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1997•The Astronomical JournalRequires access

Chemical Abundances of Galactic Cepheid Variables that Calibrate the P-L Relation

Anne M. Fry, Bruce W. Carney

Open publisher page 89 citations

Abstract

We have completed spectroscopic studies of 23 Galactic cepheids to determine possible metallicity effects on measuring the zero point of the P-L relation. We find a spread of 0.4 dex in [Fe/H], which is not the result of either observational scatter or of a metallicity gradient within the Galactic disk. We find a smaller, less significant spread of 0.2 dex in [alpha /Fe]. Our results are robust, determined by constancy of [Fe/H] derived at differing temperatures throughout the pulsational cycle, and abundances of two dwarfs compared to U Sgr in the cluster M 25. We discuss briefly the effect of metallicity on the P-L relation. We also argue that EV Sct and QZ Nor are overtone pulsators, and that the latter is not a member of the cluster NGC 6067.

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What this paper is about

We have completed spectroscopic studies of 23 Galactic cepheids to determine possible metallicity effects on measuring the zero point of the P-L relation. We find a spread of 0.4 dex in [Fe/H], which is not the result of either observational scatter or of a metallicity gradient within the Galactic disk. We find a smaller, less significant spread of 0.2 dex in [alpha /Fe]. Our results are robust, determined by constancy of [Fe/H] derived at differing temperatures throughout the pulsational cycle, and abundances of two dwarfs compared to U Sgr in the cluster M 25. We discuss briefly the effect of metallicity on the P-L relation. We also argue that EV Sct and QZ Nor are overtone pulsators, and that the latter is not a member of the cluster NGC 6067.

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Available abstract

We have completed spectroscopic studies of 23 Galactic cepheids to determine possible metallicity effects on measuring the zero point of the P-L relation. We find a spread of 0.4 dex in [Fe/H], which is not the result of either observational scatter or of a metallicity gradient within the Galactic disk. We find a smaller, less significant spread of 0.2 dex in [alpha /Fe]. Our results are robust, determined by constancy of [Fe/H] derived at differing temperatures throughout the pulsational cycle, and abundances of two dwarfs compared to U Sgr in the cluster M 25. We discuss briefly the effect of metallicity on the P-L relation. We also argue that EV Sct and QZ Nor are overtone pulsators, and that the latter is not a member of the cluster NGC 6067.

Key concepts: Cepheid variable, Physics, Astrophysics, Relation (database), Astronomy, Stars, Computer science, Database

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