The Mass Assembly Histories of Galaxies of Various Morphologies in the GOODS Fields

By K. Bundy, Richard S. Ellis, Christopher J. Conselice. 2005

291 citations recorded by the source corpus.

We present an analysis of the growth of stellar mass with cosmic time partitioned according to galaxy morphology. Using a well-defined catalog of 2150 galaxies based, in part, on archival data in the Great Observatories Origins Deep Survey (GOODS) fields, we assign morphological types in three broad classes (ellipticals, spirals, peculiar/irregulars) to a limit of zAB = 22.5 and make the resulting catalog publicly available. Utilizing 893 spectroscopic redshifts, supplemented by 1013 determined photometrically, we combine optical photometry from the GOODS catalog and deep Ks-band imaging to assign stellar masses to each galaxy in our sample. We find little evolution in the form of the galaxy stellar mass function from z ~ 1 to z = 0, especially at the high-mass end where our results are most robust. Although the population of massive galaxies is relatively well established at z ~ 1, its morphological mix continues to change, with an increasing proportion of early-type galaxies at later times. By constructing type-dependent stellar mass functions, we show that in each of three redshift intervals, E/S0 galaxies dominate the higher mass population, while spirals are favored at lower masses. This transition occurs at a stellar mass of (2-3) × 1010 M☉ at z ~ 0.3 (similar to local studies), but there is evidence that the relevant mass scale moves to higher mass at earlier epochs. Such evolution may represent the morphological extension of the "downsizing" phenomenon, in which the most massive galaxies stop forming stars first, with lower mass galaxies becoming quiescent later. We infer that more massive galaxies evolve into spheroidal systems at earlier times, and that this morphological transformation may only be completed 1-2 Gyr after the galaxies emerge from their active star-forming phase. We discuss several lines of evidence suggesting that merging may play a key role in generating this pattern of evolution.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d70049ae7d67b939b7d775420645fd32b8023177

