The correlation of star formation quenching with internal galaxy properties and environment

Kimm, Taysun; Somerville, Rachel S.; Yi, Sukyoung K.; Bosch, Frank C. van den; Salim, Samir; Fontanot, Fabio; Monaco, Pierluigi; Mo, H. J.; Pasquali, A.; Rich, R. Michael; Yang, Xiaohu

doi:10.1111/j.1365-2966.2009.14414.x

Cited by 185 publications

(246 citation statements)

References 124 publications

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“…Many studies based on semi-analytic models have shown that bulge-dominated galaxies in massive halos tend to be red and quiescent (Bower et al 2006;Croton et al 2006;Somerville et al 2008;Kimm et al 2009;Lang et al 2014), in general qualitative agreement with our results. As shown by e.g.…”

Section: Comparison With Other Theoretical Studiessupporting

confidence: 92%

The relationship between star formation activity and galaxy structural properties in CANDELS and a semi-analytic model

Brennan

Pandya

Somerville

et al. 2016

Mon. Not. R. Astron. Soc.

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We study the correlation of galaxy structural properties with their location relative to the SFR-M * correlation, also known as the star formation "main sequence" (SFMS), in the CANDELS and GAMA surveys and in a semi-analytic model (SAM) of galaxy formation. We first study the distribution of median Sérsic index, effective radius, star formation rate (SFR) density and stellar mass density in the SFR-M * plane. We then define a redshift dependent main sequence and examine the medians of these quantities as a function of distance from this main sequence, both above (higher SFRs) and below (lower SFRs). Finally, we examine the distributions of distance from the main sequence in bins of these quantities. We find strong correlations between all of these galaxy structural properties and the distance from the SFMS, such that as we move from galaxies above the SFMS to those below it, we see a nearly monotonic trend towards higher median Sérsic index, smaller radius, lower SFR density, and higher stellar density. In the semi-analytic model, bulge growth is driven by mergers and disk instabilities, and is accompanied by the growth of a supermassive black hole which can regulate or quench star formation via Active Galactic Nucleus (AGN) feedback. We find that our model qualitatively reproduces the trends described above, supporting a picture in which black holes and bulges co-evolve, and AGN feedback plays a critical role in moving galaxies off of the SFMS.

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Section: Comparison With Other Theoretical Studiessupporting

confidence: 92%

The relationship between star formation activity and galaxy structural properties in CANDELS and a semi-analytic model

Brennan

Pandya

Somerville

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Comparing the observations to the results of Kimm et al (2009) (not shown in Fig. 2), our observed, quiescent fractions at galaxy masses below log(M stellar /M⊙) < 10 are somewhat lower than theirs, particularly for satellite galaxies.…”

Section: The Stellar Mass Dependence Of Quiescent Galaxiessupporting

confidence: 72%

“…2), our observed, quiescent fractions at galaxy masses below log(M stellar /M⊙) < 10 are somewhat lower than theirs, particularly for satellite galaxies. Kimm et al (2009) use the Yang catalogue based on the SDSS data similar to our analysis, adopt the same magnitude cut and perform a completeness correction. However, they use SFR estimates based on full SED modelling, while Brinchmann et al (2004) -as used in our analysis -have estimated the SFR via emission lines.…”

Section: The Stellar Mass Dependence Of Quiescent Galaxiesmentioning

confidence: 99%

“…The effect of environmental processes has been theoretically studied by using semi-empirical models (Wetzel et al 2012), numerical simulations (see De Lucia 2011 for a review) and semi-analytic models (De Lucia & Blaizot 2007;Font et al 2008;Kimm et al 2009;Weinmann et al 2010;Guo et al 2011). Most of the currently used galaxy formation models do not explicitly include environmental processes beyond the virial radius of haloes.…”

Section: Introductionmentioning

confidence: 99%

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The influence of the environmental history on quenching star formation in a Λ cold dark matter universe

