Theoretical Uncertainties in the Subgiant--Mass Age Relation and the Absolute Age of Omega Cen

Abstract

The theoretical uncertainties in the calibration of the relationship between the subgiant mass and age in metal-poor stars are investigated using a Monte Carlo approach. Assuming that the mass and iron abundance of a subgiant star are known exactly, uncertainties in the input physics used to construct stellar evolution models and isochrones lead to a Gaussian 1-sigma uncertainty of +/-2.9% in the derived ages. The theoretical error budget is dominated by the uncertainties in the calculated opacities. Observations of detached double lined eclipsing binary OGLEGC-17 in the globular cluster Omega Cen have found that the primary is on the subgiant branch with a mass of M = 0.809+/-0.012 M_sun and [Fe/H]= -2.29+/-0.15 (Kaluzny et al. 2001). Combining the theoretical uncertainties with the observational errors leads to an age for OGLEGC-17 of 11.10+/-0.67 Gyr. The one-sided, 95% lower limit to the age of OGLEGC-17 is 10.06 Gyr, while the one-sided, 95% upper limit is 12.27 Gyr.