Volume 490, Number 3, November II 2008
|Page(s)||923 - 928|
|Section||Cosmology (including clusters of galaxies)|
|Published online||17 September 2008|
I. A catalog of 473 members
Observatoire de Paris, LERMA, 77 av. Denfert-Rochereau, 75015 Paris, France e-mail: email@example.com
2 INAF – Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italy e-mail: firstname.lastname@example.org
Accepted: 18 August 2008
This paper presents morphological type, membership, and color for a sample of galaxies in the Coma cluster direction, complete down to MB=-15.00 mag and extending down to MB=-14.25 mag. We have examined 1155 objects from the GMP 1983 catalog on B and V images of the CFH12K camera, and obtained the Hubble type in most cases. Coma cluster membership for 473 galaxies was derived using morphology, apparent size, and surface brightness, and, afterward, redshift. The comparison among morphology- and redshift- memberships and among luminosity functions derived from this morphologically-selected sample, or by using statistical members or spectroscopic members, all show that the morphological membership provided here can be trusted. For the first time, the morphological classification of Coma galaxies reaches magnitudes that are faint enough to observe the whole magnitude range of the giant types, E, S0, and spiral stages. The data presented in this paper makes our sample the richest environment where membership and morphology for complete samples down to faint magnitudes ( mag) are available, thereby enlarging the baseline of environmental studies.
Key words: galaxies: luminosity function, mass function / galaxies: elliptical and lenticular, cD / galaxies: spirals / galaxies: dwarf – galaxies: clusters: individual: Coma
Based on observations obtained at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii.
© ESO, 2008
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