The Evolving Luminosity Function of Red Galaxies

By Michael J. I. Brown, A. Dey, B. Jannuzi, K. Brand, A. Benson, M. Brodwin, Darren Croton, Peter Eisenhardt. 2006

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We trace the assembly history of red galaxies since z = 1 by measuring their evolving space density with the B-band luminosity function. Our sample of 39,599 red galaxies, selected from 6.96 deg2 of imaging from the NOAO Deep Wide-Field Survey and the Spitzer IRAC Shallow Survey, is an order of magnitude larger, in size and volume, than comparable samples in the literature. We measure a higher space density of z ~ 0.9 red galaxies than some of the recent literature, in part because we account for the faint yet significant galaxy flux that falls outside of our photometric aperture. The B-band luminosity density of red galaxies, which effectively measures the evolution of ~L* galaxies, increases by only 36% ± 13% from z = 0 to z = 1. If red galaxy stellar populations have faded by ≃1.24 B-band magnitudes since z = 1, the stellar mass contained within the red galaxy population has roughly doubled over the past 8 Gyr. This is consistent with star-forming galaxies being transformed into ≲L* red galaxies after a decline in their star formation rates. In contrast, the evolution of ≃4L* red galaxies differs only slightly from a model with negligible z < 1 star formation and no galaxy mergers. If this model approximates the luminosity evolution of red galaxy stellar populations, then ≃80% of the stellar mass contained within today's 4L* red galaxies was already in place at z = 0.7. While red galaxy mergers have been observed, such mergers do not produce rapid growth of 4L* red galaxy stellar masses between z = 1 and the present day.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/4dc37abde38281a8a4f60bbde75f4a04a43679f1

