The Age Dependent Luminosities of the Red Giant Branch Bump, Asymptotic Giant Branch Bump, and Horizontal Branch Red Clump

Color-magnitude diagrams of globular clusters often exhibit a prominent horizontal branch (HB) and may also show features such as the red giant branch (RGB) bump and the asymptotic giant branch (AGB) bump. Stellar evolution theory predicts that the luminosities of these features will depend on the metallicity and age of the cluster. We calculate theoretical lines of 2 to 12 Gyr constant age RGB-bumps and AGB-bumps in the ∆V Bump–[Fe/H] diagram, which shows the brightness difference between the bump and the HB as a function of metallicity. In order to test the predictions, we identify giant branch bumps in new Hubble Space Telescope color-magnitude diagrams for 8 SMC clusters. First, we conclude that the SMC cluster bumps are RGB-bumps. The data for clusters younger than ∼6 Gyr are in fair agreement with our predictions for the relative age dependent luminosities of the HB and RGB-bump. The ∆V Bump data for clusters older than ∼6 Gyr demonstrate a less satisfactory agreement with our calculations. We conclude that ∼6 Gyr is lower bound to the age of clusters for which the Galactic globular cluster, age independent ∆V Bump–[Fe/H] calibration is valid. Application of the ∆V HB Bump–[Fe/H] diagram to stellar population studies is discussed. Department of Physics, University of California, Davis, CA 95616 Hubble Fellow