HI SNRs, FV Wings, and the Structure of the ISM

Details HI SNRs, FV Wings, and the Structure of the ISM HI SNRs, FV Wings, and the Structure of the ISM

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aspc..323..123k&link_type=abstract

Star Formation in the Interstellar Medium: In Honor of David Hollenbach, Chris McKee and Frank Shu, ASP Conference Proceedings,

Statistics

Scientific paper

We discuss the statistics of old supernova remnants (SNRs) with expanding schi shells, or ``schi SNRs", in the Galaxy. Systematic schi 21-cm emission line studies have detected fast-moving atomic gas associated with 25 SNRs, which is about 10% of the known radio/X-ray SNRs. This number is much less than the expected number of visible schi SNRs if the interstellar medium is filled with warm neutral medium. A plausible explanation is that most of the schi SNRs are too faint to be visible in radio or X-ray. Large-scale (ℓ, v) diagrams of the schi 21-cm emission in the Galactic plane show broad wings which extend to velocities forbidden by the Galactic rotation. Many of these ``forbidden-velocity (FV)" wings are not associated with known SNRs or known external galaxies and could be candidates for heretofore unidentified old schi SNRs. We discuss the properties of the FV wings and the implications for the structure of the interstellar medium.

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