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. V. IMPROVING THE DARK-ENERGY CONSTRAINTS ABOVE z > 1 AND BUILDING AN EARLY-TYPE-HOSTED SUPERNOVA SAMPLE (2011, background): “The GOODS survey (Dickinson et al. 2003; Riess et al. 2004, 2007; Kuznetsova et al. 2008) is an example that provided a window to probe the high-z universe for studying galaxy evolution (e.g. Beckwith et al. 2006; Bouwens et al. 2006; Bundy et al. 2005) in addition toz > 1 SNe.”
The Hierarchical Build-Up of Massive Galaxies and the Intracluster Light since z = 1 (2007, background): “Evolution in the galaxy stellar mass function (GSMF) since z 1 appears quite mild for the most massive galaxies (Fontana et al. 2004, 2006; Drory et al. 2004; Bundy et al. 2005; Borch et al. 2006; Cimatti et al. 2006; Andreon 2006).”
STAR FORMATION AND DUST OBSCURATION AT z ≈ 2: GALAXIES AT THE DAWN OF DOWNSIZING (2009, methodology): “…consensus has been reached in the last years on the evolution of the galaxy stellar mass function (e.g. Dickinson et al. 2003; Drory et al. 2004; Bundy et al. 2005; Pannella et al. 2006; Fontana et al. 2006; Marchesini et al. 2008), the red- * Based on observations collected, within the COSMOS…”
A census of metals and baryons in stars in the local universe (2007, background): “…occurred at high redshifts, while low-mass galaxies are still in a phase of active star formation (e.g. Brinchmann & Ellis 2000; Juneau et al. 2005; Bundy et al. 2005), although galaxies appear to experience the same rate of decline in their global star formation from z ∼ 1 to the present…”
Breaking the hierarchy of galaxy formation (2005, background): “Recent measurements of stellar mass reveal a substantial population of large galaxies at z = 1 and beyond (Drory et al. 2003, 2005; Pozzetti et al. 2003; Fontana et al. 2004; Kodama et al. 2004; Bundy et al. 2005).”
Properties of Early-Type, Dry Galaxy Mergers and the Origin of Massive Elliptical Galaxies (2005, background): “A threshold value like this has been proposed recently (Bundy et al. 2005; Bell et al. 2005).”
The VIMOS VLT Deep Survey - Evolution of the major merger rate since z ~ 1 from spectroscopically confirmed galaxy pairs (2008, unknown): “Our finding that∼ 20% of the stellar mass in present day massive galaxies has experienced a major merger sincez ∼ 1 is an indication that major mergers are significantly contributing to the observed evolution of thest llar mass density sincez ∼ 1 (Bundy et al., 2005; Arnouts et al., 2007).”
Integral field spectroscopy with SINFONI of VVDS galaxies I. Galaxy dynamics and mass assembly at 1.2 < z < 1.6 (2009, background): “A clear result now emerging is that early type galaxies have experienced a major growth in stellar mass density from a redshiftz ∼ 2 to z ∼ 1, while late-type galaxies have been growing their stellar mass more slowly inthis period (e.g. Arnouts et al. 2007; Bundy et al. 2005).”
PRIMUS: CONSTRAINTS ON STAR FORMATION QUENCHING AND GALAXY MERGING, AND THE EVOLUTION OF THE STELLAR MASS FUNCTION FROM z = 0–1 (2013, background): “…Bayesian formalism pioneered by Kauffmann et al. (2003a) to model the optical spectral features of SDSS galaxies, and its subsequent extension to broadband photometry (e.g., Bundy et al. 2005; Salim et al. 2005, 2007; da Cunha et al. 2008; Auger et al. 2009; McGee et al. 2011; Taylor et al. 2011).”
Fueling Low-Level AGN Activity through Stochastic Accretion of Cold Gas (2006, methodology): “…to be the same in the overlapping redshift interval 0.2< z< 0.55, we extend this with the morphologically classified spiral mass functions from Bundy et al. (2005) and Franceschini et al. (2006) up toz = 1.4, and then repeat this with the Fontana et al. (2004) observations to infer the mass…”
THE RISE AND FALL OF PASSIVE DISK GALAXIES: MORPHOLOGICAL EVOLUTION ALONG THE RED SEQUENCE REVEALED BY COSMOS (2009, methodology): “…galaxies to show that automated estimators are generally robust to K-corrections, but to address this problem further and check our ZEST-based results more generally, we use the visually classified morphologies in the northern GOODS-N (Giavalisco et al. 2004) as presented in Bundy et al. (2005).”
Galaxy Zoo: the fraction of merging galaxies in the SDSS and their morphologies (2009, background): “…such studies have concentrated mostly on merger rates (Carlberg et al. 2000; Le Fevre et al. 2000; Patton et al. 2002; Conselice et al. 2003; Bundy et al. 2005; Bell et al. 2006; Conselice, Rajgor & Myers 2008; Lin et al. 2008; Lotz et al. 2008a; Hsieh. et al. 2008, Patton et al. 2008),…”
Galaxy merger morphologies and time-scales from simulations of equal-mass gas-rich disc mergers (2008, background): “Morphological disturbances can be found qualitatively through visual inspection (e.g. Kampczyk et al. 2007; Bundy et al. 2005; Brinchmann et al. 1998), or by quantitative measures such as the Gini coefficient, second-order moment of the brightest 20% of the light (M20), and asymmetry (Abraham et…”
A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. II. Formation of Red Ellipticals (2007, background): “However, those systems that can be clearly identified as truly passive appear to be overwhelmingly compact spheroids (McIntosh et al. 2005; Bundy et al. 2005), even at z 2Y3 (Labbé et al. 2005; Kriek et al. 2006; Zirm et al. 2007).”
The Galaxy Mass Function up to z=4 in the GOODS-MUSIC sample: into the epoch of formation of massive galaxies ⋆ (2006, unknown): “…by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20065475 a significant evolution, with an increase in the fraction of stellar mass residing in late type galaxies at z 1−1.5 with respect to low redshift (F04; Bundy et al. 2005; Franceschini et al. 2006).”
The WIRCam Deep Survey I. Counts, colours, and mass-functions derived from near-infrared imaging in the CFHTLS deep fields (2011, background): “A number of studies have analysed the evolution of the buildup of stellar mass in galaxies via the stellar mass function,finding that the stellar mass density approximately doubles betwe n z ∼ 1 andz ∼ 0 (e.g. Bundy et al. 2005, 2006; Borch et al. 2006; Pannella et al. 2006).”
AN ALMA SURVEY OF SUBMILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: THE REDSHIFT DISTRIBUTION AND EVOLUTION OF SUBMILLIMETER GALAXIES (2013, methodology): “We use a catalog from Bundy et al. (2005), which provides morphological classifications for z < 22.5 mag galaxies in the GOODS–South field.”
STELLAR AND TOTAL BARYON MASS FRACTIONS IN GROUPS AND CLUSTERS SINCE REDSHIFT 1 (2009, background): “For instance, the stellar mass completeness at z=1 (Mcompl = 10 10.4M⊙) is about an order of magnitude lower than the so-called “transition” stellar mass at z ≤ 1 (e.g. Bundy et al. 2005; Pannella et al. 2006).”