On the Metallicity Dependence of Classical Cepheid Light Amplitudes

Abstract

Classical Cepheids remain a cornerstone of the cosmic distance scale, and thus characterizing the dependence of their light amplitude on metallicity is important. Period-amplitude diagrams constructed for longer-period classical Cepheids in IC 1613, NGC 3109, SMC, NGC 6822, LMC, and the Milky Way imply that very metal-poor Cepheids typically exhibit smaller V-band amplitudes than their metal-rich counterparts. The results provide an alternate interpretation relative to arguments for a null and converse metallicity dependence. The empirical results can be employed to check predictions from theoretical models, to approximate mean abundances for target populations hosting numerous long-period Cepheids, and to facilitate the identification of potentially blended or peculiar objects.

To appear in ApSS

References in corpus (21)

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Cited by in corpus (11)

• The Cepheid Distance to the Seyfert 1 Galaxy NGC 4151
• Optical Identification of Cepheids in 19 Host Galaxies of Type Ia Supernovae and NGC 4258 with the Hubble Space Telescope
• TESS observations of Cepheid stars: first light results
• Anchors for the Cosmic Distance Scale: the Cepheids U Sgr, CF Cas and CEab Cas
• Determination of the iron content of Cepheids from the shape of their light curves
• On the Form of the Spitzer Leavitt Law and its Dependence on Metallicity
• A New Absolute Magnitude Calibration for Red Clump Stars
• Metallicity estimation of MW, SMC and LMC classical Cepheids from the shape of the $V$- and $I$-band light curves
• Precise Fourier parameters of Cepheid Radial Velocity Curves
• Evidence for Photometric Contamination in Key Observations of Cepheids in the Benchmark Galaxy IC 1613
• Reconstruction of Cepheid Radial Velocity Curves from the shape of the V-band Light Curves