A&A 459, 679-692 (2006)
A deep wide survey of faint low surface brightness galaxies in the direction of the Coma cluster of galaxiesC. Adami1, R. Scheidegger2, M. Ulmer2, F. Durret3, 4, A. Mazure1, M. J. West5, C. J. Conselice6, M. Gregg7, S. Kasun2, R. Pelló8, and J. P. Picat8
1 LAM, Traverse du Siphon, 13012 Marseille, France
2 Department of Physics and Astronomy, Northwestern University, 2131 Sheridan Road, Evanston IL 60208-2900, USA
3 Institut d'Astrophysique de Paris, CNRS, Université Pierre et Marie Curie, 98bis Bd. Arago, 75014 Paris, France
4 Observatoire de Paris, LERMA, 61 Av. de l'Observatoire, 75014 Paris, France
5 Department of Physics and Astronomy, University of Hawaii, 200 West Kawili Street, LS2, Hilo HI 96720-4091, USA
6 Department of Astronomy, Caltech, MS 105-24, Pasadena CA 91125, USA
7 Department of Physics, University of California at Davis, 1 Shields Avenue, Davis, CA 95616, USA
8 Observatoire Midi-Pyrénées, 14 Av. Edouard Belin, 31400 Toulouse, France
(Accepted 4 July 2005 / Received 28 August 2006)
Aims.We report on a search for faint (R total magnitude fainter than 21) and low surface brightness galaxies (R central surface brightness fainter than ~24) (fLSBs) in a deg2 area centered on the Coma cluster.
Methods.We analyzed deep B and R band CCD imaging obtained using the CFH12K camera at CFHT and found 735 fLSBs. The total B magnitudes, at the Coma cluster redshift, range from -13 to -9 with B central surface brightness as faint as 27 mag arcsec-2.
Results.Using empty field comparisons, we show that most of these fLSBs are probably inside the Coma cluster. We present the results of comparing the projected fLSB distributions with the distributions of normal galaxies and with known X-ray over densities. We also investigate their projected distribution relative to their location in the color magnitude relation. Colors of fLSBs vary between and ~1.4 for 2/3 of the sample and this part is consistent with the known CMR red-sequence for bright () ellipticals in Coma.
Conclusions.These fLSBs are likely to have followed the same evolution as giant ellipticals, which is consistent with a simple feedback/collapse formation and a passive evolution. These fLSBs are mainly clustered around NGC 4889. We found two other distinct fLSB populations. These populations have respectively redder and bluer colors compared to the giant elliptical red-sequence and possibly formed from stripped faint ellipticals and material stripped from spiral in-falling galaxies.
Key words: galaxies: clusters: individual: Coma
© ESO 2006