Dependence of galaxy quenching on halo mass and distance from its centre

By J. Woo, A. Dekel, S. Faber, K. Noeske, D. Koo, B. Gerke, M. Cooper, S. Salim, A. Dutton, J. Newman and 5 more. 2012

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We study the dependence of star-formation quenching on galaxy mass and environment, in the SDSS (z~0.1) and the AEGIS (z~1). It is crucial that we define quenching by low star-formation rate rather than by red colour, given that one third of the red galaxies are star forming. We address stellar mass M*, halo mass Mh, density over the nearest N neighbours deltaN, and distance to the halo centre D. The fraction of quenched galaxies appears more strongly correlated with Mh at fixed M* than with M* at fixed Mh, while for satellites quenching also depends on D. We present the M*-Mh relation for centrals at z~1. At z~1, the dependence of quenching on M* at fixed Mh is somewhat more pronounced than at z~0, but the quenched fraction is low (10%) and the haloes are less massive. For satellites, M*-dependent quenching is noticeable at high D, suggesting a quenching dependence on sub-halo mass for recently captured satellites. At small D, where satellites likely fell in more than a few Gyr ago, quenching strongly depends on Mh, and not on M*. The Mh-dependence of quenching is consistent with theoretical wisdom where virial shock heating in massive haloes shuts down accretion and triggers ram-pressure stripping, causing quenching. The interpretation of deltaN is complicated by the fact that it depends on the number of observed group members compared to N, motivating the use of D as a better measure of local environment.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/af2047734449eee2baf2146bd9b8a2e2014db5ae

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Citations in the corpus

Compaction and quenching of high-z galaxies in cosmological simulations: blue and red nuggets (2014, background): “However, observations indicate that compactness is a necessary, but not sufficient, condition for quenching (Cheung et al. 2012; Fang et al. 2013; Barro et al. 2013; Dekel & Burkert 2014; Woo et al. 2013, 2014).”
Physical Models of Galaxy Formation in a Cosmological Framework (2014, background): “A number of studies have shown that the probability for a galaxy to be quiescent depends on both its stellar mass and large-scale environment or halo mass (Balogh et al. 2004, Hogg et al. 2004, Peng et al. 2010, Woo et al. 2013).”
Introducing the Illustris Project: simulating the coevolution of dark and visible matter in the Universe (2014, result): “Towards lower and higher masses, SF becomes less efficient and the fraction of red galaxies increases in both directions due to quenching, which is consistent with observations (Woo et al. 2013).”
LoCuSS: THE SLOW QUENCHING OF STAR FORMATION IN CLUSTER GALAXIES AND THE NEED FOR PRE-PROCESSING (2015, background): “The fraction of star-forming galaxies within groups declines steadily with increasing group mass (at fixed stellar mass and group-centric distance) and proximity to the group center (Weinmann et al. 2006; Wetzel et al. 2012; Woo et al. 2013).”
The GALEX Arecibo SDSS Survey - VIII. Final data release. The effect of group environment on the gas content of massive galaxies (2013, methodology): “We use the latter for our environmental analysis, and adopt halo masses Mh obtained by rank ordering the groups by stellar mass, following e.g. Woo et al. (2013).”
Bulge mass is king: the dominant role of the bulge in determining the fraction of passive galaxies in the Sloan Digital Sky Survey (2014, methodology): “If we restrict our investigation to halo mass, stellar mass and δ5 (as in Woo et al. 2013) for central galaxies, i.e. disregarding our bulge + disk decompositions and hence bulge mass, disk mass, and B/T, we recover an equivalent result.”
Selection bias in dynamically measured supermassive black hole samples: its consequences and the quest for the most fundamental relation (2016, background): “There are a number of hypotheses (not necessarily mutual exclusive) put forward in the literature to explain the quenching of star formation in galaxies (e.g., Woo et al. 2013).”
A LINK BETWEEN STAR FORMATION QUENCHING AND INNER STELLAR MASS DENSITY IN SLOAN DIGITAL SKY SURVEY CENTRAL GALAXIES (2013, methodology): “C O ] 2 3 A ug 2 01 3 retical predictions and observational evidence both indicate a large scatter in the critical halo mass of at least∼ 1 dex (Kereš et al. 2005; Dekel & Birnboim 2006; Woo et al. 2013).”
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).”
ELVIS: Exploring the Local Volume in Simulations (2013, background): “If so, then in principle, environmental effects such as ram pressure, harassment, or strangulation could have quenched the galaxy it hosts (Kawata & Mulchaey 2008; Boselli et al. 2008; Grcevich & Putman 2009; Woo et al. 2013; Phillips et al. 2014).”
Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies (2015, background): “…the shape and evolution of the mass function of star-forming galaxies (SFGs) and quiescent galaxies since z ∼ 4, cementing our understanding of galaxy build up and shutdown (Peng et al. 2010; Brammer et al. 2011; Ilbert et al. 2013; Muzzin et al. 2013; Woo et al. 2013; Tomczak et al. 2013).”
BULGE GROWTH AND QUENCHING SINCE z = 2.5 IN CANDELS/3D-HST (2014, methodology): “…galaxies over cosmic time using large surveys such as SDSS, NMBS, zCOSMOS, UltraVISTA and zFOURGE showed that the probability for a galaxy being quenched increases with its mass (Peng et al. 2010; Brammer et al. 2011; Ilbert et al. 2013; Muzzin et al. 2013; Woo et al. 2013; Tomczak et al. 2014).”