CAIRNS: The Cluster and Infall Region Nearby Survey. I. Redshifts and Mass Profiles

By K. Rines, Margaret J. Geller, A. Diaferio, Michael J. Kurtz, Thomas H. Jarrett. 2003

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The CAIRNS (Cluster and Infall Region Nearby Survey) project is a spectroscopic survey of the infall regions surrounding eight nearby, rich, X-ray–luminous clusters of galaxies. We have collected 15,654 redshifts (3471 new or remeasured) within ∼5–10 h-1 Mpc of the centers of the clusters, making it the largest study of the infall regions of clusters. We determine cluster membership and the mass profiles of the clusters based on the phase-space distribution of the galaxies. All of the clusters display decreasing velocity dispersion profiles. The mass profiles are fitted well by functional forms based on numerical simulations but exclude an isothermal sphere. Specifically, NFW and Hernquist models provide good descriptions of cluster mass profiles to their turnaround radii. Our sample shows that the predicted infall pattern is ubiquitous in rich, X-ray–luminous clusters over a large mass range. The caustic mass estimates are in excellent agreement with independent X-ray estimates at small radii and with virial estimates at intermediate radii. The mean ratio of the caustic mass to the X-ray mass is 1.03 ± 0.11, and the mean ratio of the caustic mass to the virial mass (when corrected for the surface pressure term) is 0.93 ± 0.07. We further demonstrate that the caustic technique provides reasonable mass estimates even in merging clusters.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/1506893698fc5cc804a787eb352222d85a6582b4

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Observational probes of cosmic acceleration (2012, background): “…(Heisler et al., 1985), “hydrostatic” estimators for the galaxy population (Carlberg et al., 1997), or “velocity caustics” that mark the boundary between galaxies bound to the cluster potential and galaxies above the escape velocity (Regös and Geller, 1989; Diaferio, 1999; Rines et al., 2003).”
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CLASH-VLT: The mass, velocity-anisotropy, and pseudo-phase-space density profiles of the z = 0.44 galaxy cluster MACS J1206.2-0847 (2013, background): “Other studies have found this ratio to be closer to unity (Carlberg et al. 1997a; van der Marel et al. 2000; Biviano & Girardi 2003; Katgert et al. 2004; Rines et al. 2004).”
Environmental Effects on Late‐Type Galaxies in Nearby Clusters (2006, background): “By itself, this provides evidence for infall of late-type galaxies into clusters (see, e.g., Colless & Dunn 1996; Rines et al. 2003).”
Black Holes in Galaxy Mergers: Evolution of Quasars (2005, background): “…isolated disk galaxies, each with an extended dark matter halo with a Hernquist (1990) profile, motivated by cosmological simulations (e.g. Navarro et al. 1996; Busha et al. 2004) and observations of halo properties (e.g. Rines et al. 2002, 2002, 2003, 2004), an exponential gas disk, and a bulge.”
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Minor Galaxy Interactions: Star Formation Rates and Galaxy Properties (2007, background): “Rines et al. (2005) show in their Cluster and Infall Region Nearby Survey (CAIRNS) that outside 2Y3 virial radii from the cluster center, the fraction of galaxies with H star formation detected in their inner disks is comparable to that of the field.”
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CALIFA : a diameter-selected sample for an integral field spectroscopy galaxy survey (2014, background): “The number of galaxies falling inside the average caustics proposed by Rines et al. (2003) for their sample of nearby clusters up to a projected distance of 5 × R200 from any LV or HV association.”
A halo-based galaxy group finder: calibration and application to the 2dFGRS (2004, background): “…halo resides at rest at the centre, while the number density distribution of the fainter, satellite galaxies matches that of the dark matter particles (e.g., Carlberg et al. 1997; van der Marel et al. 2000; Berlind et al. 2003; Lin, Mohr & Stanford 2004; Rines et al. 2004; Diemand et al. 2004).”
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Towards a concordant model of halo occupation statistics (2006, background): “…that the average mass-to-light ratio of clusters continues to increase with mass (Adami et al. 1998; Bahcall & Comerford 2002; Girardi et al. 2002; Marinoni & Hudson 2002; Lin, Mohr & Stanford 2003, 2004; Ramella et al. 2004; Rines et al. 2004; Vale & Ostriker 2004, 2006; Popesso et al. 2005).”
Total mass biases in X-ray galaxy clusters (2008, methodology): “The methods used to derive cluster masses are mainly based on the velocity dispersion of the optical galaxy populations (e.g. Biviano & Girardi 2003; Rines et al. 2003), observations of the X-ray emitting intracluster medium (ICM) (e.g. Finoguenov et al. 2001; Reiprich & Böhringer 2002; Ettori et…”
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