MEASURING THE ULTIMATE HALO MASS OF GALAXY CLUSTERS: REDSHIFTS AND MASS PROFILES FROM THE HECTOSPEC CLUSTER SURVEY (HeCS)

Rines, Kenneth J.; Geller, Margaret J.; Diaferio, Antonaldo; Kurtz, Michael J.

doi:10.1088/0004-637x/767/1/15

Cited by 203 publications

(322 citation statements)

References 107 publications

(176 reference statements)

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“…The HeCS covered two clusters later on analysed in Umetsu et al (2014), i.e., A2261 and RXJ2129. The prediction for RXJ2129 is in excellent agreement with the measurements (Rines et al 2013, σv = 858 +71 −57 km/s). On the other hand, the prediction slightly exceeds the observed velocity dispersion of A2261 (Rines et al 2013, σv = 780 +78 −60 km/s), even though the small discrepancy is fully covered by the uncertainty due to the intrinsic dispersion of the scaling.…”

Section: Conditional Scalingsupporting

confidence: 82%

“…The prediction for RXJ2129 is in excellent agreement with the measurements (Rines et al 2013, σv = 858 +71 −57 km/s). On the other hand, the prediction slightly exceeds the observed velocity dispersion of A2261 (Rines et al 2013, σv = 780 +78 −60 km/s), even though the small discrepancy is fully covered by the uncertainty due to the intrinsic dispersion of the scaling. From top to bottom, the red, green, and blue lines show the 85, 50, and 15 per cent completeness levels, respectively.…”

Section: Conditional Scalingsupporting

confidence: 82%

See 1 more Smart Citation

CoMaLit – IV. Evolution and self-similarity of scaling relations with the galaxy cluster mass

Sereno¹,

Ettori²

2015

Monthly Notices of the Royal Astronomical Society

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The scaling of observable properties of galaxy clusters with mass evolves with time. Assessing the role of the evolution is crucial to study the formation and evolution of massive halos and to avoid biases in the calibration. We present a general method to infer the mass and the redshift dependence, and the time-evolving intrinsic scatter of the mass-observable relations. The procedure self-calibrates the redshift dependent completeness function of the sample. The intrinsic scatter in the mass estimates used to calibrate the relation is considered too. We apply the method to the scaling of mass M ∆ versus line of sight galaxy velocity dispersion σ v , optical richness, X-ray luminosity, L X , and Sunyaev-Zel'dovich signal. Masses were calibrated with weak lensing measurements. The measured relations are in good agreement with time and mass dependencies predicted in the self-similar scenario of structure formation. The lone exception is the L X -M ∆ relation whose time evolution is negative in agreement with formation scenarios with additional radiative cooling and uniform preheating at high redshift. The intrinsic scatter in the σ v -M ∆ relation is notably small, of order of 14 per cent. Robust predictions on the observed properties of the galaxy clusters in the CLASH sample are provided as cases of study. Catalogs and scripts are publicly available at

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Section: Conditional Scalingsupporting

confidence: 82%

Section: Conditional Scalingsupporting

confidence: 82%

CoMaLit – IV. Evolution and self-similarity of scaling relations with the galaxy cluster mass

Sereno¹,

Ettori²

2015

Monthly Notices of the Royal Astronomical Society

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“…This method is used (e.g. Carlberg, Yee & Ellingson 1997;Biviano & Poggianti 2009;Munari et al 2013;Rines et al 2013) when the number of spectroscopic members per cluster is low and does not allow accurate, individual, velocity dispersion measurements. Becker et al (2007), in particular, could measure with accuracy the relation between optical richness and velocity dispersion of optically selected galaxy clusters up to z = 0.3 by means of stacking systems in richness and redshift.…”

Section: Cluster L X -σ Relation From Stacked Velocity-distance Diagramsmentioning

confidence: 99%

SPIDERS: the spectroscopic follow-up of X-ray-selected clusters of galaxies in SDSS-IV

Clerc

Merloni

Zhang

et al. 2016

Mon. Not. R. Astron. Soc.

