## Abstract

Shapes of RR Lyrae light curves can be described in terms of Fourier coefficients that past research has linked with physical characteristics such as luminosity, mass, and temperature. Fourier coefficients have been derived for the V and R light curves of 785 overtone RR Lyrae variables in 16 MACHO fields near the bar of the LMC. In general, the Fourier phase differences φ_{21}, φ_{31}, and φ_{41} increase and the amplitude ratio R_{21} decreases with increasing period. The coefficients for both the V and R magnitudes follow these patterns, but the phase differences for the R curves are on average slightly greater, and their amplitudes are about 20% smaller, than the ones for the F curves. The φ_{31} and R_{21} coefficients have been compared with those of the first-overtone RR Lyrae variables in the Galactic globular clusters NGC 6441, M107, M5, M3, M2, ω Centauri, and M68. The results indicate that many of the LMC variables have properties similar to the ones in M2, M3, M5, and the Oosterhoff type I variables in ω Cen, but they are different from the Oosterhoff type II variables in ω Cen. Equations derived from hydrodynamic pulsation models have been used to calculate the luminosity and temperature for the 330 bona fide first-overtone variables. The results indicate that they have log L in the range 1.6-1.8 L_{⊙} and log T _{eff} between 3.85 and 3.87. Based on these temperatures, a mean color excess E(V-R) = 0.08 mag, equivalent to E(B-V] = 0.14 mag, has been estimated for these 330 stars. The 80 M5-like variables (selected according to their location in the φ_{31}-log P plot) are used to determine an LMC distance. After correcting for the effects of extinction and crowding, a mean apparent magnitude 〈V_{0}〉 = 18.99 ± 0.02 (statistical) ± 0.16 (systematic) has been estimated for these 80 stars. Combining this with a mean absolute magnitude M_{V} = 0.56 ± 0.06 for M5-like stars derived from Baade-Wesselink analyses, main-sequence fitting, Fourier parameters, and the trigonometric parallax of RR Lyrae, we derive an LMC distance modulus μ = 18.43 ± 0.06 (statistical) ± 0.16 (systematic) mag. The large systematic error arises from the difficulties of correcting for interstellar extinction and for crowding.

Original language | English |
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Pages (from-to) | 334-354 |

Number of pages | 21 |

Journal | Astronomical Journal |

Volume | 127 |

Issue number | 1 1777 |

DOIs | |

Publication status | Published - Jan 2004 |

## Keywords

- Galaxies: distances and redshifts
- Magellanic Clouds
- RR Lyrae variable

## ASJC Scopus subject areas

- Astronomy and Astrophysics
- Space and Planetary Science