The Integrated Sunyaev-Zeldovich Effect as a Superior Method for Measuring the Mass of Clusters of Galaxies

Motl, Patrick M.; Hallman, Eric J.; Burns, Jack O.; Norman, Michael L.

doi:10.1086/430144

Cited by 207 publications

(287 citation statements)

References 17 publications

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“…Since the SZE signal is proportional to the intracluster plasma temperature and the total number of electrons, the Y X -parameter is defined as Y X = T × M gas . This parameter has been promoted as a very good mass proxy for galaxy clusters (Motl et al 2005;Kravtsov et al 2006). Values for the slope of the L bol − Y X relation of 0.65-1.1 and for the L band −Y X relation of 0.8-1.14 agree well with the predictions (combining the L X −T and Y X −T relations) of values of 0.98 and 0.81, respectively.…”

Section: Other Relationssupporting

confidence: 66%

Modelling self-similar appearance of galaxy clusters in X-rays

Böhringer

Dolag

Chon

2012

A&A

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Context. The largest uncertainty for cosmological studies using clusters of galaxies is introduced by our limited knowledge of the statistics of galaxy cluster structure and the related scaling relations between observables and cluster mass. A large effort has therefore been made to compile global galaxy cluster properties, in particular those obtained through X-ray observations, and to study their scaling relations. However, the scaling schemes used in the literature differ. Aims. The present paper aims to clarify this situation by providing a thorough review of the scaling laws within the standard model of large-scale structure growth and to discuss various steps in practical approximations. Methods. We derived the scaling laws for X-ray observables and cluster mass within the pure gravitational structure growth scenario. Using N-body simulations we tested the recent formation approximation used in earlier analytic approaches. It involves a redshiftdependent overdensity parameter. We find this approximation less precise than using a fiducial radius based on a fixed overdensity with respect to critical density. Results. Inspired by the comparison of the predicted scaling relations with observations, we propose a first-order modification of the scaling scheme to include the observed effects of hydrodynamics in structure formation. This modification involves a cluster-mass dependent gas-mass fraction. We also discuss the observational results of the reshift evolution of the most important scaling relations and find that a redshift dependence of the gas mass to total mass relation also has to be invoked within our modification scheme. Conclusions. We find that the current observational data are, within their uncertainties, consistent with the proposed modified scaling laws.

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Section: Other Relationssupporting

confidence: 66%

Modelling self-similar appearance of galaxy clusters in X-rays

Böhringer

Dolag

Chon

2012

A&A

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“…Our observational and theoretical The SZ signal is of singular interest because it is not affected by cosmological dimming and because the total SZ flux or integrated Compton parameter, Y SZ , is expected to correlate particularly tightly with mass (e.g., Barbosa et al 1996;da Silva et al 2004;Motl et al 2005;Wik et al 2008;Aghanim et al 2009). SZ-detected cluster samples are thus expected to range to high redshift and be as near as possible to mass-selected, making them potentially very powerful cosmological probes.…”

Section: Introductionmentioning

confidence: 98%

Planckintermediate results

Ade¹,

Aghanim²,

Arnaud³

et al. 2013

A&A

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We examine the relation between the galaxy cluster mass M and Sunyaev-Zeldovich (SZ) effect signal D 2 A Y 500 for a sample of 19 objects for which weak lensing (WL) mass measurements obtained from Subaru Telescope data are available in the literature. Hydrostatic X-ray masses are derived from XMM-Newton archive data, and the SZ effect signal is measured from Planck all-sky survey data. We find an M WL −D 2 A Y 500 relation that is consistent in slope and normalisation with previous determinations using weak lensing masses; however, there is a normalisation offset with respect to previous measures based on hydrostatic X-ray mass-proxy relations. We verify that our SZ effect measurements are in excellent agreement with previous determinations from Planck data. For the present sample, the hydrostatic X-ray masses at R 500 are on average ∼20 percent larger than the corresponding weak lensing masses, which is contrary to expectations. We show that the mass discrepancy is driven by a difference in mass concentration as measured by the two methods and, for the present sample, that the mass discrepancy and difference in mass concentration are especially large for disturbed systems. The mass discrepancy is also linked to the offset in centres used by the X-ray and weak lensing analyses, which again is most important in disturbed systems. We outline several approaches that are needed to help achieve convergence in cluster mass measurement with X-ray and weak lensing observations.

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“…This expectation, borne out by both numerical simulations (e.g., da Silva et al 2004;Motl et al 2005;Kravtsov et al 2006) and indirectly from X-ray observations using Y X , the product of the gas mass and mean temperature Arnaud et al 2007;Vikhlinin et al 2009), strongly motivates the use of SZ cluster surveys as cosmological probes. Theory predicts the cluster abundance and its evolution -the mass function -in terms of M and the cosmological parameters.…”

Section: Introductionmentioning

confidence: 98%

The galaxy clusterY_SZ−L_XandY_SZ−Mrelations from the WMAP 5-yr data

Melin

Bartlett

Delabrouille

et al. 2010

A&A

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We use multifrequency matched filters to estimate, in the WMAP 5-year data, the Sunyaev-Zel'dovich (SZ) fluxes of 893 ROSAT NORAS/REFLEX clusters spanning the luminosity range L X,[0.1−2.4] keV = 2×10 41 −3.5×10 45 erg s −1 . The filters are spatially optimised by using the universal pressure profile recently obtained from combining XMM-Newton observations of the REXCESSsample and numerical simulations. Although the clusters are individually only marginally detected, we are able to firmly measure the SZ signal (>10σ) when averaging the data in luminosity/mass bins. The comparison between the bin-averaged SZ signal versus luminosity and X-ray model predictions shows excellent agreement, implying that there is no deficit in SZ signal strength relative to expectations from the X-ray properties of clusters. Using the individual cluster SZ flux measurements, we directly constrain the Y 500 −L X and Y 500 −M 500 relations, where Y 500 is the Compton y-parameter integrated over a sphere of radius r 500 . The Y 500 −M 500 relation, derived for the first time in such a wide mass range, has a normalisation Y * 500 = [1.60 ± 0.19] × 10 −3 arcmin 2 at M 500 = 3 × 10 14 h −1 M , in excellent agreement with the X-ray prediction of 1.54 × 10 −3 arcmin 2 , and a mass exponent of α = 1.79 ± 0.17, consistent with the self-similar expectation of 5/3. Constraints on the redshift exponent are weak due to the limited redshift range of the sample, although they are compatible with self-similar evolution.

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The Integrated Sunyaev-Zeldovich Effect as a Superior Method for Measuring the Mass of Clusters of Galaxies

Cited by 207 publications

References 17 publications

Modelling self-similar appearance of galaxy clusters in X-rays

Modelling self-similar appearance of galaxy clusters in X-rays

Planckintermediate results

The galaxy clusterY_SZ−L_XandY_SZ−Mrelations from the WMAP 5-yr data

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The Integrated Sunyaev-Zeldovich Effect as a Superior Method for Measuring the Mass of Clusters of Galaxies

Cited by 207 publications

References 17 publications

Modelling self-similar appearance of galaxy clusters in X-rays

Modelling self-similar appearance of galaxy clusters in X-rays

Planckintermediate results

The galaxy clusterYSZ−LXandYSZ−Mrelations from the WMAP 5-yr data

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Product

Resources

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The galaxy clusterY_SZ−L_XandY_SZ−Mrelations from the WMAP 5-yr data