The stellar population in the Wolf-Rayet knot in NGC 5430

Details The stellar population in the Wolf-Rayet knot in NGC 5430 The stellar population in the Wolf-Rayet knot in NGC 5430

Jan 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...172...43k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 172, no. 1-2, Jan. 1987, p. 43-50.

Astronomy and Astrophysics

Astrophysics

12

Emission Spectra, Star Distribution, Stellar Spectrophotometry, Wolf-Rayet Stars, H Ii Regions, Nebulae, Stellar Temperature, Ultraviolet Spectra, Visible Spectrum

Scientific paper

The barred spiral NGC 5430 contains an extremely luminous H II region showing very strong He II and N III Wolf-Rayet (WR) emission features. Spectrophotometry from 1200 - 7000 Å has been obtained. From these data, limits on the reddening and effective temperature of the stellar population are derived; Teff is between 25000 and 35000K. No UV emission lines are clearly detected. The Hα linewidth implies a very short timescale for star formation here, less than 107yr for ≡5×105 OB and WR stars. Hα photometry shows a population of normal H II regions below 3% of the flux of the giant WR complex. The two most luminous of these are closest to the WR knot; the rest appear to have a normal Hα luminosity function.

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