The level of agreement between theoretical and observed globular cluster\n luminosity functions

Luminosity functions from theoretical stellar evolution calculations are\ncompared with observed ones of several galactic globular clusters (M30, M92,\nM68, NGC6397, M4, M80, NGC6352, NGC1851). Contrary to earlier results of\nFaulkner & Stetson (1993) and Bolte (1994) we find no significant discrepancy\nthat could indicate the neglect of important physical effects in the models.\nHowever, it is confirmed that the subgiant branch is the most sensitive part\nand shows the largest deviations in the luminosity function comparison, if\nparameters are unappropriate. We also find that the main sequence is suited\nless than the Red Giant Branch for the calibration of theoretical luminosity\nfunctions. While for individual clusters different changes in the model\nassumptions might resolve mismatches, there is no systematic trend visible. It\nrather appears that the quality of the luminosity function in the subgiant part\nis insufficient and that improved observations of this particular region are\nnecessary for a better comparison. At the present quality of luminosity\nfunctions theory is in agreement with observation and a postulation of WIMPs\nacting in stellar cores does not seem to be justified. Actually, fits using\nisothermal core models on the main sequence appear to be worse than those with\nstandard stellar evolution assumptions.\n