CIRS: Cluster Infall Regions in the Sloan Digital Sky Survey. I. Infall Patterns and Mass Profiles

By K. Rines, A. Diaferio. 2006

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We use the Fourth Data Release of the Sloan Digital Sky Survey (SDSS) to test the ubiquity of infall patterns around galaxy clusters and measure cluster mass profiles to large radii. The Cluster and Infall Region Nearby Survey (CAIRNS) found infall patterns in nine clusters, but the cluster sample was incomplete. Here we match X-ray cluster catalogs with SDSS, search for infall patterns, and compute mass profiles for a complete sample of X-ray-selected clusters. Very clean infall patterns are apparent in most of the clusters, with the fraction decreasing with increasing redshift due to shallower sampling. All 72 clusters in a well-defined sample limited by redshift (ensuring good sampling) and X-ray flux (excluding superpositions) show infall patterns sufficient to apply the caustic technique. This sample is by far the largest sample of cluster mass profiles extending to large radii to date. Similar to CAIRNS, cluster infall patterns are better defined in observations than in simulations. Further work is needed to determine the source of this difference. We use the infall patterns to compute mass profiles for 72 clusters and compare them to model profiles. Cluster scaling relations using caustic masses agree well with those using X-ray or virial mass estimates, confirming the reliability of the caustic technique. We confirm the conclusion of CAIRNS that cluster infall regions are well fitted by Navarro-Frenk-White (NFW) and Hernquist profiles and poorly fitted by singular isothermal spheres. This much larger sample enables new comparisons of cluster properties with those in simulations. The shapes (specifically NFW concentrations) of the mass profiles agree well with the predictions of simulations. The mass in the infall region is typically comparable to or larger than that in the virial region. Specifically, the mass inside the turnaround radius is on average 2.19 ± 0.18 times that within the virial radius. This ratio agrees well with recent predictions from simulations of the final masses of dark matter halos.

Subfields: Astronomy and Astrophysics, Ecology, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f417f130f09c5dc4a35f807ea039a406778497cc

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Citations in the corpus

Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation (2014, methodology): “The masses were computed in two ways, one using the virial theorem (black squares) and the other (red squares) using the caustic technique (Rines & Diaferio, 2006).”
WIDE-FIELD PRECISION KINEMATICS OF THE M87 GLOBULAR CLUSTER SYSTEM (2011, methodology): “For comparison, more detailed analyses of the Virgo kinematics by Fouqué et al. (2001) and by Tully (2005) imply Mvir ∼ 1015M⊙, and by Rines & Diaferio (2006) implies rvir ≃ 1.9 Mpc and Mvir ∼ 4× 1014M⊙.”
LoCuSS: THE SLOW QUENCHING OF STAR FORMATION IN CLUSTER GALAXIES AND THE NEED FOR PRE-PROCESSING (2015, background): “For most systems, there is a strong contrast in phase-space density from inside to outside these caustics (Rines & Diaferio 2006), making their visual identification relatively simple.”
DARK MATTER HALO PROFILES OF MASSIVE CLUSTERS: THEORY VERSUS OBSERVATIONS (2011, methodology): “…observations (see, e.g., Vikhlinin et al. 2006; Buote et al. 2007; Schmidt & Allen 2007; Gastaldello et al. 2007; Vikhlinin et al. 2009; Sun et al. 2009; Ettori et al. 2011), and galaxy kinematics (Diaferio, Geller, & Rines 2005; Rines & Diaferio 2006; Wojtak & Lokas 2010 and references therein).”
Density profiles of galaxy groups and clusters from SDSS galaxy–galaxy weak lensing (2006, background): “These works (e.g., van der Marel et al. 2000; Biviano & Girardi 2003; Rines et al. 2003; Rines & Diaferio 2006) typically focus on several tens of clusters with a large number of spectroscopic redshifts per cluster, and determine the profile using the cluster infall patterns.”
Cosmological Parameters from Observations of Galaxy Clusters (2011, background): “The identification of these caustics enables mass measurements out to larger radii (up to 10h−1 Mpc), to an accuracy of ∼ 50% (e.g. Rines & Diaferio 2006).”
CLASH-VLT: The mass, velocity-anisotropy, and pseudo-phase-space density profiles of the z = 0.44 galaxy cluster MACS J1206.2-0847 (2013, methodology): “The analyses of the kinematics of individual clusters have found concentrations both in line (Łokas et al. 2006b; Rines & Diaferio 2006) and above the theoretical expectations (Łokas & Mamon 2003; Łokas et al. 2006a; Wojtak & Łokas 2007; Lemze et al. 2009; Wojtak & Łokas 2010; Abdullah et al. 2011).”
The observed concentration–mass relation for galaxy clusters (2007, unknown): “…4.9± 0.2 6.5± 0.3 Xu et al. (2001) Abell 576 0.04 CM 10.9 9.51 14.1 10.85 Rines et al. (2003) RXJ0137 0.0409 X-ray 6.34 0.99 8.32 1.17 Rines & Diaferio (2006) X-ray 4.9± 2.4 6.5± 3.1 Buote & Lewis (2004) Abell 160 0.0432 X-ray 10.14 0.91 13.16 1.04 Rines & Diaferio (2006) Abell 1983 0.0442…”
Planck intermediate results: V. Pressure profiles of galaxy clusters from the Sunyaev-Zeldovich effect (2012, unknown): “…radial quantities has long been shown in X-ray observations (e.g., Arnaud et al. 2001; Pointecouteau et al. 2005; Vikhlinin et al. 2006; Croston et al. 2008; Arnaud et al. 2010), in the optical (e.g., Rines & Diaferio 2006; Wojtak & Lokas 2010), and with weak-lensing (e.g., Postman et al. 2012).”
MEASURING THE ULTIMATE HALO MASS OF GALAXY CLUSTERS: REDSHIFTS AND MASS PROFILES FROM THE HECTOSPEC CLUSTER SURVEY (HeCS) (2012, background): “We construct the HeCS sample to take advantage of two large-area public surveys: the Sloan Digital Sky Survey (SDSS, Stoughton et al. 2002) and the ROSAT All-Sky Survey (RASS, Voges et al. 1999).”
THE CLUSTER LENSING AND SUPERNOVA SURVEY WITH HUBBLE: AN OVERVIEW (2011, methodology): “The caustic technique (Diaferio & Geller 1997; Rines & Diaferio 2006) is, like lensing-based methods, independent of the dynamical state of the cluster and also provides an important cross check on mass estimates from lensing and gas kinematics.”