Clash: Weak-Lensing Shear-and-Magnification Analysis of 20 Galaxy Clusters

Umetsu, Keiichi; Medezinski, Elinor; Nonino, M.; Merten, Julian; Postman, Marc; Meneghetti, M.; Donahue, M.; Czakon, Nicole G.; Molino, A.; Seitz, S.; Gruen, David; Lemze, Doron; Balestra, I.; Benı́tez, N.; Biviano, A.; Broadhurst, Tom; Ford, H. C.; Grillo, C.; Koekemoer, Anton M.; Melchior, P.; Mercurio, A.; Moustakas, John; Rosati, P.; Zitrin, Adi

doi:10.1088/0004-637x/795/2/163

Cited by 300 publications

(744 citation statements)

References 133 publications

(304 reference statements)

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“…We do not assume any specific functions of n b because the background distribution is not constant, and may be depleted or boosted by a magnification bias (e.g. Broadhurst, Taylor & Peacock 1995;Umetsu et al 2011Umetsu et al , 2014Coupon, Broadhurst & Umetsu 2013). The second term in the bracket denotes the member galaxy distribution; B is the fraction, f (∆C) is the colour distribution and nm(r) is the radial distribution.…”

Section: Selection Of Background Galaxiesmentioning

confidence: 99%

“…The LoCuSS sample is an LX -limited sub-set of clusters from ROSAT All-sky Survey (RASS) at 0.15 < z < 0.3; the CCCP sample is a mixture of X-ray luminous clusters for which optical data are available from the CFHT archive and a temperature-selected sub-set of clusters from the ASCA survey spanning 0.15 < z < 0.55; the WtG sample is a representative flux-limited sub-set of the RASS clusters at 0.15 < z < 0.7. Smaller, generally heterogeneous, samples of X-ray clusters are also studied, for example, by the the Cluster Lensing And Supernova Survey with Hubble (CLASH; Postman et al 2012;Umetsu et al 2014) and the 400SD surveys (Israel et al 2012). Whilst samples of Sunyaev Zeldovich (SZ) Effect detected clusters are growing rapidly, the weak-lensing studies of SZ samples currently number handfuls of clusters (e.g.…”

Section: Introductionmentioning

confidence: 99%

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LoCuSS: weak-lensing mass calibration of galaxy clusters

Okabe

Smith

2016

Mon. Not. R. Astron. Soc.

150

179

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We present weak-lensing mass measurements of 50 X-ray luminous galaxy clusters at 0.15 z 0.3, based on uniform high quality observations with Suprime-Cam mounted on the 8.2-m Subaru telescope. We pay close attention to possible systematic biases, aiming to control them at the ∼ < 4 per cent level. The dominant source of systematic bias in weak-lensing measurements of the mass of individual galaxy clusters is contamination of background galaxy catalogues by faint cluster and foreground galaxies. We extend our conservative method for selecting background galaxies with (V − i ′ ) colours redder than the red sequence of cluster members to use a colour-cut that depends on cluster-centric radius. This allows us to define background galaxy samples that suffer 1 per cent contamination, and comprise 13 galaxies per square arcminute. Thanks to the purity of our background galaxy catalogue, the largest systematic that we identify in our analysis is a shape measurement bias of 3 per cent, that we measure using simulations that probe weak shears upto g = 0.3. Our individual cluster mass and concentration measurements are in excellent agreement with predictions of the mass-concentration relation. Equally, our stacked shear profile is in excellent agreement with the Navarro Frenk and White profile. Our new LoCuSS mass measurements are consistent with the CCCP and CLASH surveys, and in tension with the Weighing the Giants at ∼ 1 − 2σ significance. Overall, the consensus at z 0.3 that is emerging from these complementary surveys represents important progress for cluster mass calibration, and augurs well for cluster cosmology.

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Section: Selection Of Background Galaxiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

LoCuSS: weak-lensing mass calibration of galaxy clusters

Okabe

Smith

2016

Mon. Not. R. Astron. Soc.

150

179

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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).…”

Section: Conditional Scalingmentioning

confidence: 99%

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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“…Let us first discuss the results on the mass µ = log Mvir. The relative error σµ/µ from shear + magnification only turns out to be Umetsu et al 2014). This is partly due to the larger number density and smaller intrinsic shear variance and partly to the well known fact that Fisher matrix variances are lower limits to the errors one can achieve.…”

Section: Present Day Constraintsmentioning

confidence: 99%

“…We can now introduce the likelihood function for the shear data as (see, e.g., Umetsu et al 2014) ln Lg(p) = − 1 2…”

Section: Cluster Mass From Lensingmentioning

confidence: 99%

Improving lensing cluster mass estimate with flexion

Cardone

Vicinanza

et al. 2016

Mon. Not. R. Astron. Soc.

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Gravitational lensing has long been considered as a valuable tool to determine the total mass of galaxy clusters. The shear profile as inferred from the statistics of ellipticity of background galaxies allows to probe the cluster intermediate and outer regions thus determining the virial mass estimate. However, the mass sheet degeneracy and the need for a large number of background galaxies motivate the search for alternative tracers which can break the degeneracy among model parameters and hence improve the accuracy of the mass estimate. Lensing flexion, i.e. the third derivative of the lensing potential, has been suggested as a good answer to the above quest since it probes the details of the mass profile. We investigate here whether this is indeed the case considering jointly using weak lensing, magnification and flexion. We use a Fisher matrix analysis to forecast the relative improvement in the mass accuracy for different assumptions on the shear and flexion signal -to -noise (S/N) ratio also varying the cluster mass, redshift, and ellipticity. It turns out that the error on the cluster mass may be reduced up to a factor ∼ 2 for reasonable values of the flexion S/N ratio. As a general result, we get that the improvement in mass accuracy is larger for more flattened haloes, but it extracting general trends is a difficult because of the many parameters at play. We nevertheless find that flexion is as efficient as magnification to increase the accuracy in both mass and concentration determination.

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Clash: Weak-Lensing Shear-and-Magnification Analysis of 20 Galaxy Clusters

Cited by 300 publications

References 133 publications

LoCuSS: weak-lensing mass calibration of galaxy clusters

LoCuSS: weak-lensing mass calibration of galaxy clusters

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

Improving lensing cluster mass estimate with flexion

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