105

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SPIDERS (The SPectroscopic IDentification of eROSITA Sources) is a programme dedicated to the homogeneous and complete spectroscopic follow-up of X-ray active galactic nuclei and galaxy clusters over a large area (∼7500 deg 2 ) of the extragalactic sky. SPIDERS is part of the Sloan Digital Sky Survey (SDSS)-IV project, together with the Extended Baryon Oscillation Spectroscopic Survey and the Time-Domain Spectroscopic Survey. This paper describes the largest project within SPIDERS before the launch of eROSITA: an optical spectroscopic survey of X-ray-selected, massive (∼10 14 -10 15 M ) galaxy clusters discovered in ROSAT and XMMNewton imaging. The immediate aim is to determine precise ( z ∼ 0.001) redshifts for 4000-5000 of these systems out to z ∼ 0.6. The scientific goal of the program is precision cosmology, using clusters as probes of large-scale structure in the expanding Universe. We present the cluster samples, target selection algorithms and observation strategies. We demonstrate the efficiency of selecting targets using a combination of SDSS imaging data, a robust red-sequence finder and a dedicated prioritization scheme. We describe a set of algorithms and workflow developed to collate spectra and assign cluster membership, and to deliver catalogues of spectroscopically confirmed clusters. We discuss the relevance of line-of-sight velocity dispersion estimators for the richer systems. We illustrate our techniques by constructing a catalogue of 230 spectroscopically validated clusters (0.031 < z < 0.658), found in pilot observations. We discuss two potential science applications of the SPIDERS sample: the study of the X-ray luminosity-velocity dispersion (L X -σ ) relation and the building of stacked phase-space diagrams.

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“…Over time, the measured escape edge in the outskirts of galaxy clusters grows in amplitude to represent the predicted escape velocity defined by the potential. This dynamical evolution of the escape edge in the cluster infall regions is important for studies which use the escape velocity technique to measure mass profiles to well beyond the virial radius (Rines & Diaferio 2006;Rines et al 2013). …”

Section: Mass and Redshift Dependencementioning

confidence: 99%

Inferring Gravitational Potentials From Mass Densities in Cluster-Sized Halos

Miller

Stark

Gifford

et al. 2016

ApJ

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We use N-body simulations to quantify how the escape velocity in cluster-sized halos maps to the gravitational potential in a ΛCDM universe. Using spherical density-potential pairs and the Poisson equation, we find that the matter density inferred gravitational potential profile predicts the escape velocity profile to within a few percent accuracy for group and cluster-sized halos (10 < < M 1013 200 15 M  , with respect to the critical density). The accuracy holds from just outside the core to beyond the virial radius. We show the importance of explicitly incorporating a cosmological constant when inferring the potential from the Poisson equation. We consider three density models and find that the Einasto and Gamma profiles provide a better joint estimate of the density and potential profiles than the Navarro, Frenk, and White profile, which fails to accurately represent the escape velocity. For individual halos, the 1σ scatter between the measured escape velocity and the density-inferred potential profile is small (<5%). Finally, while the sub-halos show 15% biases in their representation of the particle velocity dispersion profile, the sub-halo escape velocity profile matches the dark matter escape velocity profile to high accuracy with no evidence of velocity bias outside 0.4r 200 .

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MEASURING THE ULTIMATE HALO MASS OF GALAXY CLUSTERS: REDSHIFTS AND MASS PROFILES FROM THE HECTOSPEC CLUSTER SURVEY (HeCS)

Cited by 203 publications

References 107 publications

CoMaLit – IV. Evolution and self-similarity of scaling relations with the galaxy cluster mass

CoMaLit – IV. Evolution and self-similarity of scaling relations with the galaxy cluster mass

SPIDERS: the spectroscopic follow-up of X-ray-selected clusters of galaxies in SDSS-IV

Inferring Gravitational Potentials From Mass Densities in Cluster-Sized Halos

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