THE EVOLUTION OF THE STELLAR MASS FUNCTIONS OF STAR-FORMING AND QUIESCENT GALAXIES TO z = 4 FROM THE COSMOS/UltraVISTA SURVEY

By A. Muzzin, D. Marchesini, M. Stefanon, M. Franx, H. McCracken, Bo, Milvang-Jensen, J. Dunlop, Johan Peter Uldall Fynbo, G. Brammer and 2 more. 2013

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We present measurements of the stellar mass functions (SMFs) of star-forming and quiescent galaxies to z = 4 using a sample of 95,675 Ks-selected galaxies in the COSMOS/UltraVISTA field. The SMFs of the combined population are in good agreement with previous measurements and show that the stellar mass density of the universe was only 50%, 10%, and 1% of its current value at z ∼ 0.75, 2.0, and 3.5, respectively. The quiescent population drives most of the overall growth, with the stellar mass density of these galaxies increasing as ρstar∝(1 + z)−4.7 ± 0.4 since z = 3.5, whereas the mass density of star-forming galaxies increases as ρstar∝(1 + z)−2.3 ± 0.2. At z > 2.5, star-forming galaxies dominate the total SMF at all stellar masses, although a non-zero population of quiescent galaxies persists to z = 4. Comparisons of the Ks-selected star-forming galaxy SMFs with UV-selected SMFs at 2.5 < z < 4 show reasonable agreement and suggest that UV-selected samples are representative of the majority of the stellar mass density at z > 3.5. We estimate the average mass growth of individual galaxies by selecting galaxies at fixed cumulative number density. The average galaxy with log(Mstar/M☉) = 11.5 at z = 0.3 has grown in mass by only 0.2 dex (0.3 dex) since z = 2.0 (3.5), whereas those with log(Mstar/M☉) = 10.5 have grown by >1.0 dex since z = 2. At z < 2, the time derivatives of the mass growth are always larger for lower-mass galaxies, which demonstrates that the mass growth in galaxies since that redshift is mass-dependent and primarily bottom-up. Lastly, we examine potential sources of systematic uncertainties in the SMFs and find that those from photo-z templates, stellar population synthesis modeling, and the definition of quiescent galaxies dominate the total error budget in the SMFs.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/f889e23c77333a50772e2a3faef2ff5754055f36

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Citations in the corpus

THE RELATION BETWEEN STAR FORMATION RATE AND STELLAR MASS FOR GALAXIES AT 3.5 ⩽ z ⩽ 6.5 IN CANDELS (2014, unknown): “The purple error bars show the 68% range of errors from the Monte Carlo simulations described in § 5.2.1. our sample (Straatman et al. 2013; Muzzin et al. 2013; Spitler et al. in prep.).”
The mass evolution of the first galaxies: stellar mass functions and star formation rates at 4 < z < 7 in the CANDELS GOODS-South field (2014, result): “At the massive end of the z ∼ 4 galaxy SMF, our results agree with those of Muzzin et al. (2013) over the limited mass range covered by both works.”
Constraining the properties of AGN host galaxies with spectral energy distribution modelling (2015, background): “It is common practice instead, to assume simple functional forms, such as an exponentially decreasing SFR (1τ-dec, e.g., Ilbert et al. 2013; Muzzin et al. 2013), an exponentially increasing SFR (1-exp-ris, e.g., Pforr et al. 2012; Reddy et al. 2012), two exponential decreasing SFR laws with…”
Size evolution of normal and compact galaxies in the EAGLE simulation (2015, methodology): “We apply two colour cuts to the UVJ plane, that of VDW14 and that of Muzzin et al. (2013).”
The star formation activity of IllustrisTNG galaxies: main sequence, UVJ diagram, quenched fractions, and systematics (2018, background): “…a color-color based classification to distinguish between blue/star-forming and red/quenched galaxies (e.g. Wuyts et al. 2011; Williams et al. 2009, 2010; Whitaker et al. 2010; Patel et al. 2012; Quadri et al. 2012; Muzzin et al. 2013; Ilbert et al. 2013; Tomczak et al. 2014; Darvish et al. 2016).”
GOODS-HERSCHEL: STAR FORMATION, DUST ATTENUATION, AND THE FIR–RADIO CORRELATION ON THE MAIN SEQUENCE OF STAR-FORMING GALAXIES UP TO z ≃ 4 (2014, background): “…et al. 2009; Pérez-González et al. 2008; Pannella et al. 2009b; Bouwens et al. 2009; Ilbert et al. 2010; Hopkins & Beacom 2006; Karim et al. 2011; Muzzin et al. 2013; Ilbert et al. 2013; Burgarella et al. 2013; Madau & Dickinson 2014), we must now try to understand which are the main processes…”
The Herschel view of the dominant mode of galaxy growth from z = 4 to the present day (2014, methodology): “In COSMOS UltraVISTA, we follow the definition given by Muzzin et al. (2013b).”
A PUBLIC Ks-SELECTED CATALOG IN THE COSMOS/UltraVISTA FIELD: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND STELLAR POPULATION PARAMETERS, (2013, methodology): “In the left panel of Figure 6 we plot the zphot,UV ISTA vs. zphot,NMBS. Dark circles are for galaxies that are above the 95% mass-completeness limit of the survey at a given redshift (see Muzzin et al. 2013), and light symbols are for those below the 95% mass-completeness 10 limit.”
FORMING COMPACT MASSIVE GALAXIES (2015, result): “These numbers are consistent with previous measurements from other datasets (e.g., Marchesini et al. 2009; Brammer et al. 2011; Muzzin et al. 2013).”
THE MOSFIRE DEEP EVOLUTION FIELD (MOSDEF) SURVEY: REST-FRAME OPTICAL SPECTROSCOPY FOR ∼1500 H-SELECTED GALAXIES AT 1.37 ≤ z ≤ 3.8 ?> (2014, methodology): “Thus, this diagram is used to isolate quiescent from star-forming galaxies and classify galaxies out to z ∼ 4 (e.g., Muzzin et al. 2013a).”
Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, background): “Similarly, the progenitors of slow rotators change little in mass from z ∼ 2, while the the progenitors of fast rotators still grow significantly (Muzzin et al. 2013).”
Deriving Physical Properties from Broadband Photometry with Prospector: Description of the Model and a Demonstration of its Accuracy Using 129 Galaxies in the Local Universe (2016, background): “…to high redshift, both for the stellar mass function (e.g., Marchesini et al. 2009; Davidzon et al. 2013; Ilbert et al. 2013; Moustakas et al. 2013; Muzzin et al. 2013; Tomczak et al. 2014) and for the SFR– mass relationship (e.g., Brinchmann et al. 2004; Daddi et al. 2007; Noeske et al. 2007;…”
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.”
The KMOS Redshift One Spectroscopic Survey (KROSS):dynamical properties, gas and dark matter fractions of typical z~1 star-forming galaxies (2016, background): “3, with comparison to the value of the Schechter function M of the z = 0.5–1.0 star-forming galaxy mass function of Muzzin et al. (2013b).”
A SUBSTANTIAL POPULATION OF MASSIVE QUIESCENT GALAXIES AT z ∼ 4 FROM ZFOURGE (2013, methodology): “For comparison with other surveys, we integrated the COSMOS/UltraVISTA mass function at 3 < z < 4 for quiescent galaxies of Muzzin et al. (2013), based on a similar UVJ classification, to log10 M/M 10.6.”