The dwarf Low Surface Brightness galaxy population of the Virgo Cluster I. The faint-end-slope of the Luminosity Function

Details The dwarf Low Surface Brightness galaxy population of the Virgo Cluster I. The faint-end-slope of the Luminosity Function The dwarf Low Surface Brightness galaxy population of the Virgo Cluster I. The faint-end-slope of the Luminosity Function

2003-01-29

arxiv.org/abs/astro-ph/0301585v2

Mon.Not.Roy.Astron.Soc. 341 (2003) 981

Astronomy and Astrophysics

Astrophysics

12 pages, 14 figures (fig 4,6 are poor quality for size reasons). Accepted for publication in MNRAS

Scientific paper

10.1046/j.1365-8711.2003.06484.x

The widely varying dwarf galaxy counts in different environments provide a strong challenge to standard hierarchical clustering models. The luminosity function is not universal, but seems to be strongly dependent upon environment. In this paper we describe an automated procedure for detecting and measuring very low surface brightness (LSB) features in deep CCD data. We apply this procedure to large area CCD survey fields of the Virgo cluster. We show that there are many more faint ($-10 \geq M_{B} \geq -14$) low surface brightness galaxies than what would be predicted from extrapolation of the Virgo cluster catalogue luminosity function. Over our limited range of measurement the faint end slope of the luminosity function becomes $\alpha=- 1.6$. The luminosity function is flatter in the inner regions of the cluster than it is in the outer regions. Although these galaxies contribute a small fraction of the total stellar light of the cluster, they may contribute significantly to the mass in galaxies if they have large mass-to-light ratios similar to those recently measured for Local Group dwarf galaxies.

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