The region of the supernova remnant MSH 15-52 revisited - A new thermal H II region, H II G 320.5-1.4

Details The region of the supernova remnant MSH 15-52 revisited - A new thermal H II region, H II G 320.5-1.4 The region of the supernova remnant MSH 15-52 revisited - A new thermal H II region, H II G 320.5-1.4

Jun 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...180...65l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 180, no. 1-2, June 1987, p. 65-72.

Astronomy and Astrophysics

Astrophysics

15

Blue Stars, Hydrogen Clouds, Star Clusters, Supernova Remnants, Astronomical Photography, Radial Velocity, Stellar Color, Stellar Structure, Wolf-Rayet Stars

Scientific paper

The authors revisited the stellar and nebular content in the direction of MSH 15-52. This search was initiated by the discovery of a new Hα thermal region H II G 320.5-1.4 with velocity VLSR = -43 km s-1, extending over an area similar to MSH 15-52, and clearly distinct from the foreground H II region BBW 28802. From a rediscussion of the reddening and distances of hot stars with available spectra in the direction l = 320°, it is found that they constitute a single stellar association (Cir OB1) at a distance about 4 kpc, probably not much more extended than 80×80 pc. This association contains the cluster Pis 20, four WR stars and a number of stars with ages in the range 4 - 10×106yr. It is the excitation source of H II G 320.5-1.4. In such an association, bubbles may have formed previously to the explosion of supernovae; also, several supernovae may have exploded recently. Thus it is not unlikely that MSH 15-52 originated from the same SN explosion as PSR 1509-58 and expanded freely into a bubble; on the other hand, it would not be surprising that two different supernovae exploded close in time and space.

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