A new calibration of the extragalactic distance scale using Cepheids and RR Lyrae stars

Details A new calibration of the extragalactic distance scale using Cepheids and RR Lyrae stars A new calibration of the extragalactic distance scale using Cepheids and RR Lyrae stars

Nov 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...274...20s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 274, Nov. 1, 1983, p. 20-30.

Astronomy and Astrophysics

Astrophysics

62

Cepheid Variables, Cosmology, Magellanic Clouds, Milky Way Galaxy, Stellar Magnitude, Variable Stars, Calibrating, Distance, Globular Clusters, Light Curve, Stellar Luminosity, Stellar Parallax

Scientific paper

Visual absolute magnitudes of classical Cepheids, metal-poor RR Lyrae stars and short-period type II Cepheids have been determined with very high precision by combining a large number of old and new astrophysical data. Five independent methods (four observational and one theoretical) have been successfully used: (1) secular and statistical parallaxes; (2) moving-group parallaxes; (3) cluster main-sequence fitting; (4) the Baade-Wesselink method and its modifications; and (5) light-curve and velocity-curve fitting (the theoretical method). With these five adopted methods, the zero point of the galactic and extragalactic distance scale can be set on a relatively firm and self-consistent basis. Classical Cepheids and RR Lyrae stars now provide essentially identical distances to nearby galaxies: the distance modulus to the Large Magellanic Cloud is 18.5 and to the Small Magellanic Cloud is 18.8, both with an uncertainty of 0.1. The distance to the center of our Galaxy is 8.6 plus or minus 0.5 kiloparsecs. The major uncertainty in these values lies in the correction for interstellar extinction.

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