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

By T. Kimm, R. Somerville, S. Yi, F. V. D. Bosch, S. Salim, F. Fontanot, P. Monaco, H. Mo, A. Pasquali, R. Rich and 1 more. 2008

157 citations recorded by the source corpus.

We investigate the correlation of star formation quenching with internal galaxy properties and large-scale environment (halo mass) in empirical data and theoretical models. We make use of the halo-based group catalogue of Yang and collaborators, which is based on the Sloan Digital Sky Survey. Data from the Galaxy evolution explorer are also used to extract the recent star formation rate. In order to investigate the environmental effects, we examine the properties of 'central' and 'satellite' galaxies separately. For central galaxies, we are unable to conclude whether star formation quenching is primarily connected with halo mass or stellar mass, because these two quantities are themselves strongly correlated. For satellite galaxies, a nearly equally strong dependence on halo mass and stellar mass is seen. We make the same comparison for five different semi-analytic models based on three independently developed codes. We find that the models with active galactic nuclei feedback reproduce reasonably well the dependence of the fraction of central red and passive galaxies on halo mass and stellar mass. However, for satellite galaxies, the same models badly overproduce the fraction of red/passive galaxies and do not reproduce the empirical trends with stellar mass or halo mass. This satellite overquenching problem is caused by the too-rapid stripping of the satellites' hot gas haloes, which leads to rapid strangulation of star formation.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/bdf2ef4113db7c7c19e883c816dc98880abbe52f

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In Astronomy and Astrophysics

1. P. Hopkins
2. R. Somerville
3. L. Hernquist
4. R. Dav'e
5. C. Conroy
6. A. Dekel
7. Volker Springel
8. Simon D. M. White

