The RR Lyrae period–K-luminosity relation for globular clusters: an observational approach†

  1. A. Sollima1,*,
  2. C. Cacciari2,
  3. E. Valenti2

Article first published online: 22 SEP 2006

DOI: 10.1111/j.1365-2966.2006.10962.x

Issue

Monthly Notices of the Royal Astronomical Society

Monthly Notices of the Royal Astronomical Society

Volume 372, Issue 4, pages 1675–1680, November 2006

Additional Information

How to Cite

Sollima, A., Cacciari, C. and Valenti, E. (2006), The RR Lyrae period–K-luminosity relation for globular clusters: an observational approach. Monthly Notices of the Royal Astronomical Society, 372: 1675–1680. doi: 10.1111/j.1365-2966.2006.10962.x

Author Information

  1. 1

    Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, Bologna, 40127-I, Italy

  2. 2

    INAF Osservatorio Astronomico di Bologna, via Ranzani 1, Bologna, 40127-I, Italy

* Based on observations collected at the European Southern Observatory within the observing programs 49.5-0021, 51.5-0024, 59.E-0340, 64.N-0038, 68.D-0287 and at the Telescopio Nazionale Galileo.
E-mail: antonio.sollima@bo.astro.it (AS)

Publication History

  1. Issue published online: 13 OCT 2006
  2. Article first published online: 22 SEP 2006
  3. Accepted 2006 August 18. Received 2006 August 11; in original form 2006 July 4

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Keywords:

  • methods: observational;
  • techniques: photometric;
  • stars: distances;
  • stars: variables: other;
  • infrared: stars

ABSTRACT

The period–metallicity–K-band luminosity (PLK) relation for RR Lyrae stars in 15 Galactic globular clusters and in the Large Magellanic Cloud (LMC) globular cluster Reticulum has been derived. It is based on accurate near-infrared (K) photometry combined with Two-Micron All-Sky Survey (2MASS) and other literature data. The PLK relation has been calibrated and compared with the previous empirical and theoretical determinations in literature. The zero point of the absolute calibration has been obtained from the K magnitude of RR Lyr whose distance modulus has been measured via trigonometric parallax with Hubble Space Telescope (HST). Using this relation, we obtain a distance modulus to the LMC of (m−M)0= 18.54 ± 0.15 mag, in good agreement with recent determinations based on the analysis of Cepheid variable stars.

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