The Galaxy Luminosity Function from Observations of Twenty Abell Clusters

Details The Galaxy Luminosity Function from Observations of Twenty Abell Clusters The Galaxy Luminosity Function from Observations of Twenty Abell Clusters

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aj....113..117g&link_type=abstract

Astronomical Journal v.113, p. 117-129 (1997)

Astronomy and Astrophysics

Astronomy

30

Scientific paper

A luminosity function is constructed from photometric imaging of galaxies in 20 Abell clusters. The LF is well-described on the whole by a Schechter function with M(*_R) = -21.13 +/- 0.11 + 5 log h and alpha = -1.09 +/- 0.08. The value of M(*) is 0.93 +/- 0.20 magnitude brighter than the value obtained from the recent Las Campanas Redshift Survey (excluding systematic errors). The flat faint-end slope is consistent with field surveys and the lack of an upturn at absolute magnitudes brighter than M(*_R) < -16.5 is similar to behavior in the field and is inconsistent with previous claims of a steep faint-end slope in clusters.

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