Dissecting the Luminosity Function of the Coma Cluster of Galaxies Using Canada‐France‐Hawaii Telescope1 Wide‐Field Images

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Abstract
[Abridged] We determined the luminosity function (LF) of the Coma cluster galaxies selected by luminosity, and the LF bi-variate in central brightness. The Coma cluster and control fields were imaged using the CFH12K (42x28 arcmin) and UH8K (28x28 arcmin) wide-field cameras at the CFHT. Selected HST images were used for testing. Quantities were derived from measurements in at least two colors, which have the following features: (1) Galaxies as faint as three times the luminosity of the brightest globular clusters are in the completeness region of our data. (2) We have a complete census (in the explored region) of low surface brightness galaxies with central surface brightness galaxies almost as low as the faintest so far cataloged ones. (3) The explored area is among the largest ever sampled with CCDs at comparable depth for any cluster of galaxies. (4) The error budget includes all sources of errors known to date. Using HST images we also discovered that blends of globular clusters, not resolved in individual components due to seeing, look like dwarf galaxies when observed from the ground and are numerous and bright. The derived Coma LF is relatively steep (alpha=-1.4) over the 11 magnitudes sampled, but the slope and shape depend on color. A large population of faint low surface brightness galaxies was discovered, representing the largest contributor (in number) to the LF at faint magnitudes. We found a clear progression for a faintening of the LF from high surface brightness galaxies (mu~20 mag/arcsec2) to galaxies of very faint central brightnesses (mu~24.5 mag/arcsec2), and some evidence for a steepening. Compact galaxies, usually classified as stars and therefore not included in the LF, are found to be a minor population in Coma.Comment: ApJ, in pres
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