The Galaxy Luminosity Function and Luminosity Density at Redshift z = 0.1

By M. Blanton, David W. Hogg, J. Brinkmann, Andrew J. Connolly, István Csabai, N. Bahcall, M. Fukugita, J. Loveday, A. Meiksin, J. Munn and 9 more. 2002

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Using a catalog of 147,986 galaxy redshifts and fluxes from the Sloan Digital Sky Survey (SDSS), we measure the galaxy luminosity density at z = 0.1 in five optical bandpasses corresponding to the SDSS bandpasses shifted to match their rest-frame shape at z = 0.1. We denote the bands 0.1u, 0.1g, 0.1r, 0.1i, 0.1z with λeff = (3216, 4240, 5595, 6792, 8111 Å), respectively. To estimate the luminosity function, we use a maximum likelihood method that allows for a general form for the shape of the luminosity function, fits for simple luminosity and number evolution, incorporates the flux uncertainties, and accounts for the flux limits of the survey. We find luminosity densities at z = 0.1 expressed in absolute AB magnitudes in a Mpc3 to be (-14.10 ± 0.15, -15.18 ± 0.03, -15.90 ± 0.03, -16.24 ± 0.03, -16.56 ± 0.02) in (0.1u, 0.1g, 0.1r, 0.1i, 0.1z), respectively, for a cosmological model with Ω0 = 0.3, ΩΛ = 0.7, and h = 1 and using SDSS Petrosian magnitudes. Similar results are obtained using Sérsic model magnitudes, suggesting that flux from outside the Petrosian apertures is not a major correction. In the 0.1r band, the best-fit Schechter function to our results has ϕ* = (1.49 ± 0.04) × 10-2 h3 Mpc-3, M* - 5 log10 h = -20.44 ± 0.01, and α = -1.05 ± 0.01. In solar luminosities, the luminosity density in 0.1r is (1.84 ± 0.04) × 108 h L0.1r,☉ Mpc-3. Our results in the 0.1g band are consistent with other estimates of the luminosity density, from the Two-Degree Field Galaxy Redshift Survey and the Millennium Galaxy Catalog. They represent a substantial change (~0.5 mag) from earlier SDSS luminosity density results based on commissioning data, almost entirely because of the inclusion of evolution in the luminosity function model.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/67a8584c42ba716ed0b58d2c0ae9068e4663c99a

