The relation between velocity dispersion and mass in simulated clusters of galaxies: dependence on the tracer and the baryonic physics

Munari, E.; Biviano, A.; Borgani, S.; Murante, Giuseppe; Fabjan, D.

doi:10.1093/mnras/stt049

Cited by 256 publications

(401 citation statements)

References 65 publications

Supporting

Mentioning

335

Contrasting

Order By: Relevance

“…Numerical simulations confirmed that the σv-M∆ relation is consistent with the self-similar scaling with mass (Evrard et al 2008;Munari et al 2013;Saro et al 2013). Some differences may arise from the galaxy population used to estimate the velocity dispersion and from the impact of selection using galaxy colour, projected separation from the cluster centre, galaxy luminosity, and spectroscopic redshift (Saro et al 2013).…”

Section: σV-m∆supporting

confidence: 64%

“…This is the approach usually followed in numerical simulations (Evrard et al 2008;Munari et al 2013;Saro et al 2013) to built mass proxies based on the velocity dispersion without assuming dynamical equilibrium and without exploiting the properties of the infall patterns.…”

Section: Discussionmentioning

confidence: 99%

“…The shaded blue region encloses the 68 per cent confidence region around the median relation due to uncertainties on the scaling parameters. The red line represents the theoretical prediction based on Munari et al (2013) at the median redshift of the sample. Masses are in units of 10 14 M .…”

Section: Conditional Scalingmentioning

confidence: 99%

See 2 more Smart Citations

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

Sereno¹,

Ettori²

2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

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

show abstract

Section: σV-m∆supporting

confidence: 64%

Section: Discussionmentioning

confidence: 99%

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

View full text Add to dashboard Cite

show abstract

“…For haloes without these effects, the velocity dispersion profiles are isothermal and isotropic as in Paper I, with a velocity dispersion that depends on halo mass and radius through the scaling σ 2 200 = 1 2 GM200/R200 (but see Mamon et al 2010;Munari et al 2013;Old et al 2013). The updated model, including a more realistic velocity dispersion profile and an anisotropy model, will be described in Skibba (in preparation).…”

Section: Halo Occupation Distribution Modelmentioning

confidence: 97%

Galaxy Cluster Mass Reconstruction Project – II. Quantifying scatter and bias using contrasting mock catalogues

Old

Wojtak

Mamon

et al. 2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

This article is the second in a series in which we perform an extensive comparison of various galaxy-based cluster mass estimation techniques that utilise the positions, velocities and colours of galaxies. Our aim is to quantify the scatter, systematic bias and completeness of cluster masses derived from a diverse set of 25 galaxy-based methods using two contrasting mock galaxy catalogues based on a sophisticated halo occupation model and a semi-analytic model. Analysing 968 clusters, we find a wide range in the RMS errors in log M 200c delivered by the different methods (0.18 to 1.08 dex, i.e., a factor of ∼1.5 to 12), with abundance matching and richness methods providing the best results, irrespective of the input model assumptions. In addition, certain methods produce a significant number of catastrophic cases where the mass is under-or over-estimated by a factor greater than 10. Given the steeply falling high-mass end of the cluster mass function, we recommend that richness or abundance matching-based methods are used in conjunction with these methods as a sanity check for studies selecting high mass clusters. We see a stronger correlation of the recovered to input number of galaxies for both catalogues in comparison with the group/cluster mass, however, this does not guarantee that the correct member galaxies are being selected. We do not observe significantly higher scatter for either mock galaxy catalogues. Our results have implications for cosmological analyses that utilise the masses, richnesses, or abundances of clusters, which have different uncertainties when different methods are used.

show abstract

“…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

View full text Add to dashboard Cite

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.

show abstract

The relation between velocity dispersion and mass in simulated clusters of galaxies: dependence on the tracer and the baryonic physics

Cited by 256 publications

References 65 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

Galaxy Cluster Mass Reconstruction Project – II. Quantifying scatter and bias using contrasting mock catalogues

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

Contact Info

Product

Resources

About