Combined BVRI and Hα / [SII] Observations of M31 SNRs

Details Combined BVRI and Hα / [SII] Observations of M31 SNRs Combined BVRI and Hα / [SII] Observations of M31 SNRs

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...182.0219m&link_type=abstract

American Astronomical Society, 182nd AAS Meeting, #02.19; Bulletin of the American Astronomical Society, Vol. 25, p.787

Astronomy and Astrophysics

Astronomy

Scientific paper

We present results of combined BVRI, Hα , and [SII] CCD observations of emission-line regions in M31. These regions contain complex stellar associations and extensive Hα emission. Much of the Hα emission is due to photo-ionization (Hriptsize II regions), but supernova remnants (SNRs) are also mixed in with the emission regions. Several groups (Blair et. al. 1981, D'Odorico et. al. 1980) have identified SNRs based on the [SII] to Hα ratio. While objects with a relatively high value of [SII] / Hα are very likely to be SNRs, this ratio is not very high for many SNRs. Such SNRs are therefore easily missed in optical searches for extragalactic SNRs. We present a different, complementary test for SNRs based on a comparison of the Hα flux and the presence or absence of hot, ionizing stars. Our combined BVRI, Hα , [SII] data has revealed ~ 200 objects which are candidate SNRs throughout M31 based on this test.

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