The optical emission from the supernova remnant HB 3

Details The optical emission from the supernova remnant HB 3 The optical emission from the supernova remnant HB 3

Mar 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983pasp...95..196f&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 95, March 1983, p. 196-200.

Astronomy and Astrophysics

Astronomy

5

Emission Spectra, Light Emission, Radio Sources (Astronomy), Stellar Envelopes, Supernova Remnants, Astronomical Photography, Atomic Spectra, H Alpha Line, H Ii Regions

Scientific paper

The supernova remnant HB 3 was first detected as a radio source by Brown and Hazard (1953). On the basis of subsequent radio studies, it was concluded that the object was a supernova remnant (SNR). HB 3 is located at the far western edge of the H II region/molecular cloud complex W3-W4-W5 (IC 1795-1805-1848). However, a physical association of HB 3 with this complex is uncertain. In the present investigation, attention is called to the probability that HB 3 exhibits a more extensive optical emission structure than previously realized, and one which agrees well with both the position and morphology of the radio emission. It is found that narrow-passband optical images strongly suggest an almost complete optical emission shell for HB 3. Spectroscopic observations are, however, required to confirm that this emission is characteristic of a SNR.

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