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Constraints on intrinsic alignment contamination of weak lensing surveys using the MegaZ-LRG sample (2010, methodology): “In addition to the luminosity functions from Faber et al. (2007), we also consider fitted Schechter parameters presented in Giallongo et al. (2005), as well as the sets of luminosity functions published by Wolf et al. (2003), Willmer et al. (2006),and Brown et al. (2007).”
RED NUGGETS AT z ∼ 1.5: COMPACT PASSIVE GALAXIES AND THE FORMATION OF THE KORMENDY RELATION (2008, background): “…VIII, Abraham et al. 2007; GDDS Paper III, Glazebrook et al. 2004; Fontana et al. 2004; Rudnick et al. 2003), a process that continues at redshifts below unity as well (Faber et al. 2007; Bell et al. 2004), although the magnitude of the evolution is uncertain (Brown et al. 2007; Chen et al. 2003).”
MEASURING BARYON ACOUSTIC OSCILLATIONS ALONG THE LINE OF SIGHT WITH PHOTOMETRIC REDSHIFTS: THE PAU SURVEY (2008, methodology): “…a mock galaxy sample with L > L at z = 0.16 using the red sequence described by Cool et al. (2006), and the luminosity function described in Brown et al. (2007), and fit their g − r and r − i colors using the average template of Eisenstein et al. (2003) and the first PCA component (shown…”
PRIMUS: CONSTRAINTS ON STAR FORMATION QUENCHING AND GALAXY MERGING, AND THE EVOLUTION OF THE STELLAR MASS FUNCTION FROM z = 0–1 (2013, background): “…extent to which massive galaxies also grow through stellar accretion (i.e., mergers) remains controversial (Cimatti et al. 2006; Scarlata et al. 2007; Brown et al. 2007; Rudnick et al. 2009; Stewart et al. 2009; Ilbert et al. 2010; Pozzetti et al. 2010; Robaina et al. 2010; Maraston et al. 2012).”
CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY (2011, unknown): “As early as z ≈ 3, star formation begins to shut down rapidly in massive galaxies (e.g., Juneau et al. 2005; Papovich et al. 2006), leading to the formation of a quenched “red sequence” that grows with time (Bell et al. 2004; Faber et al. 2007; Brown et al. 2007).”
Galaxy merger morphologies and time-scales from simulations of equal-mass gas-rich disc mergers (2008, background): “…galaxy (Toomre 1977), spheroidal galaxies, red galaxies, and post-starburst galaxies have been used to indirectly trace the role of galaxy mergers in galaxy evolution (e.g. Bell et al. 2004; Faber et al. 2007; Brown et al. 2007; Abraham et al. 2007; Hopkins et al. 2007; Hogg et al. 2006).”
3D-HST+CANDELS: THE EVOLUTION OF THE GALAXY SIZE–MASS DISTRIBUTION SINCE z = 3 (2014, unknown): “…number density of L ∗ early types has strongly increased over the redshift range examined in this paper (0 < z < 3), as was shown by, e.g., Bell et al. (2004); Faber et al. (2007); Brown et al. (2007); Ilbert et al. (2010); Brammer et al. (2011); Buitrago et al. (2013); Muzzin et al. (2013).”
The Hierarchical Build-Up of Massive Galaxies and the Intracluster Light since z = 1 (2007, background): “Estimates of evolution in the luminosity function are also more or less consistent with massive galaxies passively evolving from z 1 to the present (Cirasuolo et al. 2006; Wake et al. 2006; Faber et al. 2005; Willmer et al. 2006; Brown et al. 2007; Caputi et al. 2006; Blanton 2006).”
The importance of satellite quenching for the build-up of the red sequence of present-day galaxies (2007, background): “…et al. 2004; Tanaka et al. 2005; Cooper et al. 2006; Cucciati et al. 2006; Willmer et al. 2006), and that the total stellar mass density on the red sequence has roughly doubled over the last 6–8 Gyr (e.g. Bell et al. 2004; Borch et al. 2006; Zucca et al. 2006; Brown et al. 2007; Faber et al. 2007).”
The Stellar Mass Assembly of Galaxies from z = 0 to z = 4: Analysis of a Sample Selected in the Rest-Frame Near-Infrared with Spitzer (2007, result): “Our results are consistent with the stellar population models assumed by Brown et al. (2007) for the most luminous (and probably most massive) red galaxies.”
THE NEXT GENERATION VIRGO CLUSTER SURVEY (NGVS). I. INTRODUCTION TO THE SURVEY (2012, background): “To date, even the most ambitious studies of the CMD have tended to focus on high- and intermediate-luminosity galaxies (e.g., Faber et al. 2007; Brown et al. 2007; Cassata et al. 2007; Mei et al. 2009).”
THE MAJOR AND MINOR GALAXY MERGER RATES AT z < 1.5 (2011, background): “At the same time, massive galaxies have been transformed from rapidly star-forming disk galaxies into quiescent bulge-dominated galaxies hosting super-massive black holes (e.g. Bell et al. 2004; Faber et al. 2007; Brown et al. 2007).”
Red Galaxy Growth and the Halo Occupation Distribution (2008, methodology): “While there are some discrepancies between the various surveys, which we discuss below, there is a broad consensus that the B-band luminosity density of red galaxies evolves slowly at z < 1 (Bell et al. 2004; Brown et al. 2007; Faber et al. 2007).”
WHAT TURNS GALAXIES OFF? THE DIFFERENT MORPHOLOGIES OF STAR-FORMING AND QUIESCENT GALAXIES SINCE z ∼ 2 FROM CANDELS (2011, background): “Furthermore, these two populations evolve in their relative importance: while the star-forming population has a stellar mass function that evolves slowly (Bundy et al. 2005; Borch et al. 2006; Bell et al. 2007; Peng et al. 2010; Brammer et al. 2011), the quiescent galaxy stellar mass function evolve”
Star formation and mass assembly in high-redshift galaxies (2009, background): “Several groups (e.g., Faber et al. 2007; Brown et al. 2007) studied the evolution of massive galaxies atz .”
THE NUMBER DENSITY AND MASS DENSITY OF STAR-FORMING AND QUIESCENT GALAXIES AT 0.4 ⩽ z ⩽ 2.2 (2011, background): “Furthermore, the most massive galaxies do not appear to evolve significantly at 0< z< 1 (Wake et al. 2006; Brown et al. 2007), implying that they were assembled at higher redshifts.”
Galaxy luminosities, stellar masses, sizes, velocity dispersions as a function of morphological type (2009, background): “Journal compilation C© 2010 RAS, MNRAS 404, 2087–2122 Downloaded from https://academic.oup.com/mnras/article-abstract/404/4/2087/1088291 by guest on 28 July 2018 et al. 2006; Brown et al. 2007; Cool et al. 2008).”