EDP Sciences
Free access
Volume 410, Number 2, November I 2003
Page(s) L25 - L28
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:20031495

A&A 410, L25-L28 (2003)
DOI: 10.1051/0004-6361:20031495


The UV luminosity function of nearby clusters of galaxies

L. Cortese1, G. Gavazzi1, A. Boselli2, J. Iglesias-Paramo2, J. Donas2 and B. Milliard2

1  Universitá degli Studi di Milano-Bicocca, P.zza della Scienza 3, 20126 Milano, Italy
    e-mail: Luca.Cortese@mib.infn.it; Giuseppe.Gavazzi@mib.infn.it
2  Laboratoire d'Astrophysique de Marseille, BP 8, Traverse du Siphon, 13376 Marseille Cedex 12, France
    e-mail: alessandro.boselli@oamp.fr; jorge.iglesias@oamp.fr

(Received 18 July 2003 / Accepted 23 September 2003)

We present the UV composite luminosity function for galaxies in the Virgo, Coma and Abell 1367 clusters. The luminosity function (LF) is well fitted by a Schechter function with $M_{\rm UV}^* - 5~ \log\,h_{\rm 75}= -20.75 \pm 0.40$ and $\alpha = -1.50 \pm 0.10$ and does not differ significantly from the local UV luminosity function of the field. This result is in agreement with recent studies carried out in the $\rm H\alpha$ and B-bands which find no difference between the LFs of star forming galaxies in clusters and in the field. This indicates that, whatever mechanisms are responsible for quenching the star formation in clusters, they influence similarly the giant and the dwarf populations, leaving the shape of the LF unchanged and only modifying its normalization.

Key words: galaxies: luminosity function -- galaxies: clusters: individual: Abell1367, Coma, Virgo -- galaxies: evolution

Offprint request: L. Cortese, Luca.Cortese@mib.infn.it

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