The DEEP2 Galaxy Redshift Survey: The Galaxy Luminosity Function to z ~ 1

By C. Willmer, S. Faber, D. Koo, B. Weiner, J. Newman, A. Coil, Andrew J. Connolly, C. Conroy, M. Cooper, Michael Davis and 13 more. 2005

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The evolution of the B-band galaxy luminosity function is measured using a sample of more than 11,000 galaxies with spectroscopic redshifts from the DEEP2 Redshift Survey. The rest-frame M_B versus U-B color-magnitude diagram of DEEP2 galaxies shows that the color-magnitude bi-modality seen in galaxies locally is still present at redshifts z > 1. Dividing the sample at the trough of this color bimodality into predominantly red and blue galaxies, we find that the luminosity function of each galaxy color type evolves differently. Blue counts tend to shift to brighter magnitudes at constant number density, while the red counts remain largely constant at a fixed absolute magnitude. Using Schechter functions with fixed faint-end slopes we find that M*_B for blue galaxies brightens by ~ 1.3 magnitudes per unit redshift, with no significant evolution in number density. For red galaxies M*_B brightens somewhat less with redshift, while the formal value of phi* declines. When the population of blue galaxies is subdivided into two halves using the rest-frame color as the criterion, the measured evolution of both blue subpopulations is very similar.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d335838a9c116b341e5bb1ac6971b35991c141bb

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Citations in the corpus

THE MAJOR AND MINOR GALAXY MERGER RATES AT z < 1.5 (2011, methodology): “This work reanalyzes paired galaxies from the TeamKeck Treasury Redshift Survey (Wirth et al. 2004), DEEP2 Galaxy Redshift Survey (Davis et al. 2004; Lin et al. 2004), CNOC2 Survey (Yee et al. 2000; Patton et al. 2002), and Millennium Galaxy Survey (Liske et al. 2003; de Propris et al. 2005) with a ”
Rates and Properties of Type Ia Supernovae as a Function of Mass and Star Formation in Their Host Galaxies (2006, methodology): “…an alternative approach would be to use a parameterized form of the mass or luminosity functions, either directly inferred from high-redshift spectroscopic surveys (e.g., Ilbert et al. 2005; Willmer et al. 2005; Bundy et al. 2005) or lowredshift functions adjusted for evolution to high redshift.”
The Evolving Luminosity Function of Red Galaxies (2006, methodology): “0.2 < z < 0.4 65 20:27 0:270:31 21.66 (5.15 0.64) ; 10 3 0.29 0.4 < z < 0.6 106 20:49 0:170:18 21.67 (3.12 0.30) ; 10 3 0.29 0.6 < z < 0.8 197 20:22 0:090:10 21.46 (3.53 0.35) ; 10 3 0.29 0.8 < z < 1.0 164 20:73 0:110:12 21.76 (2.36 0.18) ; 10 3 0.29 1.0 < z < 1.2 114 20:53 0:110:12 21.57 (2.39 0.22”
INSPIRALLING SUPERMASSIVE BLACK HOLES: A NEW SIGNPOST FOR GALAXY MERGERS (2008, methodology): “We compute rest-frame U−B colors and MB absolute magnitudes using a K-correction code developed for DEEP2 galaxies (Willmer et al. 2006).”
The Stellar Mass Tully-Fisher Relation to z = 1.2 from AEGIS (2006, background): “A redshift limit of z = 1.2 ensures that galaxies of all colors on the “blue sequence” (Willmer et al. 2006) are well-sampled.”
HYDROGEN-POOR SUPERLUMINOUS SUPERNOVAE AND LONG-DURATION GAMMA-RAY BURSTS HAVE SIMILAR HOST GALAXIES (2013, background): “The overall range is −16 to −22 mag, but the population is strikingly low-luminosity with a median absolute magnitude of 〈MB〉 ≈ −17.6 mag (≈0.05L∗; Willmer et al. 2006).”