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تسجيل مستخدم جديدThe Ages of 55 Globular Clusters as Determined Using an Improved delta V_TO^HB Method Along with Color-Magnitude Diagram Constraints, and Their Implications for Broader Issues
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Ages have been derived for 55 globular clusters (GCs) from overlays of isochrones onto the turnoff photometry, assuming distances based on fits of zero-age horizontal branch (ZAHB) models to the lower bound of the observed distributions of HB stars. The error bar arising just from the fitting of ZAHBs and isochrones is ~ +/- 0.25 Gyr, while that associated with distance and chemical abundance uncertainties is ~ +/- 1.5-2 Gyr. Ages vary from mean values of ~12.5 Gyr at [Fe/H] < -1.7 to ~11 Gyr at [Fe/H] > -1.0. At intermediate metallicities, the age-metallicity relation (AMR) appears to be bifurcated: one branch apparently contains clusters with disk-like kinematics, whereas the other branch is populated by clusters with halo-type orbits. There is no apparent dependence of age on Galactocentric distance (R_G) nor is there a clear correlation of HB type with age. Subtle variations in the subgiant branch (SGB) slopes of [Fe/H] < -1.5 GCs are tentatively attributed to helium abundance differences. Curiously, GCs with steep M13-like SGBs tend to be massive systems, located at small R_G, that show the strongest evidence for multiple stellar populations. The others are typically low-mass systems that, at the present time, should not be able to retain the matter lost by mass-losing stars. The apparent separation of the two groups in terms of their present-day gas retention properties is difficult to understand if all GCs were initial ~20 times their current masses. The lowest mass systems may have never been able to retain enough gas to produce a significant population of second-generation stars; in this case, the observed light element abundance variations were presumably present in the gas out of which the observed cluster stars formed.
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