The 2dF Galaxy Redshift Survey: Luminosity functions by density environment and galaxy type

By Darren Croton, G. Farrar, P. Norberg, M. Colless, J. Peacock, I. Baldry, C. Baugh, Joss Bland-Hawthorn, T. Bridges, R. Cannon and 19 more. 2004

219 citations recorded by the source corpus.

We use the 2dF Galaxy Redshift Survey to measure the dependence of the bJ-band galaxy luminosity function on large-scale environment, defined by density contrast in spheres of radius 8h-1 Mpc, and on spectral type, determined from principal component analysis. We find that the galaxy populations at both extremes of density differ significantly from that at the mean density. The population in voids is dominated by late types and shows, relative to the mean, a deficit of galaxies that becomes increasingly pronounced at magnitudes brighter than MbJ, - 5 log10 h ≲ -18.5. In contrast, cluster regions have a relative excess of very bright early-type galaxies with MbJ, - 5 log10 h ≲ -21. Differences in the mid- to faint-end population between environments are significant: at MbJ, -5 log10 h = -18 early- and late-type cluster galaxies show comparable abundances, whereas in voids the late types dominate by almost an order of magnitude. We find that the luminosity functions measured in all density environments, from voids to clusters, can be approximated by Schechter functions with parameters that vary smoothly with local density, but in a fashion that differs strikingly for early- and late-type galaxies. These observed variations, combined with our finding that the faint-end slope of the overall luminosity function depends at most weakly on density environment, may prove to be a significant challenge for models of galaxy formation.

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Citations in the corpus

Galaxy Zoo: the dependence of morphology and colour on environment (2008, background): “The mass function of galaxies is also expected to depend on morphological type (Maller 2008), as it varies with other galaxy properties (Croton et al. 2005; Baldry et al. 2006).”
Environmental Dependence of Properties of Galaxies in the Sloan Digital Sky Survey (2006, methodology): “Croton et al. (2005) measured the Schechter function parameters for early and late-type galaxies in the 2dFGRS. Contrary to Croton et al., we find that M? for early types is changing slowly below the mean density and that luminosity for late types rises at high density ( /̄ > 5).”
Formation of Early-Type Galaxies from Cosmological Initial Conditions (2005, background): “For more massive systems than the ones studied here it has been argued that feedback from AGNs might have a bigger impact and be responsible for the sharp cutoff at the bright end of the luminosity function of ellipticals (Croton et al. 2005).”
SPECTROSCOPIC CONFIRMATION OF TWO MASSIVE RED-SEQUENCE-SELECTED GALAXY CLUSTERS AT z ∼ 1.2 IN THE SpARCS-NORTH CLUSTER SURVEY (2008, background): “…(e.g., Dressler 1980; Goto et al. 2003; Park et al. 2007), stellar mass (e.g., Kauffmann et al. 2004), color (e.g., Hogg et al. 2003; Balogh et al. 2004; Blanton et al. 2005), and luminosity (e.g., Croton et al. 2005; Park et al. 2007) are all strongly correlated with local galaxy density.”
Galaxy and Mass Assembly (GAMA): the GAMA galaxy group catalogue (G3Cv1) (2011, background): “This process assumes that a global LF is appropriate for all groups over a range of masses and environments, which is known not to be the case (e.g. Eke et al. 2004; Croton et al. 2005; Robotham et al. 2006).”
A Dark Core in Abell 520 (2007, background): “The brightest galaxy within 150 kpc of peak 3 has MB = −20.3, hardly brighter than L∗ at z = 0.2 (Croton et al. 2005; Dahlen et al. 2005).”
Internal and Collective Properties of Galaxies in the Sloan Digital Sky Survey (2006, background): “The existence of the large scale structure affects both normalization and shape of LF (e.g. Croton et al. 2005).”
The DEEP2 Galaxy Redshift Survey: the relationship between galaxy properties and environment at z∼ 1 (2006, methodology): “For example, using large data sets from local surveys such as the SDSS, Blanton et al. (2004), Kauffmann et al. (2004) and Croton et al. (2005) measured the relationship between star formation history and local galaxy density for environments ranging from voids to clusters.”
The Link between Submillimetre Galaxies and Luminous Ellipticals: Near-Infrared IFU Spectroscopy of Submillimetre Galaxies (2006, methodology): “Integrating down the z = 0 luminosity function of early-type galaxies from Croton et al. (2005) (see also Wake et al. 2006), to a median magnitude of MK ∼ −25.1 we determine a space density of 9 × 10−5 Mpc−3 (we note that using the LRG luminosity function from Wake et al. 2006 we obtain 1.1.”
Galaxy bimodality versus stellar mass and environment (2006, methodology): “Croton et al. (2005) found an increase of ∼ 1mag between void and clusterlike environments using bJ luminosities.”
THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS (2007, background): “…and color, depend on local density (Gómez et al. 2003; Balogh et al. 2004a,b; Hogg et al. 2004; Kauffmann et al. 2004; Tovmassian et al. 2004; Blanton et al. 2005a; Christlein & Zabludoff 2005; Croton et al. 2005; Rojas et al. 2005; Cooper et al. 2006; Mandelbaum et al. 2006; Cooper et al. 2007).”
The DEEP2 galaxy redshift survey: evolution of the colour–density relation at 0.4 < z < 1.35 (2006, background): “…that the connections between local environment and galaxy properties such as morphology, color, and luminosity extend over the full range of densities, from rich clusters to voids (e.g., Kauffmann et al. 2004; Balogh et al. 2004a; Blanton et al. 2005; Croton et al. 2005; Rojas et al. 2005).”
Galaxy halo masses and satellite fractions from galaxy–galaxy lensing in the Sloan Digital Sky Survey: stellar mass, luminosity, morphology and environment dependencies (2005, background): “…between color and environment, with red galaxies typically found in overdense regions (Davis & Geller 1976; Dressler 1980; Postman & Geller 1984; Balogh et al. 1998, 1999; Carlberg et al. 2001; Blanton et al. 2003a; Hogg et al. 2003; Balogh et al. 2004a,b; Hogg et al. 2004; Croton et al. 2005).”
The Dependence of Halo Clustering on Halo Formation History, Concentration, and Occupation (2005, background): “…assumption is avoided to some extent in many modern implementations that use halo merging histories extracted directly from N-body simulations (e.g., Springel et al. 2001, 2005; Helly et al. 2003; Hatton et al. 2003; Kang et al. 2005; Croton et al. 2005; De Lucia et al. 2006; Bower et al. 2006).”
THE STELLAR MASS CONTENT OF SUBMILLIMETER-SELECTED GALAXIES (2010, methodology): “When we integrate theK-band luminosity function of earlytype galaxies atz = 0 of Croton et al. (2005), we find that we can match the space density of SMG descendants of φD ∼ 0.5×10−3Mpc−3 by integrating the early-type luminosity function down to 1.3L∗.”