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Citations in the corpus

The Sloan Digital Sky Survey Quasar Survey: Quasar Luminosity Function from Data Release 3 (2006, methodology): “Therefore, in this paper, we follow Wisotzki (2000) and Blanton et al. (2003a) and K-correct to a redshift closer to the median redshift of our sample.”
Galaxy groups and clouds in the local (z∼ 0.01) Universe (2010, methodology): “For instance, using the data of (Blanton et al. 2003) on total luminosity density and (Zandivarez et al. 2006) on luminosity function in groups from SDSS survey and taking into account the fraction of galaxies in groups (54 per cent), we receive that only 20 per cent of the total light is…”
Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation (2014, methodology): “The luminosity evolution of the SDSS galaxies is estimated in Blanton et al. (2003), where they basically assume that the luminosity function of galaxies is constant with distance.”
The physical properties of star-forming galaxies in the low-redshift universe (2003, methodology): “Number distributions as function of many photometric properties and as a function of local density have been discussed in detail by Blanton et al. (2003b) and by Hogg et al. (2003).”
THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS (2007, methodology): “All reported magnitudes are adjusted to this redshift, and are noted as e.g., 0.25Mi. Blanton et al. (2003b) give a complete discussion of this bandpass shifting procedure.”
Satellite kinematics – III. Halo masses of central galaxies in SDSS (2010, positive): “1(z) is the k-correction to redshift z = 0.1, 1.62 is the evolution correction factor from Blanton et al. (2003a), and DM(z) is given by DM(z) = 5 logDL(z) + 25.0 , (A2) where DL(z) is the luminosity distance of the galaxy in h−1Mpc.”
What Shapes the Luminosity Function of Galaxies? (2003, result): “While the slope is not as flat as that measured by Cole et al. (2001) or Blanton et al. (2003), it is in good agreement with the steeper slope reported by Huang et al. (2003).”
New York University Value-Added Galaxy Catalog: A Galaxy Catalog Based on New Public Surveys (2004, methodology): “Given the tiling region and the set of targets within it, we determine the location of spectroscopic tiles of radius 1N49 and decide to which targets to assign fibers (Blanton et al. 2003a).”
Stellar masses of SDSS-III/BOSS galaxies at z ∼ 0.5 and constraints to galaxy formation models (2012, background): “In the local universe, recent results on the stellar mass function of galaxies include Blanton et al. (2003), Bell et al. (2003), Baldry et al. (2004), Baldry et al. (2006), Baldry et al. (2008), Li & White (2009), Baldry et al. (2012).”
Molecular Hydrogen and Global Star Formation Relations in Galaxies (2007, background): “For example, the faint-end of the galaxy luminosity function has a shallow slope (αL ≈ 1.0 − 1.3, e.g., Blanton et al. 2001, 2003) compared to the steeper mass function of dark matter halos (αDM ≈ 2, e.g., Press & Schechter 1974; Sheth & Tormen 1999), indicating a decrease in SFE in low-mass…”
Dark matter in elliptical galaxies — II. Estimating the mass within the virial radius (2004, methodology): “We also showed in paper I that the mass-to-light ratio of the Universe is ΥB = Ωm Υclosure,B = 3ΩmH 2 0 8π GjB = 390 h70 , (20) given the luminosity density found by Liske et al. (2003) and Blanton et al. (2003) in the2dFGRS andSDSS surveys, respectively.”
A CATALOG OF BULGE+DISK DECOMPOSITIONS AND UPDATED PHOTOMETRY FOR 1.12 MILLION GALAXIES IN THE SLOAN DIGITAL SKY SURVEY (2011, background): “Blanton et al. (2003) reported a systematic trend between their Sérsicbased magnitude and SDSS Petrosian magnitudes as a function of the Sérsic index value with Petrosian magnitudes underestimating the g- and r-band fluxes by 20% in their high (n ≃ 4) Sérsic index galaxies.”
THE COS-HALOS SURVEY: AN EMPIRICAL DESCRIPTION OF METAL-LINE ABSORPTION IN THE LOW-REDSHIFT CIRCUMGALACTIC MEDIUM (2012, methodology): “In the following, we restrict the study to galaxies with L > 0.1L∗ to isolate L ≈ L∗ galaxies, where we use the R-band absolute magnitude of −21.2 for an L∗ galaxy (Blanton et al. 2003).”
The Physics of Galaxy Clustering. I. A Model for Subhalo Populations (2004, background): “15), which is close to the observed number density of galaxies with rband absolute magnitudes of Mr<∼ − 19.5 (Blanton et al. 2003).”
The Velocity Dispersion Function of Early-Type Galaxies (2003, positive): “The luminosity function of the entire SDSS sample, φtot(L), has been estimated by Blanton et al. (2003).”
An Observational Determination of the Bolometric Quasar Luminosity Function (2006, background): “These problems are well known from local galaxy luminosity functions and can introduce significant effects even in samples spanning the range z 0Y0:1 (see, e.g., Blanton et al. 2003), where many of the low-redshift QLF measurements cover a significantly larger z 0Y0:3.”
Active Galactic Nuclei in the Sloan Digital Sky Survey. II. Emission-Line Luminosity Function (2005, methodology): “We start from a lowredshift (z < 0:33) galaxy sample that is complete in r-band Petrosian magnitude at 17.77 (Strauss et al. 2002) over 1151 deg2 (see Zakamska et al. [2003] for a selection of high-redshift type II quasars from the SDSS).”
IDENTIFYING ELUSIVE ELECTROMAGNETIC COUNTERPARTS TO GRAVITATIONAL WAVE MERGERS: AN END-TO-END SIMULATION (2012, background): “The number density of galaxies is 0.6 per deg2 per Mpc at z=0.1 and L>0.1 L? and scales with z 2 (Blanton et al. 2003).”
THE CONNECTION BETWEEN GALAXIES AND DARK MATTER STRUCTURES IN THE LOCAL UNIVERSE (2012, methodology): “The NYU-VAGC is based on the SDSS spectroscopic sample.”
Galaxy ecology: groups and low-density environments in the SDSS and 2dFGRS (2003, methodology): “In particular, we will consider the rest frame Petrosian (g−r) colour, denoted (g−r)0, and use the k-corrections of Blanton et al. (2003a).”