Hirschmann¹,

Lucia²,

Wilman³

et al. 2014

Monthly Notices of the Royal Astronomical Society

113

145

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We present a detailed analysis of the influence of the environment and of the environmental history on quenching star formation in central and satellite galaxies in the local Universe. We take advantage of publicly available galaxy catalogues obtained from applying a galaxy formation model to the Millennium simulation. In addition to halo mass, we consider the local density of galaxies within various fixed scales. Comparing our model predictions to observational data (SDSS), we demonstrate that the models are failing to reproduce the observed density dependence of the quiescent galaxy fraction in several aspects: for most of the stellar mass ranges and densities explored, models cannot reproduce the observed similar behaviour of centrals and satellites, they slightly under-estimate the quiescent fraction of centrals and significantly overestimate that of satellites. We show that in the models, the density dependence of the quiescent central galaxies is caused by a fraction of "backsplash" centrals which have been satellites in the past. The observed stronger density dependence on scales of 0.2 − 1 Mpc may, however, indicate additional environmental processes working on central galaxies. Turning to satellite galaxies, the density dependence of their quiescent fractions reflects a dependence on the time spent orbiting within a parent halo, correlating strongly with halo mass and distance from the halo centre. Comparisons with observational estimates suggest relatively long gas consumption time scales of roughly 5 Gyr in low mass satellite galaxies. The quenching time scales decrease with increasing satellite stellar mass. Overall, a change in modelling both internal processes and environmental processes is required for improving currently used galaxy formation models.

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“…Kimm et al 2009;Kimm, Yi & Khochfar 2011;Wang et al 2014;Hirschmann et al 2014;Phillips et al 2015). While satellites are rapidly quenched -following infall -in the models, analysis of satellite populations identified in the Sloan Digital Sky Survey (SDSS, York et al 2000) instead find that quenching proceeds remarkably slowly, such that a typical e-mail: sfilling@uci.edu † e-mail: cooper@uci.edu ‡ Einstein fellow satellite with M 10 8 M orbits within its host halocontinuing to form stars -for ∼ 3 − 7 Gyr before being quenched (De Lucia et al 2012;Wetzel et al 2013;Wheeler et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Under pressure: quenching star formation in low-mass satellite galaxies via stripping

Fillingham

Cooper

Pace

et al. 2016

Mon. Not. R. Astron. Soc.

119

123

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Recent studies of galaxies in the local Universe, including those in the Local Group, find that the efficiency of environmental (or satellite) quenching increases dramatically at satellite stellar masses below ∼ 10 8 M . This suggest a physical scale where quenching transitions from a slow "starvation" mode to a rapid "stripping" mode at low masses. We investigate the plausibility of this scenario using observed HI surface density profiles for a sample of 66 nearby galaxies as inputs to analytic calculations of ram-pressure and turbulent viscous stripping. Across a broad range of host properties, we find that stripping becomes increasingly effective at M * 10 8−9 M , reproducing the critical mass scale observed. However, for canonical values of the circumgalactic medium density (n halo < 10 −3.5 cm −3 ), we find that stripping is not fully effective; infalling satellites are, on average, stripped of only 40 − 60% of their cold gas reservoir, which is insufficient to match observations. By including a host halo gas distribution that is clumpy and therefore contains regions of higher density, we are able to reproduce the observed HI gas fractions (and thus the high quenched fraction and short quenching timescale) of Local Group satellites, suggesting that a host halo with clumpy gas may be crucial for quenching low-mass systems in Local Group-like (and more massive) host halos.

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The correlation of star formation quenching with internal galaxy properties and environment

Cited by 185 publications

References 124 publications

The relationship between star formation activity and galaxy structural properties in CANDELS and a semi-analytic model

The relationship between star formation activity and galaxy structural properties in CANDELS and a semi-analytic model

The influence of the environmental history on quenching star formation in a Λ cold dark matter universe

Under pressure: quenching star formation in low-mass satellite galaxies via stripping

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