The Luminosity Function of Globular Clusters as an Extragalactic Distance Indicator
Abstract
The absolute magnitude M* of the peak of the globular cluster luminosity function (GCLF), approximated by a Gaussian, can be calibrated independently in the Galaxy and M 31 through RR Lyr stars and Cepheids, respectively. They yield, in perfect agreement, M*_B = -6.93+-0.08 and M*_V = -7.62+-0.08. Application of these values to the GCLFs in the Leo Group (n=2), the Virgo cluster (n=8), and the Coma cluster (n=2) gives distances which agree with the best determinations from other methods. However, the corresponding distance of the Fornax cluster (n=7) is significantly underestimated, and the distances of several field galaxies are inconsistent. A second parameter, like the width of the GCLF or the color of the peak, is apparently needed to control differences in the GC formation history.
Cite
@article{arxiv.astro-ph/9903005,
title = {The Luminosity Function of Globular Clusters as an Extragalactic Distance Indicator},
author = {G. A. Tammann and A. Sandage},
journal= {arXiv preprint arXiv:astro-ph/9903005},
year = {2007}
}
Comments
13 pages, 10 tables, LaTeX (paspconf.sty + natbib.sty). Contribution to the proceedings of the Colloquium "Harmonizing Cosmic Distance Scales in a Post-Hipparcos Era", Haguenau, France, 14-16 Sep.98, ASP Conf. Series, eds. D. Egret & A. Heck