The spatial and kinematic distributions of cluster galaxies in a ΩCDM universe: comparison with observations

By A. Diaferio, G. Kauffmann, M. Balogh, Simon D. M. White, D. Schade, E. Ellingson. 2000

155 citations recorded by the source corpus.

We combine dissipationless N-body simulations and semi-analytic models of galaxy formation to study the spatial and kinematic distributions of cluster galaxies in a ΛCDM cosmology. We investigate how the star formation rates (SFRs), colours and morphologies of galaxies vary as a function of distance from the cluster centre, and compare our results with the CNOC1 survey of galaxies from 15 X-ray-luminous clusters in the redshift range 0.18<z<0.55. In our model, gas no longer cools on to galaxies after they fall into the cluster and, as a result, their SFRs decline on time-scales of ∼1–2 Gyr. Galaxies in cluster cores have lower SFRs and redder colours than galaxies in the outer regions, because they were accreted earlier. Our colour and star formation gradients agree with those derived from the data. The difference in velocity dispersions between red and blue galaxies observed in the CNOC1 clusters is also well reproduced by the model. We assume that the morphologies of cluster galaxies are determined solely by their merging histories. A merger between two equal-mass galaxies produces a bulge, and subsequent cooling of gas results in the formation of a new disc. Morphology gradients in clusters arise naturally, with the fraction of bulge-dominated galaxies highest in cluster cores. The fraction of bulge-dominated galaxies inside the virial radius depends on the mass of the cluster, but is independent of redshift for clusters of fixed mass. Galaxy colours and SFRs do not depend on cluster mass. We compare the distributions of galaxies in our simulations as a function of bulge-to-disc ratio, and as a function of projected clustercentric radius, with those derived from the CNOC1 sample. We find excellent agreement for bulge-dominated galaxies. The simulated clusters contain too few galaxies of intermediate bulge-to-disc ratios, suggesting that additional processes may influence the morphological evolution of disc-dominated galaxies in clusters. Although the properties of the cluster galaxies in our model agree extremely well with the data, the same is not true of field galaxies. Both the SFRs and the colours of bright field galaxies appear to evolve much more strongly from redshift 0.2 to 0.4 in the CNOC1 field sample than in our simulations.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

