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

Abstract

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 distribution of magnitude measurement errors and small corrections for incompleteness in the galaxy catalogue. Throughout the interval −16.5 > M italicb J− 5 log10h > −22, the luminosity function is accurately described by a Schechter function with M★ italicb J− 5 log10h=−19.66 ± 0.07, α=−1.21 ± 0.03 and Φ★= (1.61 ± 0.08) × 10−2h3 Mpc−3, giving an integrated luminosity density of ρL= (1.82 ± 0.17) × 108h L⊙ Mpc−3 (assuming an Ω0= 0.3, Λ0= 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 appropriate 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 apparent 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.

Reionization in sterile neutrino cosmologies

“…For the L 6 = 700 case, we also show an extreme model in which the feedback has been completely turned off ('NoFb'). The black points are observational estimates (Norberg et al 2002;Driver et al 2012). …”

The abundance and colours of galaxies in high-redshift clusters in the cold dark matter cosmology

“…The panels show the luminosity functions in the b J , z, H and K bands, as labelled. Data points show the observational estimates from the Two-Micron All-Sky Survey (Kochanek et al 2001), Two-degree Field Galaxy Redshift Survey (2dFGRS; Cole et al 2001;Norberg et al 2002), the Six-degree Field Galaxy Survey (6dFGS; Jones et al 2006) and the Galaxy And Mass Assembly Survey (GAMA; Driver et al 2012). The solid blue line shows the prediction for the fiducial GALFORM model with the default dust attenuation calculations.…”

Superclusters of galaxies from the 2dF redshift survey

“…We take M = 5.33 in the b j band. In calculation of luminosities we used the k + e-corrections according to Norberg et al (2002). The weights used to calculate estimated total luminosities of superclusters are shown in the Fig.…”

“…What is important here is not only the absence of faint members of groups at large distance, but also the absence of faint groups. In this paper we are interested in the total luminosities of large systems (superclusters), thus in calculation of estimated total luminosities we use the set of Schechter parameters α 1 = −1.21, M * 1 − 5 log 10 h = −19.66, as found by Norberg et al (2002) for the whole 2dF galaxy sample. Our calculations show that this set of Schechter parameters yields total mean luminosity density which is approximately independent of the distance from the observer, as expected for a fair sample of the Universe (see Fig.…”