A Chandra X-Ray Measurement of the Expansion Rate of G266.2-1.2

Details A Chandra X-Ray Measurement of the Expansion Rate of G266.2-1.2 A Chandra X-Ray Measurement of the Expansion Rate of G266.2-1.2

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.1804a&link_type=abstract

American Astronomical Society, HEAD meeting #11, #18.04; Bulletin of the American Astronomical Society, Vol. 41, p.686

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Scientific paper

The age and distance of the supernova remnant G266.2-1.2 are a source of controversy. Some argue that the spectrum of the remnant possesses line features associated with the decay of titanium-44. In this case, the remnant must be young (600-1200 yr) and close (0.1-0.5 kpc). Others find little or no evidence of such features and argue that the large absorption column density places the remnant beyond Vela (> 0.25 kpc) and possibly in the Vela Molecular Ridge (1-2 kpc). At this distance, the remnant is most likely several thousand years old. To help resolve this controversy, we reobserved the northeastern rim of the remnant with the ACIS on Chandra. We present a comparison of the Chandra X-ray data from 2003 and 2008. This comparison provides a measure of the the expansion rate of the northeastern rim. To the extent that this motion is representative of the remnant as a whole, we present constraints on the age of the remnant. GEA and JCH are supported by the contract SV3-73016 between MIT and the Smithsonian Astrophysical Observatory. The Chandra X-Ray Center at the Smithsonian Astrophysical Observatory is operated on behalf of NASA under the contract NAS8-03060.

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