Radioactivity, Particle Acceleration, And Supernova Ejecta In The Youngest Galactic SNR G1.9+0.3

Details Radioactivity, Particle Acceleration, And Supernova Ejecta In The Youngest Galactic SNR G1.9+0.3 Radioactivity, Particle Acceleration, And Supernova Ejecta In The Youngest Galactic SNR G1.9+0.3

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011head...12.3425b&link_type=abstract

American Astronomical Society, HEAD meeting #12, #34.25

Astronomy and Astrophysics

Astronomy

Scientific paper

A supernova explosion around 1900 produced a young remnant G1.9+0.3, presumably located near the Galactic center, that can now be studied at X-ray and radio wavelengths. A deep (980 ks) Chandra X-ray observation of G1.9+0.3 has just been completed (May and July 2011). We report first results based on this observation. In the interior, there is an excess of counts near 4.1 keV over a nonthermal continuum. A preliminary Markov chain Monte Carlo modeling of this feature with a Gaussian line and an underlying power-law continuum gives line energy of 4.1 keV and FWHM of 35000 km/s (but with a large 90% confidence interval from 11000 to 59000 km/s). The estimated line strength is nearly identical to our previous estimate based on the shorter-duration Chandra observations from 2007 and 2009. If this line is identified with radioactive 44Sc, 10-5 solar masses of 44Ti was produced in the explosion.
The radio-bright northern shell shows K lines of Si, S, Ar, and Fe, with no Sc present. The Fe line is moderately broad (FWHM of 12000 km/s). A plane shock fit to the spectrum indicates an oversolar (1.6 solar) Fe abundance and plasma temperature of 3.7 keV. These are presumably heavy-element ejecta heated to high temperatures in the reverse shock.
The total X-ray flux increased by 2.8% between the 2009 and 2011 Chandra observations. G1.9+0.3 is the only Galactic supernova remnant that is brightening at X-ray and radio wavelengths.
We also present preliminary results of spectro-spatial analysis of the Chandra data cube, based on a method described by Krishnamurthy, Raginsky, & Willett (2010). Our aim is to study spatial distribution of the supernova ejecta, and variations in the nonthermal synchrotron continuum that dominates the total X-ray spectrum.

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