The evolution of quiescent galaxies at high redshifts (z≥ 1.4)

Sánchez, H. Domínguez; Pozzi, F.; Gruppioni, C.; Cimatti, A.; Ilbert, O.; Pozzetti, L.; McCracken, H. J.; Capak, P.; Floc’h, E. Le; Salvato, M.; Zamorani, G.; Carollo, C. M.; Contini, T.; Kneib, Jean-Paul; Fèvre, O. Le; Lilly, S. J.; Mainieri, V.; Renzini, A.; Scodeggio, M.; Bardelli, S.; Bolzonella, M.; Bongiorno, A.; Caputi, K.; Coppa, G.; Cucciati, O.; Torre, S. de la; Ravel, L. de; Franzetti, P.; Garilli, B.; Iovino, A.; Kampczyk, P.; Knobel, C.; Kovač, K.; Lamareille, F.; Borgne, J. F. Le; Brun, V. Le; Maier, C.; Mignoli, M.; Pelló, R.; Peng, Yingjie; Pérez-Montero, E.; Ricciardelli, E.; Silverman, John D.; Tanaka, Masayuki; Tasca, L.; Tresse, L.; Vergani, D.; Zucca, E.

doi:10.1111/j.1365-2966.2011.19263.x

Cited by 56 publications

(9 citation statements)

References 81 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This indicates that SF quenching (to local quiescent galaxy level) is faster for more massive galaxies. This fast increase of quiescent fraction at high-z agrees with the result of Domínguez Sánchez et al (2011).…”

supporting

confidence: 81%

EVOLUTION OF STAR FORMATION PROPERTIES OF HIGH-REDSHIFT CLUSTER GALAXIES SINCEz= 2

Lee

Kim

et al. 2015

ApJ

View full text Add to dashboard Cite

Using a stellar mass-limited sample of ∼46,600 galaxies (M M 10 9.1 * >  ) at z 0.5 2 < < , we show that the stellar mass, rather than the environment, is the main parameter controlling quenching of star formation in galaxies with M M 10 10 * >  out to z = 2. On the other hand, the environmental quenching becomes efficient at z 1 < regardless of galaxy mass, and it serves as a main mechanismfor quenching star formation for lower mass galaxies. Our result is based on deep optical and near-infrared imaging data over 2800 arcmin 2 , enabling us to negate cosmic variance and identify 46 galaxy cluster candidates with M M 10 14  . From M 10 9.5 *~t o M 10 10.5  , the fraction of quiescent galaxies increases by a factor of ∼10 over the entire redshift range, but the difference between cluster and field environment is negligible. Rapid evolution in the quiescent fraction is seen from z = 2 to z = 1.3 for massive galaxies, suggesting a build-up of massive quiescent galaxies at z 1.3 > . For galaxies with M M 10 10 * <  at z 1.0 < , the quiescent fraction is found to be as much as a factor of 2 larger in clusters than in field, showing the importance of environmental quenching in low-mass galaxies at low redshift. Most high-mass galaxies are already quenched at z 1 > , therefore environmental quenching does not play a significant role for them, although the efficiency of environmental quenching is nearly identical between high-and low-mass galaxies.

show abstract

supporting

confidence: 81%

EVOLUTION OF STAR FORMATION PROPERTIES OF HIGH-REDSHIFT CLUSTER GALAXIES SINCEz= 2

Lee

Kim

et al. 2015

ApJ

View full text Add to dashboard Cite

show abstract

“…The set of observables used for the calibration process is the stellar mass functions (SMF) at z = 0 and z = 2, the star formation rate distribution function (SFRF), the fraction of mass in cold gas as a function of stellar mass (CGMF) and the relation between bulge mass and the mass of the central supermassive BH (BHB). For the SMFs, we adopt the compilation data used by Henriques et al (2015), which for z = 0 is a combination of the SMF of the SDSS from Baldry et al (2008) and Li & White (2009), and of the Galaxy And Mass Assembly (GAMA) from Baldry et al (2012), while for z = 2 is a combination of the data of the Cosmic Evolution Survey (COSMOS) from Domínguez Sánchez et al (2011), the Ultra Deep Survey (UltraVISTA) from Muzzin et al (2013) and Ilbert et al (2013), and the FourStar Galaxy Evolution Survey (ZFOURGE) from Tomczak et al (2014). For the SFRF, which is the number density of galaxies in a certain SFR interval, we use data from a flux-limited sample of galaxies observed with the Herschel satellite which gives the total (IR+UV) instantaneous SFR for the redshift interval z ∈ [0.0, 0.3], as presented in Gruppioni et al (2015).…”

