We present new near-infrared (J and K) magnitudes for 114 RR Lyrae stars in the globular cluster omega Centauri (NGC 5139), which we combine with data from the literature to construct a sample of 180 RR Lyrae stars with J and K mean magnitudes on a common photometric system. This is currently the largest such sample in any stellar system. We also present updated predictions for J- and K-band period-luminosity relations for both fundamental and first-overtone RR Lyrae stars, based on synthetic horizontal branch models with metal abundance ranging from Z = 0.0001 to 0.004. By adopting for the omega Cen variables with measured metal abundances an alpha-element enhancement of a factor of 3 (approximate to 0.5 dex) with respect to iron, we find a true distance modulus mu(0) = 13.70 +/- 0.06 +/- 0.06 ( random and systematic errors, respectively), corresponding to a distance d = 5.5 +/- 0.03 +/- 0.03 kpc. Our estimate is in excellent agreement with the distance inferred for the eclipsing binary OGLEGC 17, but differ significantly from the recent distance estimates based on cluster dynamics and on high-amplitude delta Scuti stars.
Del Principe, M., Piersimoni, A.m., Storm, J., Caputo, F., Bono, G., Stetson, P.b., et al. (2006). A pulsational distance to omega Centauri based on near-infrared period-luminosity relations of RR Lyrae stars. THE ASTROPHYSICAL JOURNAL, 652(1 I), 362-369 [10.1086/508136].
A pulsational distance to omega Centauri based on near-infrared period-luminosity relations of RR Lyrae stars
BONO, GIUSEPPE;BUONANNO, ROBERTO;
2006-01-01
Abstract
We present new near-infrared (J and K) magnitudes for 114 RR Lyrae stars in the globular cluster omega Centauri (NGC 5139), which we combine with data from the literature to construct a sample of 180 RR Lyrae stars with J and K mean magnitudes on a common photometric system. This is currently the largest such sample in any stellar system. We also present updated predictions for J- and K-band period-luminosity relations for both fundamental and first-overtone RR Lyrae stars, based on synthetic horizontal branch models with metal abundance ranging from Z = 0.0001 to 0.004. By adopting for the omega Cen variables with measured metal abundances an alpha-element enhancement of a factor of 3 (approximate to 0.5 dex) with respect to iron, we find a true distance modulus mu(0) = 13.70 +/- 0.06 +/- 0.06 ( random and systematic errors, respectively), corresponding to a distance d = 5.5 +/- 0.03 +/- 0.03 kpc. Our estimate is in excellent agreement with the distance inferred for the eclipsing binary OGLEGC 17, but differ significantly from the recent distance estimates based on cluster dynamics and on high-amplitude delta Scuti stars.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
