Evidence for Steep Luminosity Functions in Clusters of Galaxies

Propris, Roberto De; Pritchet, C. J.; Harris, W. E.; McClure, R. D.

doi:10.1086/176163

Cited by 80 publications

(81 citation statements)

References 28 publications

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“…The preponderance of giant ellipticals in clusters ( Dressler 1980) is clearly related to the strong dependence on luminosity for red, luminous galaxies. The denseness of the environments of the lower luminosity red galaxies may be a signature of the luminous end of the dwarf elliptical population, which also resides in clusters (Ferguson & Sandage 1989;de Propris et al 1995;Mobasher et al 2003). The strong dependence of environment on color for bluer galaxies is clearly related to the lack of star forming galaxies in clusters.…”

Section: Summary and Discussionmentioning

confidence: 99%

Relationship between Environment and the Broadband Optical Properties of Galaxies in the Sloan Digital Sky Survey

Blanton

Eisenstein²,

Hogg

et al. 2005

ApJ

608

661

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We examine the relationship between environment and the luminosities, surface brightnesses, colors, and profile shapes of luminous galaxies in the Sloan Digital Sky Survey (SDSS). For the SDSS sample, galaxy color is the galaxy property most predictive of the local environment. Galaxy color and luminosity-measures of the star formation history-jointly comprise the most predictive pair of properties. At fixed luminosity and color, density is not closely related to surface brightness or to Sérsic index-measures of galaxy structure. In the text, we discuss what measurable residual relationships exist, generally finding that at red colors and fixed luminosity, the mean density decreases at the highest surface brightnesses and Sérsic indices. In general, these results suggest that the structural properties of galaxies are less closely related to galaxy environment than are their masses and star formation histories.

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Section: Summary and Discussionmentioning

confidence: 99%

Relationship between Environment and the Broadband Optical Properties of Galaxies in the Sloan Digital Sky Survey

Blanton

Eisenstein²,

Hogg

et al. 2005

ApJ

608

661

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“…Measuring the faint-end luminosity function (LF) of galaxies in clusters has been the subject of many detailed research papers in the last few years (e.g., Sandage, Binggeli, & Tammann 1985 ;Driver et al 1994 ;De Propris et al 1995 ;Gaidos 1997 ;Lobo et al 1997 ;Lumsden et al 1997 ;Lopez-Cruz et al 1997 ;Valotto et el. 1997 ;Wilson et al 1997 ;Smith et al 1997 ;Trentham 1997Trentham , 1998Driver et al 1998 ;Garilli et al 1999).…”

Section: Introductionmentioning

confidence: 99%

Do Clusters Contain a Large Population of Dwarf Galaxies?

Valotto

Moore

Lambas

2001

ApJ

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We analyze systematic e †ects in the determination of the galaxy luminosity function in clusters using a deep mock catalog constructed from a numerical simulation of a hierarchical universe. The results indicate a strong tendency to derive a rising faint end in clusters selected in two dimensions, (a [ [1.5) using a galaxy catalog constructed with a universal Ñat luminosity function with a^[1.0. This is a result of the projection e †ects inherent in catalogs of clusters constructed using two-dimensional data. Many of the clusters found in two dimensions have no signiÐcant three-dimensional counterparts, and most su †er from massive background contamination that cannot be corrected for by subtracting random o †set Ðelds. The luminosity function of high surface brightness galaxies in the Ðeld and within small groups follows a Schechter function with a fairly Ñat faint-end slope, n(L ) P La, with a \ [0.9 to [1.2. On the contrary, observational studies of clusters constructed using Abell, EDCC, and APM catalogs are systematically found to have steeper luminosity functions with a \ [1.4 to [2.0. This may be attributed to projection e †ects rather than a dominant population of high surface brightness dwarf galaxies in clusters. It should be straightforward to conÐrm our results by measuring redshifts of (M Z M* ] 2) these faint cluster galaxies.

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“…Marzke et al (1994b) report an upturn in the luminosity function of late-type galaxies with M(B) > −16 + log 10 h, but LCRS, Autofib, and Cowie et al (1996) all derive a flat faint-end slope. There is, however, evidence for a steep faint-end slope in galaxy clusters (e.g., De Propris et al 1995, Bernstein et al 1995. Environmental influences on galaxy evolution may be reflected in variations of the LF for galaxies in different environments, and it is therefore important to measure the LF in a variety of environments.…”

Section: Introductionmentioning

confidence: 99%

The Norris Survey of the Corona Borealis Supercluster. III. Structure and Mass of the Supercluster

Small

Sargent

et al. 1998

ApJ

106

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We measure the field galaxy luminosity function (LF) as a function of color and redshift from z = 0 to z = 0.5 using galaxies from the Norris Survey of the Corona Borealis Supercluster. The data set consists of 603 field galaxies with 0 < z ≤ 0.5 and spans a wide range in apparent magnitude (14.0 m ∼ < r ∼ < 21.5 m ), although our field galaxy LF analysis is limited to 493 galaxies with r ≤ 20.0 m . We use the observed g − r colors of the galaxies to compute accurate corrections to the rest B AB and r bands. We find that our local r-band LF, when normalized to counts in high galactic latitude fields, agrees well with the local LF measured in the Las Campanas Redshift Survey. Our B AB -band local LF, however, does not match the b j -band LF from the Stromlo/APM survey, having a normalization 1.6 times higher. We see compelling evidence that the B AB -band field galaxy LF evolves with redshift. The evolution is strongest for the population of star-forming galaxies with [O II] λ3727 rest-frame equivalent widths greater than 10Å. The population of red, quiescent galaxies shows no sign of evolution to z = 0.5. The evolution of the LF which we observe is consistent with the findings of other faint galaxy redshift surveys. The fraction of galaxies with [O II] emission increases rapidly with redshift, but the fraction of galaxies with strong Hδ absorption, a signature of a burst of star-formation, does not. We thus conclude that the star formation in distant galaxies is primarily long-lived.We also compute the LFs of the Corona Borealis supercluster (z ≈ 0.07, 419 galaxies with 14.1 m ≤ r ≤ 20.0 m ) and the Abell 2069 supercluster (z ≈ 0.11, 1 present address: Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK -2 -318 galaxies with 15.1 m ≤ r ≤ 20.0 m ). The shapes of the two supercluster luminosity functions are broadly similar to the shape of the local luminosity function. However, there are important differences. Both supercluster LFs have an excess of very bright galaxies. In addition, the characteristic magnitude of the Corona Borealis supercluster LF is roughly half a magnitude brighter than that of the local field galaxy LF, and there is a suggestion of an upturn in the LF for galaxies fainter than M(B AB ) ∼ −17 m .

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Evidence for Steep Luminosity Functions in Clusters of Galaxies

Cited by 80 publications

References 28 publications

Relationship between Environment and the Broadband Optical Properties of Galaxies in the Sloan Digital Sky Survey

Relationship between Environment and the Broadband Optical Properties of Galaxies in the Sloan Digital Sky Survey

Do Clusters Contain a Large Population of Dwarf Galaxies?

The Norris Survey of the Corona Borealis Supercluster. III. Structure and Mass of the Supercluster

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