Section: Calibration Processmentioning

confidence: 99%

Semi-analytic galaxies – I. Synthesis of environmental and star-forming regulation mechanisms

Cora

Vega-Martínez

Hough

et al. 2018

Monthly Notices of the Royal Astronomical Society

132

153

View full text Add to dashboard Cite

We present results from the semi-analytic model of galaxy formation sag applied on the MultiDark simulation MDPL2. sag features an updated supernova (SN) feedback scheme and a robust modelling of the environmental effects on satellite galaxies. This incorporates a gradual starvation of the hot gas halo driven by the action of ram pressure stripping (RPS), that can affect the cold gas disc, and tidal stripping (TS), which can act on all baryonic components. Galaxy orbits of orphan satellites are integrated providing adequate positions and velocities for the estimation of RPS and TS. The star formation history and stellar mass assembly of galaxies are sensitive to the redshift dependence implemented in the SN feedback model. We discuss a variant of our model that allows to reconcile the predicted star formation rate density at z 3 with the observed one, at the expense of an excess in the faint end of the stellar mass function at z = 2. The fractions of passive galaxies as a function of stellar mass, halo mass and the halo-centric distances are consistent with observational measurements. The model also reproduces the evolution of the main sequence of star forming central and satellite galaxies. The similarity between them is a result of the gradual starvation of the hot gas halo suffered by satellites, in which RPS plays a dominant role. RPS of the cold gas does not affect the fraction of quenched satellites but it contributes to reach the right atomic hydrogen gas content for more massive satellites (M 10 10 M ).

show abstract

“…The inverse of the sSFR defines the time required for a galaxy to form its stellar mass at the current star formation rate, therefore this parameter is a relatively straightforward indicator of star formation activity or quiescence. The threshold sSFR to separate between actively star-forming and quiescent objects varies with studies and it ranges between 10 −10 yr −1 and 10 −11 yr −1 (Domínguez Sánchez et al 2011;Bruce et al 2012;Ibar et al 2013;McLure et al 2013;Domínguez Sánchez et al 2016;Oemler et al 2017), implying that a galaxy will double its stellar mass in a timescale τ = sSFR −1 comparable or greater than the age of the Universe.…”

Section: Evolution Of Specific Star Formation Ratesmentioning

confidence: 99%

Bulgeless galaxies in the COSMOS field: environment and star formation evolution at z < 1

Grossi

Fernandes

Sobral

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Combining the catalogue of galaxy morphologies in the COSMOS field and the sample of Hα emitters at redshifts z = 0.4 and z = 0.84 of the HiZELS survey, we selected ∼ 220 star-forming bulgeless systems (Sérsic index n ≤ 1.5) at both epochs. We present their star formation properties and we investigate their contribution to the star formation rate function (SFRF) and global star formation rate density (SFRD) at z < 1. For comparison, we also analyse Hα emitters with more structurally evolved morphologies that we split into two classes according to their Sérsic index n: intermediate (1.5 < n ≤ 3) and bulge-dominated (n > 3). At both redshifts the SFRF is dominated by the contribution of bulgeless galaxies and we show that they account for more than 60% of the cosmic SFRD at z < 1. The decrease of the SFRD with redshift is common to the three morphological types but it is stronger for bulge-dominated systems. Starforming bulgeless systems are mostly located in regions of low to intermediate galaxy densities (Σ ∼ 1 − 4 Mpc −2 ) typical of field-like and filament-like environments and their specific star formation rates (sSFRs) do not appear to vary strongly with local galaxy density. Only few bulgeless galaxies in our sample have high (sSFR > 10 −9 yr −1 ) and these are mainly low-mass systems. Above M * ∼ 10 10 M ⊙ bulgeless are evolving at a "normal" rate (10 −9 yr −1 < sSFR <10 −10 yr −1 ) and in the absence of an external trigger (i.e. mergers/strong interactions) they might not be able to develop a central classical bulge.

show abstract

The evolution of quiescent galaxies at high redshifts (z≥ 1.4)

Abstract: International audienceno abstrac

Cited by 56 publications

References 81 publications

EVOLUTION OF STAR FORMATION PROPERTIES OF HIGH-REDSHIFT CLUSTER GALAXIES SINCEz= 2

EVOLUTION OF STAR FORMATION PROPERTIES OF HIGH-REDSHIFT CLUSTER GALAXIES SINCEz= 2

Semi-analytic galaxies – I. Synthesis of environmental and star-forming regulation mechanisms

Bulgeless galaxies in the COSMOS field: environment and star formation evolution at z < 1

Contact Info

Product

Resources

About