LoCuSS: A COMPARISON OF SUNYAEV-ZEL'DOVICH EFFECT AND GRAVITATIONAL-LENSING MEASUREMENTS OF GALAXY CLUSTERS

Marrone, Daniel P.; Smith, Graham P.; Richard, Johan; Joy, M.; Bonamente, Massimiliano; Hasler, Nicole; Hamilton-Morris, V.; Kneib, Jean-Paul; Culverhouse, T.; Carlstrom, J. E.; Greer, Christopher H.; Hawkins, David; Hennessy, Ryan; Lamb, James W.; Leitch, E. M.; Loh, Michael; Miller, Amber; Mroczkowski, Tony; Muchovej, Stephen; Pryke, C.; Sharp, Matthew; Woody, D. P.

doi:10.1088/0004-637x/701/2/l114

Cited by 52 publications

(63 citation statements)

References 40 publications

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“…More recently, Bonamente et al (2008) examined the scaling relations between Y SZ and total mas, gas mass and gas temperature using 38 clusters observed with Chandra and OVRO/BIMA and found that the slope and the evolution of the observed relations agree with that predicted by a self-similar model in which the evolution of cluster is dominated by gravitational processes (also see Huang et al 2010, for a similar result using AMiBA). Marrone et al (2009) measured the relation between Y SZ and lensing mass within 350 kpc, derived from a strong and weak lensing analysis of HST observations of 14 Xray luminous clusters of galaxies. They found no evidence of segregation in Y between disturbed and undisturbed clusters, as had been seen with T X on the same physical scales.…”

Section: Sz Scaling Relations: Pre-survey-era Observationsmentioning

confidence: 99%

Scaling Relations for Galaxy Clusters: Properties and Evolution

et al. 2013

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Well-calibrated scaling relations between the observable properties and the total masses of clusters of galaxies are important for understanding the physical processes that give rise to these relations. They are also a critical ingredient for studies that aim to constrain cosmological parameters using galaxy clusters. For this reason much effort has been spent during the last decade to better understand and interpret relations of the properties of the intra-cluster medium. Improved X-ray data have expanded the mass range down to galaxy groups, whereas SZ surveys have openened a new observational window on the intracluster medium. In addition, continued progress in the performance of cosmological simulations has allowed a better understanding of the physical processes and selection effects affecting the observed scaling relations. Here we review the recent literature on various scaling relations, focussing on the latest observational measurements and the progress in our understanding of the deviations from self similarity.

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Section: Sz Scaling Relations: Pre-survey-era Observationsmentioning

confidence: 99%

Scaling Relations for Galaxy Clusters: Properties and Evolution

et al. 2013

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“…Weak lensing (WL) mass measurements, which directly probe the projected mass distribution of the cluster, provide a promising way to measure cluster mass independently of their dynamical states (e.g., Marrone et al 2009;McInnes et al 2009;High et al 2012;Hoekstra et al 2012;Miyatake et al 2013;von der Linden et al 2014;Jee et al 2014;Gruen et al 2014;Battaglia et al 2015;Smith et al 2015). However, recent tSZ and WL measurements suggest that the scatter in the tSZ-WL mass scaling relation is on the order of ∼ 20% (e.g., Marrone et al 2012), which is considerably larger than the intrinsic scatter predicted by numerical simulations.…”

Section: Introductionmentioning

confidence: 99%

Covariance in the thermal SZ–weak lensing mass scaling relation of galaxy clusters

Shirasaki

Nagai

Lau

2016

Mon. Not. R. Astron. Soc.

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The thermal Sunyaev-Zel'dovich (tSZ) effect signal is widely recognized as a robust mass proxy of galaxy clusters with small intrinsic scatter. However, recent observational calibration of the tSZ scaling relation using weak lensing (WL) mass exhibits considerably larger scatter than the intrinsic scatter predicted from numerical simulations. This raises a question as to whether we can realize the full statistical power of ongoing and upcoming tSZ-WL observations of galaxy clusters. In this work, we investigate the origin of observed scatter in the tSZ-WL scaling relation, using mock maps of galaxy clusters extracted from cosmological hydrodynamic simulations. We show that the inferred intrinsic scatter from mock tSZ-WL analyses is considerably larger than the intrinsic scatter measured in simulations, and comparable to the scatter in the observed tSZ-WL relation. We show that this enhanced scatter originates from the combination of the projection of correlated structures along the line of sight and the uncertainty in the cluster radius associated with WL mass estimates, causing the amplitude of the scatter to depend on the covariance between tSZ and WL signals. We present a statistical model to recover the unbiased cluster scaling relation and cosmological parameter by taking into account the covariance in the tSZ-WL mass relation from multi-wavelength cluster surveys.

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“…The only investigations of the mass-Y SZ relation using weak lensing masses published to date have been those of Marrone et al (2009Marrone et al ( , 2012, using data from the Local Cluster Substructure Survey (LoCuSS) 1 . The first directly compared 2D quantites (i.e., cylindrical SZ effect vs. projected mass) within a fixed physical radius of 350 kpc, while the second compared the spherically integrated Compton parameter against deprojected mass.…”

Section: Introductionmentioning

confidence: 99%

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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LoCuSS: A COMPARISON OF SUNYAEV-ZEL'DOVICH EFFECT AND GRAVITATIONAL-LENSING MEASUREMENTS OF GALAXY CLUSTERS

Cited by 52 publications

References 40 publications

Scaling Relations for Galaxy Clusters: Properties and Evolution

Scaling Relations for Galaxy Clusters: Properties and Evolution

Covariance in the thermal SZ–weak lensing mass scaling relation of galaxy clusters

Planckintermediate results

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