The 2dF Galaxy Redshift Survey: The bJ-band galaxy luminosity function and survey selection function

By P. Norberg, Shaun Cole, C. Baugh, Carlos S. Frenk, I. Baldry, Joss Bland-Hawthorn, T. Bridges, R. Cannon, M. Colless, C. Collins and 18 more. 2001

361 citations recorded by the source corpus.

We use more than 110 500 galaxies from the 2dF Galaxy Redshift Survey (2dFGRS) to estimate the bJ-band galaxy luminosity function at redshift z = 0, taking account of evolution, the distri- bution of magnitude measurement errors and small corrections for incompleteness in the galaxy catalogue. Throughout the interval −16.5 > MbJ − 5 log10 h > −22, the luminosity function is accurately described by a Schechter function with MJ − 5 log10 h =− 19.66 ± 0.07, α = −1.21 ± 0.03 and � � = (1.61 ± 0.08) × 10 −2 h 3 Mpc −3 , giving an integrated luminosity den- sity of ρL = (1.82 ± 0.17) × 10 8 h LMpc −3 (assuming an � 0 = 0.3, 0 = 0.7 cosmology). The quoted errors have contributions from the accuracy of the photometric zero-point, from large-scale structure in the galaxy distribution and, importantly, from the uncertainty in the ap- propriate evolutionary corrections. Our luminosity function is in excellent agreement with, but has much smaller statistical errors than, an estimate from the Sloan Digital Sky Survey (SDSS) data when the SDSS data are accurately translated to the bJ band and the luminosity functions are normalized in the same way. We use the luminosity function, along with maps describing the redshift completeness of the current 2dFGRS catalogue, and its weak dependence on ap- parent magnitude, to define a complete description of the 2dFGRS selection function. Details and tests of the calibration of the 2dFGRS photometric parent catalogue are also presented.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

The VIMOS-VLT deep survey - Evolution of the galaxy luminosity function up to z = 2 in first epoch data (2004, neutral): “In this band the VVDS slope is instead consistent with that derived by Norberg et al. (2002) from the 2dFGRS.”
The Millennium Galaxy Catalogue: 16 ⩽ BMGC < 24 galaxy counts and the calibration of the local galaxy luminosity function (2002, methodology): “In Table 3 we list the LF parameters from the 2dFGRS (Norberg et al. 2002), SDSS-CD (Blanton et al. 2001), ESP (Zucca et al. 1997), CS (Brown et al. 2001), Durham/UKST (Ratcliffe et al. 1998), Mt Stromlo/APM (Loveday et al. 1992), SSRS2 (Marzke et al. 1998) and NOG (Marinoni et al. 1999) surveys.”
The VIMOS VLT Deep Survey. Evolution of the luminosity functions by galaxy type up to z = 1.5 from first epoch data (2005, neutral): “At present the local luminosity function is well determined by the results obtained by the 2dF Galaxy Redshift Survey (2dFGRS, Norberg et al. 2002) and by the Sloan Digital Sky Survey (SDSS, Blanton et al. 2003).”
Reconciling the local galaxy population with damped Lyman α cross-sections and metal abundances (2005, methodology): “For the value ofL∗ we adopted the recent measurement ofM∗B − 5 log h75 = −20.3 from Norberg et al. (2002),M∗R − 5 log h75 = −21.1 from Lin et al. (1996), and M∗K − 5 log h75 = −24.1 from Cole et al. (2001).”
The high‐redshift galaxy population in hierarchical galaxy formation models (2006, methodology): “As az = 0 standard we use the local LF from the 2dF survey Norberg et al. (2002).”
Galaxy and Mass Assembly (GAMA): the GAMA galaxy group catalogue (G3Cv1) (2011, methodology): “The galaxy LF can be directly estimated from the data (e.g. Loveday et al. 1995; Norberg et al. 2002; Blanton et al. 2003), while the linking parameters cannot be estimated from the data.”
The many lives of active galactic nuclei: cooling flows, black holes and the luminosities and colour (2005, methodology): “We demonstrate this by overplotting K-band data from Cole et al. (2001) and Huang et al. (2003) in the left-hand panel, and bJ-band data from Norberg et al. (2002) in the right-hand panel.”
Galaxy and Mass Assembly (GAMA): ugriz galaxy luminosity functions (2011, result): “Allowing for LF evolution enabled reconciliation of previously discrepant luminosity densities obtained from SDSS commissioning data (Blanton et al. 2001) and the Two-degree field Galaxy Redshift Survey (Folkes et al. 1999; Norberg et al. 2002).”
The nature and space density of fossil groups of galaxies (2003, background): “The space density of all galaxies more luminous than our faintest central galaxy (MR < −22.8 + 5 logh50, or LR > 1.5L∗) is 2 × 10−4 h350 Mpc−3, based on the 2dF galaxy redshift survey luminosity function of Norberg et al. (2002) and assuming B − R = 1.5 mag.”
RELATIVISTIC JET FEEDBACK IN EVOLVING GALAXIES (2010, background): “…dispersion (Magorrian et al. 1998; Gebhardt et al. 2000; Tremaine et al. 2002), the deficit of bright galaxies in the galaxy luminosity function (Cole et al. 2001; Norberg et al. 2002; Huang et al. 2003), and the completion of star formation in massive galaxies at epochs of redshift z .”
The Halo Occupation Distribution and the Physics of Galaxy Formation (2002, methodology): “The clustering of galaxies is well known to depend on galaxy color or spectral type and on galaxy morphology (see Norberg et al. 2002a; Zehavi et al. 2002, and numerous references therein).”
Galaxy groups in the 2dFGRS: the group-finding algorithm and the 2PIGG catalogue (2004, methodology): “…each angular position and redshift is computed from the 2dFGRS luminosity function as n(z, θ) = ∫ blim J (θ) b bright J Φ(M(bJ, z))cz(bJ, θ)dbJ. (2.7) The luminosity function used here is that estimated by Norberg et al. (2002), convolved with their model of the 2dFGRS magnitude measurement errors.”
The 6dF Galaxy Survey: final redshift release (DR3) and southern large-scale structures (2009, background): “For example, the evolutionary corrections that initially beset comparisons between 2dFGRS and SDSS (cf. Norberg et al. 2002; Blanton et al. 2001) are negligible for 6dFGS, which spans lookback times of only 0.2 to 0.7 Gyr across [0.5z̄, 1.5z̄] (compared to 0.5 to 1.3 Gyr for SDSS and 2dFGRS).”
THE NEXT GENERATION VIRGO CLUSTER SURVEY (NGVS). I. INTRODUCTION TO THE SURVEY (2012, background): “Determinations of the luminosity function have improved dramatically in accuracy as redshift surveys have grown in size (e.g., Efstathiou et al. 1988; Loveday et al. 1992; Marzke et al. 1994; Lin et al. 1996; Cole et al. 2001; Norberg et al. 2002; Blanton et al. 2003).”
Cosmological baryonic and matter densities from 600 000 SDSS luminous red galaxies with photometric redshifts (2006, background): “(i) Galaxies in more distant redshift slices are preferentially more luminous (owing to the fixed apparent magnitude threshold) and hence more strongly clustered (e.g. Norberg et al. 2002).”