The SWIRE-VVDS-CFHTLS surveys: stellar mass assembly over the last 10 Gyr. Evidence for a major build up of the red sequence between z = 2 and z = 1

By Stéphane Arnouts, C. Walcher, O. Fèvre, G. Zamorani, O. Ilbert, V. Brun, L. Pozzetti, Sandro Bardelli, L. Tresse, Elena Zucca and 36 more. 2007

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(abridged abstract) We present an analysis of the stellar mass growth over the last 10 Gyrs using a large 3.6$\mu$ selected sample. We split our sample into active (blue) and quiescent (red) galaxies. Our measurements of the K-LFs and LD evolution support the idea that a large fraction of galaxies is already assembled at $z\sim 1.2$. Based on the analysis of the evolution of the stellar mass-to-light ratio (in K-band) for the spectroscopic sub-sample, we derive the stellar mass density for the entire sample. We find that the global evolution of the stellar mass density is well reproduced by the star formation rate derived from UV dust corrected measurements. Over the last 8Gyrs, we observe that the stellar mass density of the active population remains approximately constant while it gradually increases for the quiescent population over the same timescale. As a consequence, the growth of the stellar mass in the quiescent population must be due to the shutoff of star formation in active galaxies that migrate into the quiescent population. From $z=2$ to $z=1.2$, we observe a major build-up of the quiescent population with an increase by a factor of 10 in stellar mass, suggesting that we are observing the epoch when an increasing fraction of galaxies are ending their star formation activity and start to build up the red sequence.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

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).”
THE STAR FORMATION HISTORY OF MASS-SELECTED GALAXIES IN THE COSMOS FIELD (2010, background): “Regarding the second point, the mass function of SF galaxies is commonly (e.g. Lilly et al. 1995; Bell et al. 2003, 2007; Zucca et al. 2006; Arnouts et al. 2007; Pozzetti et al. 2009; Ilbert et al. 2005, 2010) found to be well parametrized by a power law with an exponential cutoff at a…”
Mid- and far-infrared luminosity functions and galaxy evolution from multiwavelength Spitzer observations up to z ~ 2.5 (2009, methodology): “As in Arnouts et al. (2007), we used the flux measurements derived in 3 arcsec apertures for faint sources, while we adopted adaptive apertures (as for Kron magnitudes in Bertin & Arnouts 1996) for bright sources (mAB(3.6) < 19.5).”
COSMOS PHOTOMETRIC REDSHIFTS WITH 30-BANDS FOR 2-deg2 (2008, methodology): “…used to study the evolution of galaxy stellar masses and luminosities (e.g. Fontana et al. 2000; Wolf et al. 2003; Gabasch et al. 2004; Caputi et al. 2006; Arnouts et al. 2007), for angular clustering analysis (e.g. Heinis et al. 2007; McCracken et al. 2007), to study the relation between galaxy…”
THE NUMBER DENSITY AND MASS DENSITY OF STAR-FORMING AND QUIESCENT GALAXIES AT 0.4 ⩽ z ⩽ 2.2 (2011, background): “In particular, Arnouts et al. (2007) and Ilbert et al. (2010) find an increase of a factor of∼10 in the stellar mass density of quiescent galaxies betweenz= 2 andz= 1.2, which would imply very dramatic changes over a relatively short (≈ 2 Gyr) period.”
The evolution of stellar mass and the implied star formation history (2008, background): “The stellar mass estimates of Arnouts et al. (2007) are, however, significantly above the average of the compilation, as can be seen in Fig.”
GMASS ultradeep spectroscopy of galaxies at $z$ ~ 2 - II. Superdense passive galaxies: how did they form and evolve? (2008, background): “15–17) is further evidence that the redshift range of about 1< z < 2 is the critical cosmic epoch for the assembly and structural transformation of ETGs (e.g. Fontana et al. 2004, Glazebrook et al. 2004, Abraham et al. 2007, Arnouts et al. 2007).”
GALAXY STELLAR MASS ASSEMBLY BETWEEN 0.2 < z < 2 FROM THE S-COSMOS SURVEY (2009, methodology): “The stellar masses based on a Salpeter IMF (Arnouts et al. 2007), “diet” Salpeter IMF (Bell et al. 2008) and Kroupa IMF (Borch et al. 2006) were converted into a Chabrier IMF by adding -0.24 dex, -0.09 dex, and 0 dex, respectively, to the logarithm of the stellar masses.”
GOODS-Herschel: dust attenuation properties of UV selected high redshift galaxies (2012, methodology): “The K-band luminosity is transformed in stellar mass using the calibration of Arnouts et al. (2007) modified by Ilbert et al. (2010) and AFUV is deduced from log(LIR/LFUV) following Buat et al. (2011a).”
Multiwavelength Study of Massive Galaxies at z~2. I. Star Formation and Galaxy Growth (2007, methodology): “…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).”
A HIGHLY CONSISTENT FRAMEWORK FOR THE EVOLUTION OF THE STAR-FORMING “MAIN SEQUENCE” FROM z ∼ 0–6 (2014, methodology): “We correct these based on the results o Arnouts et al. (2007).”
WHAT TURNS GALAXIES OFF? THE DIFFERENT MORPHOLOGIES OF STAR-FORMING AND QUIESCENT GALAXIES SINCE z ∼ 2 FROM CANDELS (2011, background): “Broad trends One of the most notable trends seen by Arnouts et al. (2007), Taylor et al. (2009), Ilbert et al. (2010), Domínguez Sánchez et al. (2011), Brammer et al. (2011) and elaborated upon in Fig.”
GALAXY STELLAR MASS FUNCTIONS FROM ZFOURGE/CANDELS: AN EXCESS OF LOW-MASS GALAXIES SINCE z = 2 AND THE RAPID BUILDUP OF QUIESCENT GALAXIES (2013, background): “These results are consistent with previous works which have generally found that the star-forming SMF evolves relatively weakly with redshift (Arnouts et al. 2007; Bell et al. 2007; Pozzetti et al. 2010; Brammer et al. 2011; Muzzin et al. 2013).”
Post-starburst galaxies: more than just an interesting curiosity (2008, methodology): “The interpretation is that some blue galaxies migrate on to the red sequence after the quenching of their star formation, whilst the remainder continue to form new stars (e.g. Arnouts et al. 2007; Faber et al. 2007).”
EVOLUTION OF GALAXIES AND THEIR ENVIRONMENTS AT z = 0.1–3 IN COSMOS (2013, methodology): “As noted earlier, the correspondence between the rest-frame b-i color and the galaxy type is taken from Arnouts et al. (2007) and the stellar mass from the COSMOS photoz catalog was estimated using a color dependent mass-to-light ratio (see Ilbert et al. 2009).”
STELLAR AND TOTAL BARYON MASS FRACTIONS IN GROUPS AND CLUSTERS SINCE REDSHIFT 1 (2009, methodology): “In our case we use M/L values that correspond to the individual star formation histories of individual member galaxies (Arnouts et al. 2007) and we do not make assumption on the M/L of the ICL.”
The VIMOS Ultra-Deep Survey: ~10 000 galaxies with spectroscopic redshifts to study galaxy assembly at early epochs 2 < z ≃ 6 (2014, background): “2012, Madau & Dickinson 2014), and the history of stellar mass assembly (e.g. Arnouts et al. 2007, Ilbert et al. 2013).”