In Instrumentation

1. P. Hopkins
2. R. Somerville
3. L. Hernquist
4. R. Dav'e
5. C. Conroy
6. A. Dekel
7. Joel R. Primack
8. F. V. D. Bosch

Citations in the corpus

• Cold gas stripping in satellite galaxies: from pairs to clusters (2016, background): “…is that satellites infalling into the halo have undergone a distinct evolutionary history from that of their central, as well as being the bulk of the group and cluster populations (e.g. van den Bosch et al. 2008; Kimm et al. 2009; Peng et al. 2012; Wetzel, Tinker & Conroy 2012; Woo et al. 2013).”
• Are Brightest Halo Galaxies Central Galaxies (2010, background): “…galaxy group catalogues to split the galaxy population into centrals and satellites, and to compare their properties (e.g., Weinmann et al. 2006, 2009; Skibba et al. 2007; van den Bosch et al. 2008; Pasquali et al. 2009, 2010; Hansen et al. 2009; Kimm et al. 2009; Skibba 2009; Guo et al. 2009).”
• The environmental history of group and cluster galaxies in a Λ cold dark matter universe (2011, methodology): “The results obtained are in good agreement with those presented in Kimm et al. (2009).”
• A STELLAR MASS THRESHOLD FOR QUENCHING OF FIELD GALAXIES (2012, background): “Currently favored models suggest that massive galaxies are quenched because they can maintain a hot gaseous halo, due to processes such as heating from supernova or active galactic nuclei (e.g., Croton et al. 2006; Dekel & Birnboim 2008; Kimm 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, background): “…environment, AGN content, and dark-matter halo mass are critical for determining galaxy quenching, and the evolution of galaxy bimodality (e.g., Weinmann et al. 2006; Bell et al. 2007; Kimm et al. 2009; Peng et al. 2010; Wetzel et al. 2012; Woo et al. 2012; Aird et al. 2012; Knobel et al. 2012).”
• Tracking the impact of environment on the galaxy stellar mass function up to z ~ 1 in the 10 k zCOSMOS sample (2009, background): “…a too efficient strangulation produces an instantaneous shut down of the star formation when a galaxy enters in a halo (see Weinmann et al. 2006; Font et al. 2008; Kang & van den Bosch 2008; Kimm et al. 2009; Fontanot et al. 2009, for a description of the issue and some attempts to solve it).”
• Evolution of density profiles in high-z galaxies: compaction and quenching inside-out (2015, background): “There is solid observational evidence that the shut-down of star formation in galaxies is correlated with both galaxy mass and environment (e.g., Dressler 1980; Balogh et al. 2004; Baldry et al. 2006; Kimm et al. 2009).”
• DWARF GALAXIES WITH OPTICAL SIGNATURES OF ACTIVE MASSIVE BLACK HOLES (2013, background): “For instance, while BH feedback is often invoked to explain star formation quenching in massive galaxies (e.g., Croton et al. 2006; Kimm et al. 2009), the quenched fraction of central galaxies decreases with stellar mass (Wetzel et al. 2012) and may become zero below a stellar mass near 109 M…”
• MASS AND ENVIRONMENT AS DRIVERS OF GALAXY EVOLUTION. II. THE QUENCHING OF SATELLITE GALAXIES AS THE ORIGIN OF ENVIRONMENTAL EFFECTS (2011, background): “…recent observational analyses have therefore distinguished between satellites and centrals (e.g. Weinmann et al. 2006 & 2009; von der Linden et al. 2007; van den Bosch et al. 2008a & 2008b; Yang et al. 2009a & 2009b; Pasquali et al. 2009 & 2010; Skibba 2009; Hansen et al. 2009; Kimm et al. 2009).”
• Physical Models of Galaxy Formation in a Cosmological Framework (2014, methodology): “…observed bimodality of the color and sSFR distribution and the fraction of quiescent galaxies as a function of stellar mass (Bower et al. 2006, Croton et al. 2006, Kimm et al. 2009, Somerville et al. 2008); certainly, including AGN feedback greatly improved the results relative to the old models.”
• Galaxy evolution in groups and clusters: star formation rates, red sequence fractions and the persistent bimodality (2011, methodology): “…with halo mass which nearly equals the intrinsic dependence on galaxy mass (Weinmann et al. 2006; Blanton & Berlind 2007; Hansen et al. 2009; Kimm et al. 2009), as well as satellites being more likely to be quenched at smaller radii (Weinmann et al. 2006; Blanton & Berlind 2007; Hansen et…”
• Star formation in semi-analytic galaxy formation models with multiphase gas (2015, background): “However, the evolution of the number of massive “quenched” galaxies in models with AGN feedback seems to match observations reasonably well (Kimm et al. 2009; Brennan et al. 2015).”
• Dependence of galaxy quenching on halo mass and distance from its centre (2012, methodology): “As discussed in §5.3, our results are consistent with those of previous work (eg., Weinmann et al. 2006a; Blanton & Roweis 2007; Hansen et al. 2009; Kimm et al. 2009; Wetzel et al. 2012a).”
• Galaxy evolution in cosmological simulations with outflows ― I. Stellar masses and star formation rates (2011, background): “…or not; the observed galaxies may simply have lower specific SFRs. Interestingly, a recent semianalytic model that is more successful than our simulations at matching a wider range of data still suffers from the same discrepancy, showing an upturn in red fraction at low masses (Kimm et al. 2009).”
• MERGERS IN ΛCDM: UNCERTAINTIES IN THEORETICAL PREDICTIONS AND INTERPRETATIONS OF THE MERGER RATE (2010, methodology): “0.01−0.05 in these environments (specifically see e.g. Haines et al. 2007; Weinmann et al. 2009a; Kimm et al. 2009), and then only in the final stages and/or close passages, not just at the moment of crossingRvir (references above and Yang et al. 2009; van den Bosch et al. 2008; Kang & van den…”
• Galaxy evolution in groups and clusters: satellite star formation histories and quenching time-scales in a hierarchical Universe (2012, background): “…et al. 2001; De Propris et al. 2004; Weinmann et al. 2006; Blanton & Berlind 2007; Kimm et al. 2009; van den Bosch et al. 2008; Hansen et al. 2009; Kimm et al. 2009; Pasquali et al. 2009; von der Linden et al. 2010; Prescott et al. 2011; Peng et al. 2012; Wetzel et al. 2012; Woo et al. 2013).”