The VIMOS VLT deep survey: the assembly history of the stellar mass in galaxies: from the young to the old universe

By L. Pozzetti, M. Bolzonella, F. Lamareille, G. Zamorani, P. Franzetti, O. Fèvre, A. Iovino, S. Temporin, O. Ilbert, Stéphane Arnouts and 40 more. 2007

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We present a detailed analysis of the Galaxy Stellar Mass Function of galaxies up to z=2.5 as obtained from the VVDS. We estimate the stellar mass from broad-band photometry using 2 different assumptions on the galaxy star formation history and show that the addition of secondary bursts to a continuous star formation history produces systematically higher (up to 40%) stellar masses. At low redshift (z=0.2) we find a substantial population of low-mass galaxies ( 10^8 Msun at z=1), and a mild mass-dependent average evolution (`mass-downsizing'). In particular our data are consistent with mild/negligible ( 6x10^10 Msun). For less massive systems the no-evolution scenario is excluded. A large fraction (>=50%) of massive galaxies have been already assembled and converted most of their gas into stars at z=1, ruling out the `dry mergers' as the major mechanism of their assembly history below z=1. This fraction decreases to 33% at z=2. Low-mass systems have decreased continuously in number and mass density (by a factor up to 4) from the present age to z=2, consistently with a prolonged mass assembly also at z 1.5 we note a flattening in the number and mass density of massive galaxies, compared to previous surveys, produced by a population with extremely red colours (MI-MK=0.8).

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/2149155d1559c6e0bac05c0d7362d2520b78d6d4

