Deprojection of luminosity functions of galaxies in the Coma cluster

Abstract

We use a simple analytic model to deproject 2-d luminosity functions (LF) of galaxies in the Coma cluster measured by Beijersbergen et al. 2002. We demonstrate that the shapes of the LFs change after deprojection. It is therefore essential to correct LFs for projection effects. The deprojected LFs of the central area have best-fitting Schechter parameters of M^{*}_U=-18.31^{+0.08}_{-0.08} and α_U=-1.27^{+0.018}_{-0.018}, M^{*}_B=-19.79^{+0.14}_{-0.15} and α_B=-1.44^{+0.016}_{-0.016} and M^{*}_r=-21.77^{+0.20}_{-0.28} and α_r=-1.27^{+0.012}_{-0.012}. The corrections are not significant enough to change the previously observed trend of increasing faint end slopes with increasing distance to the cluster center. The weighted U, B, and r band slopes of the deprojected LFs show a slightly weaker steepening with increasing projected cluster radius.

Accepted for publication in A&A as a Research Note

References in corpus (3)

• The NGC4839 group falling into the Coma cluster observed by XMM-Newton
• U, B and r band luminosity functions of galaxies in the Coma cluster
• Do clusters contain a large population of dwarf galaxies?

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• The Possible z=0.83 Precursors of z=0 M* Early-type Cluster Galaxies
• Luminosity segregation in three clusters of galaxies (A119, 2443, 2218)
• A phylogenetic analysis of galaxies in the Coma Cluster and the field: a new approach to galaxy evolution