsed delayed detonation models can indeed reproduce the major features of the global spectrum. In particular, stratification of the ejecta, with the Fe shocked most recently, is required to explain the lack of prominent Fe-K emission.

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