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Citations in the corpus

A Wide-Field Hubble Space Telescope Study of the Cluster Cl 0024+16 at z = 0.4. I. Morphological Distributions to 5 Mpc Radius (2003, background): “…that clusters evolve continuously by merging and accreting structures from the surrounding field (e.g., Zabludoff & Franx 1993; Abraham et al. 1996a; Balogh, Navarro, & Morris 2000), as described in popular theories of structure formation (e.g., Kauffmann 1995a, 1995b; Diaferio et al. 2001).”
The formation history of elliptical galaxies (2005, background): “This implies that the cluster– centric distance of the galaxies is correlated with the time they were accreted onto a larger structure (Diaferio et al. 2001; Gao et al. 2004).”
The SAURON project - IV. The mass-to-light ratio, the virial mass estimator and the Fundamental Plane of elliptical and lenticular galaxies (2005, background): “Hierarchical galaxy formation scenarios (Diaferio et al. 2001) predict that the galaxies in the field should have a significantlylower M/L than the galaxies in clusters, nearly independently of redshift.”
What determines satellite galaxy disruption (2009, methodology): “Better agreement with observations has been found using semi-analytic models of star formation applied to subhalo catalogs (Springel et al. 2001; Diaferio et al. 2001), which correlate stellar mass to a subhalo’s mass at the time the stellar component was assembled (before infall), thus indicating…”
Mass-to-Light Ratios of Field Early-Type Galaxies at z ~ 1 from Ultradeep Spectroscopy: Evidence for Mass-dependent Evolution (2005, background): “In fact, in the hierarchical picture the formation redshift of galaxies with a given mass depends on environment (Diaferio et al. 2001).”
LoCuSS: THE SLOW QUENCHING OF STAR FORMATION IN CLUSTER GALAXIES AND THE NEED FOR PRE-PROCESSING (2015, result): “This approach gained early support when Balogh et al. (2000), Diaferio et al. (2001), and Ellingson et al. (2001) were able to reproduce the observed radial population gradients of star-forming galaxies in clusters in terms of galaxies on their first infall into the cluster.”
Galaxy ecology: groups and low-density environments in the SDSS and 2dFGRS (2003, background): “Thus, star formation will gradually decline in any galaxy which is part of a larger halo (Balogh et al. 2000; Diaferio et al. 2001); groups will be the first environment to demonstrate this effect.”
The 2dF Galaxy Redshift Survey: The environmental dependence of galaxy star formation rates near clusters (2002, background): “These models are able to reproduce radial gradients c© 0000 RAS, MNRAS 000, 000–000 in star formation within the virial radius of clusters to a remarkably high degree of accuracy (Diaferio et al. 2001; Okamoto & Nagashima 2001).”
Measurement of Galaxy Cluster Sizes, Radial Profiles, and Luminosity Functions from SDSS Photometric Data (2004, background): “…of 180 times the mean background (e.g. Jenkins et al. 2001; Kravtsov et al. 2004), 200 times the critical density, i.e. 200Ω−1M times the mean background (e.g. Diaferio et al. 2001; Evrard et al. 2002; Kochanek et al. 2003), to the “virial mass” (Eke, Cole, & Frenk 1996; Bullock et al. 2001).”
The Build-up of the Colour-Magnitude Relation (2005, background): “Strangulation (which is often referred to as suffocation, starvation or halo gas stripping) is considered to be effective both in groups and clusters (Larson, Tinsley & Caldwell 1980; Balogh, Navarro & Morris 2000; Diaferio et al. 2001; Okamoto & Nagashima 2003).”
The Dependence on Environment of the Color-Magnitude Relation of Galaxies (2003, background): “…Royal Observatory, University of Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK. bulge-dominated than those in typical density regions (e.g., Cen & Ostriker 1993; Kauffmann, White, & Guiderdoni 1993; Kauffmann, Colberg, & Diaferio 1999; Kauffmann 1996; Benson et al. 2000; Diaferio et al. 2001).”
Pre-Processing of Galaxies before Entering a Cluster (2003, background): “However, major mergers alone cannot account for the observed fractions of galaxies with intermediate bulge-to-disk luminosity ratios such as S0 galaxies in clusters (Okamoto, Nagashima 2001; Diaferio et al. 2001).”
THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS (2007, methodology): “For example, the model presented by Diaferio et al. (2001) predicts: that the mean satellite color gets bluer as a function of cluster-centric distance until reaching a plateau at the field value around 2–3r200; that the mean satellite color depends on halo mass only for M <∼ 5×1013h−1M⊙; and that…”
The Assembly History of Field Spheroidals: Evolution of Mass-to-Light Ratios and Signatures of Recent Star Formation (2005, unknown): “Although the difference between the FP evolution of cluster and field spheroidals (Table 2) is in the sense expected by hierarchical models (Diaferio et al. 2001; De Lucia et al. 2004), quantitatively it is not as pronounced as expected (vanDokkum et al. 2001; Treu 2004).”
The Evolution of the Star Formation Activity in Galaxies and Its Dependence on Environment (2005, background): “…models because the local density of galaxies and DM is related to the epoch of initial collapse (Bower et al. 1991, Kauffmann 1995a, 1995b, Kauffmann et al. 1999, Benson et al. 2001, Diaferio et al. 2001, Springel et al. 2001): the most massive structures at any epoch are the earliest to collapse.”
Keck Spectroscopy of Distant GOODS Spheroidal Galaxies: Downsizing in a Hierarchical Universe (2005, background): “Such “downsizing” (i.e. stellar growth that moves systematically to lower mass systems as the Universe expands; Cowie et al. 1996) appears contrary to the expectations of hierarchical models of galaxy formation (Diaferio et al. 2001).”
CAIRNS: The Cluster and Infall Region Nearby Survey. I. Redshifts and Mass Profiles (2003, background): “This conclusion is consistent with previous investigations of galaxies in and near clusters (Balogh et al. 1997; Diaferio et al. 2001; Ellingson et al. 2001; Lewis et al. 2002; Gómez et al. 2003; Treu et al. 2003; Balogh et al. 2004; Gray et al. 2004; Tanaka et al. 2004), and the emission…”