Large Magellanic Cloud Distance from Cepheid Variables using Least Squares Solutions

Abstract

Distance to the Large Magellanic Cloud (LMC) is determined using the Cepheid variables in the LMC. We combine the individual LMC Cepheid distances obtained from the infrared surface brightness method and a dataset with a large number of LMC Cepheids. Using the standard least squares method, the LMC distance modulus can be found from the ZP offsets of these two samples. We have adopted both a linear P-L relation and a ``broken'' P-L relation in our calculations. The resulting LMC distance moduli are 18.48+-0.03 mag and 18.49+-0.04 mag (random error only), respectively, which are consistent to the adopted 18.50 mag in the literature.

2 pages and 1 figure, to appear in proceeding of "Galaxies in the Local Volume" Sydney 8-13 July 2007

References in corpus (2)

• Period-color and amplitude-color relations in classical Cepheid variables III: The Large Magellanic Cloud Cepheid models
• Period-color and amplitude-color relations in classical Cepheid variables V: The Small Magellanic Cloud Cepheid models

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• Three dimensional maps of the Magellanic Clouds using RR~Lyrae stars and Cepheids - I. The Large Magellanic Cloud
• The mass-loss, expansion velocities and dust production rates of carbon stars in the Magellanic Clouds
• Optical properties of amorphous carbon dust around C-stars: new constraints from 2MASS and Gaia observations
• Classical Cepheids, what else?