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The optical emission from the supernova remnant HB 3The 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.
Document ID
Document Type
Reprint (Version printed in journal)
External Source(s)
Fesen, R. A. (NASA Goddard Space Flight Center Greenbelt, MD, United States)
Gull, T. R. (NASA Goddard Space Flight Center Laboratory for Astronomy and Solar Physics, Greenbelt, MD, United States)
Date Acquired
August 11, 2013
Publication Date
March 1, 1983
Publication Information
Publication: Astronomical Society of the Pacific, Publications
Volume: 95
ISSN: 0004-6280
Subject Category
Distribution Limits