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Citations in the corpus

The SEDs and host galaxies of the dustiest GRB afterglows (2011, background): “Systematic uncertainties of up to an average of 0.2−0.3 dex in M∗ are caused by the specific details of the stellar population models and the assumed attenuation/extinction law (Pozzetti et al. 2007; Küpcü Yoldaş et al. 2007; Kajisawa et al. 2009; Ilbert et al. 2010).”
CFHTLenS: the relation between galaxy dark matter haloes and baryons from weak gravitational lensing (2013, methodology): “The additional near-infrared data allows us to rely on these estimates up to a redshift of 1.5 (Pozzetti et al. 2007).”
The VIMOS VLT Deep Survey final data release: a spectroscopic sample of 35 016 galaxies and AGN out to z ~ 6.7 selected with 17.5 ≤ iAB ≤ 24.75 (2013, background): “…above, based on a complete census of the galaxy population (e.g. Ilbert et al. 2005; Le Fèvre et al. 2005b; Cucciati et al. 2006; Arnouts et al. 2007; Franzetti et al. 2007; Pozzetti et al. 2007; Tresse et al. 2007; Guzzo et al. 2008; Zucca et al. 2008; de Ravel et al. 2009; Meneux et al. 2009).”
PRIMUS: CONSTRAINTS ON STAR FORMATION QUENCHING AND GALAXY MERGING, AND THE EVOLUTION OF THE STELLAR MASS FUNCTION FROM z = 0–1 (2013, result): “By contrast, previous studies have found much stronger evidence for downsizing within the global galaxy population (see, e.g., Fontana et al. 2006; Pérez-González et al. 2008; Pozzetti et al. 2007, 2010).”
The dependence of Type Ia Supernovae luminosities on their host galaxies (2010, methodology): “We note that the use of stochastic SFHs results in increased derived stellar masses of galaxies by about 0.14 dex (Pozzetti et al. 2007; Lamareille et al. 2009).”
The many manifestations of downsizing: hierarchical galaxy formation models confront observations (2009, methodology): “Similarly, using different libraries of SF histories has an effect on the final mass determination (Pozzetti et al. 2007; Stringer et al. 2009).”
A new measurement of the evolving near-infrared galaxy luminosity function out to z≃ 4: a continuing challenge to theoretical models of galaxy formation (2008, background): “…the advent of the Spitzer satellite has provided the opportunity to derive reliable estimates for the stellar masses in galaxies at high redshift, allowing a direct study of the evolution of the mass function (Fontana 2004, 2006; Drory et al. 2005; Perez-Gonzalez et al. 2008; Pozzetti et al. 2007).”
The VIMOS VLT Deep Survey - Evolution of the major merger rate since z ~ 1 from spectroscopically confirmed galaxy pairs (2008, unknown): “…contribution of merging to the evolution process and its impact on important quantities like the cosmic star formation rate (e.g. Bouwens et al., 2006; Tresse et al., 2007; Woods et al., 2006) or the global stellar mass density (e.g. Arnouts et al., 2007; Bundy et al., 2005; Pozzetti et al., 2007).”
Constraining the properties of AGN host galaxies with spectral energy distribution modelling (2015, methodology): “This approach for inferring galaxy parameters has also been extensively tested to identify limitations and potential sources of systematics (e.g. Pozzetti et al. 2007; Marchesini et al. 2009; Conroy et al. 2009; Wuyts et al. 2009; Ilbert et al. 2010; Michałowski et al. 2012; Pforr et al. 2012;…”
Accreting supermassive black holes in the COSMOS field and the connection to their host galaxies (2012, methodology): “Following Fontana et al. (2006) and Pozzetti et al. (2007), we impose the prior Eg(B − V) < 0.15 if tage/τ > 4 (i.e. we exclude the models implying large dust extinctions in the absence of a significant SFR, tage/τ > 4).”
THE EVOLUTION OF GALAXY NUMBER DENSITY AT z < 8 AND ITS IMPLICATIONS (2016, methodology): “These fits are all normalized to have the same Salpeter IMF with Pozzetti et al. (2007), Duncan et al. (2014), and Mortlock et al. (2015) originally using a Chabrier IMF, and Muzzin et al. (2013) using a Kroupa IMF.”
Tracking the impact of environment on the galaxy stellar mass function up to z ~ 1 in the 10 k zCOSMOS sample (2009, methodology): “We applied 2 priors (the same used in Pozzetti et al. 2007, and proposed by Fontana et al. 2004 and Kauffmann et al. 2003) to avoid such a problem.”
THE MAJOR AND MINOR GALAXY MERGER RATES AT z < 1.5 (2011, methodology): “…green asterisks); Bottom: ngal(z) for galaxies selected with Mstar > 1010M⊙ from Bell et al. 2003 (2MASS, black square), Bundy et al. 2005 (GOODS, black filled circles), Ilbert et al. 2009 (black diamonds), Pozzetti et al. 2007 (VVDS, open circles), and Bundy et al 2006 (DEEP2, black asterisks).”
Modelling and interpreting spectral energy distributions of galaxies with BEAGLE (2016, methodology): “…tool, we follow an alternative approach, similar that adopted by Acquaviva, Raichoor & Gawiser (2015, see also HYPERZ, Bolzonella et al. 2000; Pozzetti et al. 2007), and consider redshift just as an additional model parameter to be constrained along with the other physical parameters when…”
Post-starburst galaxies: more than just an interesting curiosity (2008, methodology): “Pozzetti et al. (2007) calculate the total mass density of galaxies as a function of redshift in the VVDS spectroscopic sample, using the same Chabrier (2003) IMF as used in this work.”
Fitting the integrated spectral energy distributions of galaxies (2010, result): “Pozzetti et al. (2007) found a similar difference (0.14 dex) when comparing Bruzual and Charlot (2003) and Maraston (2005) models.”
Multiwavelength Study of Massive Galaxies at z~2. I. Star Formation and Galaxy Growth (2007, background): “…density of massive galaxies takes place in the cosmic time interval between z 3 and 1 (e.g., Dickinson et al. 2003; Rudnick et al. 2003, 2006; Fontana et al. 2004, 2006; Daddi et al. 2004a, hereafter D04a; van Dokkum et al. 2006; Franceschini et al. 2006; Pozzetti et al. 2007; Arnouts et al. 2007).”