The 2dF Galaxy Redshift Survey: luminosity dependence of galaxy clustering

By P. Norberg, C. Baugh, E. Hawkins, S. Maddox, J. Peacock, Shaun Cole, Carlos S. Frenk, Joss Bland-Hawthorn, T. Bridges, R. Cannon and 17 more. 2001

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We investigate the dependence of the strength of galaxy clustering on intrinsic luminos- ity using the Anglo-Australian two degree field galaxy redshift survey (2dFGRS). The 2dFGRS is over an order of magnitude larger than previous redshift surveys used to address this issue. We measure the projected two-point correlation function of galax- ies in a series of volume-limited samples. The projected correlation function is free from any distortion of the clustering pattern induced by peculiar motions and is well described by a power-law in pair separation over the range 0.1 < (r/h 1 Mpc) < 10. The clustering of L � (MbJ 5log10 h = 19.7) galaxies in real space is well fit by a correlation length r0 = 4.9 ± 0.3h 1 Mpc and power-law slope = 1.71 ± 0.06. The clustering amplitude increases slowly with absolute magnitude for galaxies fainter than M � , but rises more strongly at higher luminosities. At low luminosities, our results agree with measurements from the SSRS2 by Benoist et al. However, we find a weaker dependence of clustering strength on luminosity at the highest luminosities. The cor- relation function amplitude increases by a factor of 4.0 between MbJ 5log10 h = 18 and 22.5, and the most luminous galaxies are 3.0 times more strongly clustered than Lgalaxies. The power-law slope of the correlation function shows remarkably little variation for samples spanning a factor of 20 in luminosity. Our measurements are in very good agreement with the predictions of the hierarchical galaxy formation models of Benson et al.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

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Citations in the corpus

The Halo Occupation Distribution: Toward an Empirical Determination of the Relation between Galaxies and Mass (2001, background): “We thank Carlton Baugh, Andrew Benson, James Bullock, Chris Burke, Shaun Cole, Carlos Frenk, Andrey Kravtsov, and Roman Scoccimarro for helpful discussions, input, and comments, and Carlton Baugh for making the APM correlation function available to us in electronic format.”
The 2dF Galaxy Redshift Survey: correlation functions, peculiar velocities and the matter density of the Universe (2002, methodology): “The relation for 2dFGRS galaxies found by Norberg et al. (2001) was( r0 r∗0 )γr /2 = 0.85 + 0.15 ( L L∗ ) , (10) which gives, for L = 1.4L∗ (see Section 2.1), r∗0 = 4.71 ± 0.24, which will allow direct comparisons with other surveys.”
Galaxy Clustering in Early Sloan Digital Sky Survey Redshift Data (2002, background): “The 2dFGRS analysis (Norberg et al. 2001) also recovers nearly identical power-law slopes in the different luminosity ranges.”
Evolution and Color Dependence of the Galaxy Angular Correlation Function: 350,000 Galaxies in 5 Square Degrees (2004, background): “As the clustering properties of galaxies are expected to depend on luminosity and have been shown to do so locally (Norberg et al. 2001), this can hinder interpretation of the evolution of clustering measured in ω(θ) studies.”
Voids in the Two-Degree Field Galaxy Redshift Survey (2003, methodology): “We adopt the global k-correction + evolution correction found for b J selected galaxies in the ESO Slice Project (Zucca et al. 1997) and adopted by the 2dFGRS team (Norberg et al. 2001) and use k + e = 0.03z (0.01 + z 4 ) .”
The 2dF Galaxy Redshift Survey: power-spectrum analysis of the final data set and cosmological implications (2005, methodology): “They were also used in the analysis of the dependence of the correlation function on galaxy type and luminosity (Norberg et al. 2001, 2002a) and when analysing higher order counts in cells statistics (Baugh et al. 2004; Croton et al. 2004).”
The dependence of clustering on galaxy properties (2005, background): “Our results are also in quite good agreement with those of Tegmark et al. The dashed curve in Fig.6 shows the result of Norberg et al. (2001), based on wp(rp) measurements of somewhat more luminous galaxies in the 2dF survey (log 10 L/L∗ >∼ − 0.6).”
A primer on hierarchical galaxy formation: the semi-analytical approach (2006, background): “Surveys such as the 2dFGRS and SDSS allow the measurement of the galaxy luminosity function with, for the most part, random errors (arising from the volume covered and the number of galaxies) that are smaller than systematic effects, such as the choice of band-shifting and evolutionary corrections (”
The Shape of the Sloan Digital Sky Survey Data Release 5 Galaxy Power Spectrum (2007, methodology): “The smooth shape matches the overall shape of the simple formula of Norberg et al. (2001), b/b ¼ 0:85þ 0:15L/L (solid line), withM ¼ 20:44 (Blanton et al. 2003b).”
Galaxy groups in the 2dFGRS: the group-finding algorithm and the 2PIGG catalogue (2004, background): “…bearing on group-finding in the 2dFGRS: the local luminosity function in the bJ-band (see figure 10 of Madgwick et al. 2002; Cole et al. 2000), the clustering of luminous galaxies (Benson et al. 2000) and the dependence of galaxy clustering on luminosity (Benson et al. 2001; Norberg et al. 2001).”
Galaxy and Mass Assembly (GAMA): survey diagnostics and core data release (2010, background): “…Eke et al. 2004), merger rates (e.g. Bell et al. 2006), quantification of largescale structure (e.g. Percival et al. 2001), galaxy clustering (e.g. Norberg et al. 2001) and, in conjunction with cosmic microwave background and Type Ia supernova searches, convergence towards the basic cosmological…”
The 2dF Galaxy Redshift Survey: The Amplitudes of fluctuations in the 2dFGRS and the CMB, and implications for galaxy biasing (2001, methodology): “Possible variation of galaxy clustering with redshift is still within measurement errors of Norberg et al. (2001a,2002).”
The 2dF Galaxy Redshift Survey: The bJ-band galaxy luminosity function and survey selection function (2001, methodology): “Such variations are perhaps to be expected given the results of Norberg et al. (2001, 2002), which show that galaxies of different luminosity have systematically different clustering properties.”
Galaxy clustering and galaxy-galaxy lensing: a promising union to constrain cosmological parameters (2008, background): “…the advent of large galaxy redshift surveys, it has become possible to obtain accurate measurements of the clustering of galaxies as a function of their properties, such as luminosity, morphology and colour (e.g. Guzzo et al. 2000; Norberg et al. 2001, 2002; Zehavi et al. 2005; Wang et al. 2007).”
The Luminosity and Color Dependence of the Galaxy Correlation Function (2004, methodology): “At luminosities LP 0:2L , the Tegmark et al. (2004a) formula provides a better fit to our data than the extrapolation of the Norberg et al. (2001) formula.”
Cosmic evolution of the atomic and molecular gas contents of galaxies (2011, background): “than optically selected samples (e.g. Norberg et al. 2001),indicating that local HI selected galaxies are preferentially found in lower mass haloes than their optical counterparts.”
The New Galaxy: Signatures of Its Formation (2002, background): “In this sense, the hierarchy relates the large-scale density to the morphology and evolution of its individual galaxies; this is the so-called ‘morphologydensity relation’ (Dressler 1980; Hermit et al. 1996; Norberg et al. 2001).”