Mean Absolute Magnitudes of OB+, OB, and OB- Stars

Details Mean Absolute Magnitudes of OB+, OB, and OB- Stars Mean Absolute Magnitudes of OB+, OB, and OB- Stars

May 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996pasp..108..395r&link_type=abstract

Publications of the Astronomical Society of the Pacific, v.108, p.395

Astronomy and Astrophysics

Astronomy

7

Scientific paper

Photoelectric Beta values for over 1200 stars listed in Stephenson and Sanduleak's Catalog of Luminous Stars in the Southern Milky Way are used in conjunction with Reed and Beatty's (1995) M_V(Beta) calibration to determine mean absolute magnitudes for Nassau and Stephenson's (1960: NS) objective-prism based OB+, OB, and OB- classes of stars. The NS sequence proves to be one of decreasing luminosity, but a systematic effect is present: the mean absolute magnitude of stars in each class is a function of apparent magnitude V. MK-quality spectral classifications for a subset of over 300 stars indicates that the source of this effect appears to be inclusion of increasing numbers of dwarf stars in each NS class with increasing V. The M_V(Beta) calibration indicates taht, at a given V, the OB+ (OB-) stars are intrinsically ~0.8 magnitudes brighter (fainter) than the OB stars; while these differences are statistically significant, the range of absolute magnitudes present in each type, sigma (M_V) ~1.1, is large enough to render NS classifications only marginally useful as luminosity discriminants. However, our results can be of use in estimating absolute magnitudes for stars for which only an NS classification is available, and in checking for inconsistencies between NS classifications and Beta-V photometry. (SECTION: Stars)

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