Wolf-Rayet stars in the giant H II region NGC 604

Details Wolf-Rayet stars in the giant H II region NGC 604 Wolf-Rayet stars in the giant H II region NGC 604

Sep 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...248.1015d&link_type=abstract

Astrophysical Journal, Part 1, vol. 248, Sept. 15, 1981, p. 1015-1020.

Other

68

H Ii Regions, Nebulae, Stellar Spectra, Wolf-Rayet Stars, Emission Spectra, Hydrogen Ions, Spectral Line Width, Stellar Evolution

Scientific paper

Spectra obtained at various positions in NGC 604, the brightest H II region in M33, show the emission features typical of Wolf-Rayet (W-R) stars. By comparing these spectra of NGC 604 with data for the other W-R stars, it is determined from the equivalent widths of the Wolf-Rayet bands that about 50% of the observed continuum is due to W-R stars. Since most of the light in the B and V bandpasses from a Population I association is due to main sequence and supergiant O, B, and A stars, and the W-R stars have comparable absolute magnitudes at these wavelengths, a ratio of W-R to blue stars of about 1.0 is estimated. The presence of some 50 W-R stars with a mean type of WN 7 is interpreted as the result of a single burst of star formation approximately 4,000,000 years ago in the core of NGC 604.

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