Abstract
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 and find 105 dwarf LSB galaxies previously uncatalogued over an area of ∼ 14 sq deg. We show that there are many more faint (−14 ≤ M B ≤ −10) LSB galaxies than 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 α = −1.6. 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.
By a comparison with different environments, the Virgo Cluster seems to be highly ‘dwarf rich’ if considering the dwarf to giant ratio or its luminosity function faint end slope.
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Sabatini, S., Roberts, S., Davies, J. (2003). Dwarf LSB Galaxies and their Environment: The Virgo Cluster, The URSA Major Cluster, Isolated Galaxies and Voids. In: Lobo, C., Serote Roos, M., Biviano, A. (eds) Galaxy Evolution in Groups and Clusters. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-0107-6_13
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DOI: https://doi.org/10.1007/978-94-010-0107-6_13
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