The Galactic Cepheid period-luminosity relation from the visual surface brightness method

Details The Galactic Cepheid period-luminosity relation from the visual surface brightness method The Galactic Cepheid period-luminosity relation from the visual surface brightness method

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...329..790g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 329, June 15, 1988, p. 790-796. Research supported by the American Astronom

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B Stars, Cepheid Variables, Open Clusters, Stellar Luminosity, Stellar Magnitude, Stellar Oscillations, Brightness Distribution, Computational Astrophysics, Radial Velocity, Southern Hemisphere

Scientific paper

The distances of 52 southern hemisphere Galactic Cepheids covering a period range of 3 to 40 days are determined using the visual surface brightness method (VSBM). Absolute magnitudes of these stars are calculated, and a period-luminosity relation of small dispersion is obtained which is based on twice as many Cepheids as any former calibration. Essential agreement is found between the surface brightness and the ZAMS-fitting distance scale of Caldwell and Coulson (1987). Cepheid absolute magnitudes based on Stro["!mgren photometry of open cluster B stars are on average 0.2 mag fainter than these scales. Advantages and drawbacks of the present version of the VSBM are discussed, and it is concluded that its present degree of refinement is adequate to determine the Cepheid luminosity zero point to better than 0.2 mag. The slope of the visual surface brightness-color relation valid for Cepheids has now been established to a high degree of confidence.

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