The 2dF galaxy redshift survey: near-infrared galaxy luminosity functions

Abstract

We combine the Two Micron All Sky Survey (2MASS) Extended Source Catalogue and the 2dF Galaxy Redshift Survey to produce an infrared selected galaxy catalogue with 17 173 measured redshifts. We use this extensive data set to estimate the galaxy luminosity functions in the J‐ and KS‐bands. The luminosity functions are fairly well fitted by Schechter functions with parameters MJ*−5 log h=−22.36±0.02, αJ=−0.93±0.04, ΦJ*=0.0104±0.0016 h3 Mpc−3 in the J‐band and MKS*−5 log h=−23.44±0.03, αKS=−0.96±0.05, ΦKS*=0.0108±0.0016 h3 Mpc−3 in the KS‐band (2MASS Kron magnitudes). These parameters are derived assuming a cosmological model with Ω0=0.3 and Λ0=0.7. With data sets of this size, systematic rather than random errors are the dominant source of uncertainty in the determination of the luminosity function. We carry out a careful investigation of possible systematic effects in our data. The surface brightness distribution of the sample shows no evidence that significant numbers of low surface brightness or compact galaxies are missed by the survey. We estimate the present‐day distributions of bJ−KS and J−KS colours as a function of the absolute magnitude and use models of the galaxy stellar populations, constrained by the observed optical and infrared colours, to infer the galaxy stellar mass function. Integrated over all galaxy masses, this yields a total mass fraction in stars (in units of the critical mass density) of Ωstarsh =(1.6±0.24)×10−3 for a Kennicutt initial mass function (IMF) and Ωstarsh =(2.9±0.43)×10−3 for a Salpeter IMF. These values are consistent with those inferred from observational estimates of the total star formation history of the Universe provided that dust extinction corrections are modest.

zCOSMOS – 10k-bright spectroscopic sample

“…Figure 6 shows the number densities (ρ N ), derived by the 1/V max method, for two different mass limits of log(M/M ) > 9.77, 10.77 (corresponding to log(M/M ) > 10, 11 for a Salpeter (1955) IMF, as often used in the literature). We compare our results with literature data from other high-z deep surveys (VVDS, DEEP2, GOODS-MUSIC, FORS Deep Field, COMBO17; see Pozzetti et al 2007, for details and references), and for the local Universe (Cole et al 2001;Bell et al 2003;Baldry et al 2008). The local values for zCOSMOS were derived assuming an evolution from the lowest redshift bin to z = 0 (see next section for details).…”

Massive $z\sim1.3$ evolved galaxies revealed

“…Thus, the two EROs presented here are among the most luminous and, possibly, the most massive evolved galaxies detected so far at z > 1. If we assume the local mean stellar mass-to-light ratio obtained by Cole et al (2001) with the Kennicut IMF (0.73 M /L ) we derive a stellar mass for the two EROs M stars 7 × 10 11 M which would exceed 10 12 M if we assume the M stars /L they derived with the Salpeter IMF (1.32 M /L ). However, these mean mass-to-light ratios are relevant to local galaxies.…”

The XXL Survey

“…To better compare our results with other works we convert L K to stellar mass using a fixed mass-to-light ratio of 0.73 (Cole et al 2001) (right axis of Fig. 3).…”