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A new Large Magellanic Cloud K-band distance from precision measurements of nearby red clump stars

Authors

  • C. D. Laney,

    Corresponding author
    1. Department of Physics and Astronomy, N283 ESC, Brigham Young University, Provo, UT 84601, USA
    2. South African Astronomical Observatory, PO Box 9, Observatory 7935, South Africa
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  • M. D. Joner,

    Corresponding author
    1. Department of Physics and Astronomy, N283 ESC, Brigham Young University, Provo, UT 84601, USA
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  • G. Pietrzyński

    Corresponding author
    1. Universidad de Concepción, Departamento de Astronomia, Casilla 160-C, Concepción, Chile
    2. Warsaw University Observatory, Al Ujazdowskie 4, 00-478 Warsaw, Poland
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E-mail: cephradius@yahoo.com (CDL); jonerm@forty-two.byu.edu (MDJ); pietrzyn@sirius.astrouw.pl (GP)

ABSTRACT

High-precision (inline image) new JHK observations of 226 of the brightest and nearest red clump stars in the solar neighbourhood are used to determine distance moduli for the Large Magellanic Cloud (LMC). The resulting K- and H-band values of 18.47 ± 0.02 and 18.49 ± 0.06 imply that any correction to the K-band Cepheid PL relation due to metallicity differences between Cepheids in the LMC and the solar neighbourhood must be quite small.

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