Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21725625v&link_type=abstract
American Astronomical Society, AAS Meeting #217, #256.25; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
A search for expanding, HI shells around galactic supernova remnants (SNR) was conducted using the Inner Galactic Plane Arecibo L-band Feed Array (I-GALFA) HI survey. This survey, which mapped out the distribution of HI emission within the galactic plane, spanned an area that included a total of thirty eight SNR positions. HI intensity was viewed over a velocity range of -150 km/s to +150 km/s, of which five SNRs were found to have an associated expanding HI shell, ten to have central HI emission, and six to have some HI absorption. The SNR G65.3+5.7 was selected to study more in depth because it appears to have HI emission that correlated with the optical and radio continuum emission. This supernova remnant has a very bright optical shell dominated by OIII emission with x-ray radiation at its center. The HI emitting shell was visible within the velocity range of -12 km/s to +10 km/s, which overlaps the systematic velocity of 8 ± 10 km/s derived in previous research, providing further evidence of the shell's association with the SNR. It was found to have a size of approximately 260’ across, yielding a physical radius of 38pc at a distance of 1kpc. The observed HI shell mass was derived by extrapolating the temperature brightness of the shell and the background from the HI images and doing an integration to yield a value of 2000Msolar. This value was then used to calculate a hydrogen number density of 0.353 cm-3. Assuming an initial explosion energy of 1051 ergs and a metallicity of 1, the expansion velocity of this shell was determined as 550 km/s and the age as approximately 21,000 years. These values for physical size, number density, expansion velocity, and age agree well with the values derived in previous optical, x-ray, and radio studies.
Kang Junhai
Vincent Chelsea
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