The 2dF Galaxy Redshift Survey: galaxy luminosity functions per spectral type

By D. Madgwick, Ofer Lahav, I. Baldry, C. Baugh, Joss Bland-Hawthorn, T. Bridges, R. Cannon, Shaun Cole, M. Colless, C. Collins and 17 more. 2001

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We calculate the optical bJ luminosity function of the 2dF Galaxy Redshift Survey (2dFGRS) for different subsets defined by their spectral properties. These spectrally selected subsets are defined using a new parameter, �, which is a linear combination of the first two projections derived from a Principal Component Analysis. This parameter � identifies the average emission and absorption line strength in the galaxy rest-frame spectrum and hence is a useful indicator of the present star formation. We use a total of 75,000 galaxies in our calculations, chosen from a sample of high signal-tonoise ratio, low redshift galaxies observed before January 2001. We find that there is a systematic steepening of the faint end slope (�) as one moves from passive (� = 0.54) to active (� = 1.50) star-forming galaxies, and that there is also a corresponding faintening of the rest-frame characteristic magnitude M � 5log10(h) (from 19.6 to 19.2). We also show that the Schechter function provides a poor fit to the quiescent (Type 1) LF for very faint galaxies (MbJ 5log10(h) fainter than 16.0), perhaps suggesting the presence of a significant dwarf population. The luminosity functions presented here give a precise confirmation of the trends seen previously in a much smaller preliminary 2dFGRS sample, and in other surveys. We also present a new procedure for determining self-consistent K-corrections and investigate possible fibreaperture biases.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a2623a42b39c794d649112ce742d5c5a26fb1d3e

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Citations in the corpus

The Evolution and Structure of Early-Type Field Galaxies: A Combined Statistical Analysis of Gravitational Lenses (2004, background): “…luminous matter inside an aperture R is then M lum(R) ¼ L Lev L 1þx g R Re ; ð10Þ where quantities are scaled relative to those of an L *galaxy, which we define as having a present-day (z ¼ 0) characteristic magnitude of M (0) ¼ 19:9þ 5 log h in the rest-frame B band (e.g., Madgwick et al. 2002).”
The DEEP2 galaxy redshift survey: evolution of the colour–density relation at 0.4 < z < 1.35 (2006, methodology): “Parameters for the HOD and the CLF are chosen to match the 2dFGRS luminosity function (Madgwick et al. 2002) and two–point correlation function (Madwgick et al. 2003).”
The many lives of active galactic nuclei: cooling flows, black holes and the luminosities and colour (2005, methodology): “For comparison we overplot observational results from Madgwick et al. (2002) for 2dFGRS galaxies split by spectral type.”
Galaxy pairs in the 2dF survey — I. Effects of interactions on star formation in the field (2002, unknown): “We notice that the dependence of b on η estimated by Madgwick et al. (2002b) is stronger than the linear one adopted in this paper.”
Early-type Galaxies in the Sloan Digital Sky Survey. II. Correlations between Observables (2003, methodology): “The 2dF Galaxy Redshift Survey (2dFGRS) galaxies classified as being of type 1 by Madgwick et al. (2002) should be similar to early types.”
Constraints on a Universal Stellar Initial Mass Function from Ultraviolet to Near-Infrared Galaxy Luminosity Densities (2003, background): “From Madgwick et al. (2002), 61% and 39% are the fractional contributions to the bJ band from late and early types, respectively, based on spectroscopic classification (assuming spectral types 2–4 for late, type 1 for early).”
Deep GALEX Imaging of the COSMOS HST Field: A First Look at the Morphology of z ~ 0.7 Star-forming Galaxies (2007, background): “In particular, large surveys such as SDSS (York et al. 2000) and 2dF Galaxy Redshift Survey (e.g. Madgwick et al. 2002) have really propelled statistical studies of galaxy properties.”
The 6dF Galaxy Survey: Samples, observational techniques and the first data release (2004, background): “…the precise determination of the luminosity function of galaxies (e.g. Folkes et al. 1999; Blanton et al. 2001; Cole et al. 2001; Cross et al. 2001; Madgwick et al. 2002; Norberg et al. 2002; Blanton et al. 2003), the space density of nearby rich galaxy clusters (De Propris et al. 2002; Goto et…”
GALAXY GROUPS IN THE SDSS DR4. III. THE LUMINOSITY AND STELLAR MASS FUNCTIONS (2008, background): “Both functions have been extensively investigated in the literature for galaxies of different colors and morphological types (e.g., Lin et al. 1996; Norberg et al. 2002; Madgwick et al. 2002; Blanton et al. 2003b; Bell et al. 2003; Fontana et al. 2006).”
The 2dF Galaxy Redshift Survey: Luminosity functions by density environment and galaxy type (2004, methodology): “In addition, the extreme underdense and overdense regions of the survey are further dissected as a function of 2dFGRS galaxy spectral type, η, which can approximately be cast as earlyand late-type galaxy populations (Madgwick et al. 2002, see Section 2).”
The Velocity Dispersion Function of Early-Type Galaxies (2003, background): “The same theoretical models also predict the distribution of luminosities, the galaxy luminosity function, which is much easier to measure (see, e.g., the recent determinations by Cross et al. 2001; Blanton et al. 2002; Madgwick et al. 2002).”
Galaxy groups in the 2dFGRS: the group-finding algorithm and the 2PIGG catalogue (2004, background): “…a number of observables that have a direct 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…”
The VIMOS VLT Deep Survey. Evolution of the luminosity functions by galaxy type up to z = 1.5 from first epoch data (2005, unknown): “Madgwick et al. (2002), analyzing 2dFGRS data, find a systematic steepening of the faint end slope and a faintening of M∗ of the luminosity function as one moves from passive to active star forming galaxies.”
Optical and Radio Properties of Extragalactic Sources Observed by the FIRST Survey and the Sloan Digital Sky Survey (2002, background): “…than that limit also have spectra (region IId), because they are targeted for SDSS spectroscopy as the luminous red 48 Blanton et al. (2001) find that galaxies withMr d 22 are dominated by red galaxies (see also Madgwick et al. 2002 for consistent results based on the 2dFGalaxy Redshift Survey).”
Early-Type Galaxies in the Sloan Digital Sky Survey. I. The Sample (2003, methodology): “Rather than follow the procedure adopted by the 2dFGRS (Madgwick et al. 2002) or a procedure based on finding the closest template spectrum to each galaxy and using it to compute theK-correction (e.g., Lin et al. 1999 for the CNOC2 survey), we use a single redshift-dependent template spectrum to…”
Scaling relations and the fundamental line of the local group dwarf galaxies (2008, methodology): “Our program for PCA is a modified version of a routine kindly provided to us by Ofer Lahav (described in Madgwick et al. 2002).”