Department of Astronomy, P. Universidad Católica, Av. Vicuña Mackenna 4860, Casilla 306, Santiago 22, Chile e-mail: [jborisso;dante]@astro.puc.cl
2 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching b. München, Germany e-mail: email@example.com
3 Columbia University, Dept. of Astronomy, New York, USA e-mail: firstname.lastname@example.org
4 Lawrence Livermore National Laboratory, Livermore, California, USA e-mail: email@example.com
5 Mount Stromlo Observatory, Canberra ACT, Australia e-mail: firstname.lastname@example.org
Accepted: 24 March 2004
We present the radial velocities, metallicities and the K-band magnitudes of 74 RR Lyrae stars in the inner regions of the LMC. The intermediate resolution spectra and infrared images were obtained with FORS1 at the ESO VLT and with the SOFI infrared imager at the ESO NTT. The best 43 RR Lyrae with measured velocities yield an observed velocity dispersion of km s-1. We obtain a true LMC RR Lyrae velocity dispersion of km s-1, which is higher than the velocity dispersion of any other LMC population previously measured. This is the first empirical evidence for a kinematically hot, metal-poor halo in the LMC as discussed in Minniti et al. ([CITE]). Using Layden's (1994) modification of the method we measured the metallicity for 23 of our stars. The mean value is dex. The absolute magnitudes MV and MK of RR Lyrae stars are linear functions of metallicity. In the V band, our data agree with the Olech et al. ([CITE]) relation, in the K band the slope is flatter. The average apparent V luminosity of 70 RR Lyrae stars is and the average K luminosity of 37 RR Lyrae stars is . There is no obvious relation between apparent V magnitude and Log P, while the RR Lyrae K band magnitudes show a well defined linear trend with Log P. Using the Bono et al. ([CITE]) and Bono et al. (2003) theoretical Near-Infrared Period-Luminosity-Metallicity relations we calculate the LMC distance modulus .
Key words: galaxies: Magellanic clouds / stars: variables: RR Lyrae / galaxies: formation
Based on observations collected with the Very Large Telescope and the New Technology Telescope of the European Southern Observatory within the Observing Programs 64.N-0176(B) and 70.B-0547.
© ESO, 2004