The Globular Cluster Luminosity Function as a Distance Indicator: Dynamical Effects

The dynamical evolution of the globular cluster systems in galaxies is predicted, based on the standard dynamical theory normalized to the example of the Milky Way. The major processes varying with the galactocentric distance are the tidal shocks and dynamical friction. Our simple model explains, on a quantitative basis, the observed differences of the inner and outer populations of globular clusters. We can thus calculate corrections for dynamical evolution for the luminosity function of globular clusters with the assumption that the initial luminosity function is identical in all galaxies (and we can test this assumption as well, in certain cases). Then we can compute the expected distribution of absolute magnitudes and compare it with the observed distribution of apparent magnitudes to estimate the distance moduli for M31 and M87. Using this new method we find (dmM31 = 24.05 ± 0.23, dmM87 = 30.83 ± 0.17) as compared to current best estimates using other methods of (dmM31 = 24.30 ± 0.20, dmM87 = 31.0±0.1). As a check on the method we compute, and compare with observations, the differences between the inner and outer globular clusters in all three galaxies. This new method, coupled with HST observations, promises to provide an independent method of estimating distances to galaxies with recession velocities ∼< 10, 000 km s−1, or d ∼< 100h−1 Mpc. Subject headings: globular clusters: general — galaxies: star clusters — galaxies: distances and redshifts — galaxies: individual (M31, M87)