Weak lensing analysis of SZ-selected clusters of galaxies from the SPT and Planck surveys

Seitz, S.; Brimioulle, F.; Kosyra, R.; Koppenhoefer, J.; Lee, Chien‐Hsiu; Bender, Ralf; Riffeser, A.; Eichner, T.; Weidinger, T.; Bierschenk, M.

doi:10.1093/mnras/stu949

Cited by 122 publications

(180 citation statements)

References 164 publications

Supporting

Mentioning

161

Contrasting

Order By: Relevance

“…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. High et al 2012;Gruen et al 2014).…”

Section: Introductionmentioning

confidence: 99%

LoCuSS: weak-lensing mass calibration of galaxy clusters

Okabe

Smith

2016

Mon. Not. R. Astron. Soc.

153

179

View full text Add to dashboard Cite

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.

show abstract

Section: Introductionmentioning

confidence: 99%

LoCuSS: weak-lensing mass calibration of galaxy clusters

Okabe

Smith

2016

Mon. Not. R. Astron. Soc.

153

179

View full text Add to dashboard Cite

show abstract

“…Averaging the weak-lensing signals from several clusters reduces some of these biases (Corless & King 2009), but this requires significant sample sizes. Initial calibrations of tSZ masses using weaklensing observations include measurements on two ACT clusters (Miyatake et al 2013;Jee et al 2014), individual SPT clusters (McInnes et al 2009;High et al 2012), Planck clusters (e.g., von der Linden et al 2014b;Hoekstra et al 2015), both SPT and Planck clusters (Gruen et al 2014), and selected pointed observations of massive clusters from the literature (Marrone et al 2009;Hoekstra et al 2012;Marrone et al 2012). These calibrations are often presented in terms of a bias parameter,…”

Section: Introductionmentioning

confidence: 99%

Weak-lensing mass calibration of the Atacama Cosmology Telescope equatorial Sunyaev-Zeldovich cluster sample with the Canada-France-Hawaii telescope stripe 82 survey

Battaglia

Leauthaud

Miyatake

et al. 2016

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

Mass calibration uncertainty is the largest systematic effect for using clusters of galaxies to constrain cosmological parameters. We present weak lensing mass measurements from the Canada-FranceHawaii Telescope Stripe 82 Survey for galaxy clusters selected through their high signal-to-noise thermal Sunyaev-Zeldovich (tSZ) signal measured with the Atacama Cosmology Telescope (ACT). For a sample of 9 ACT clusters with a tSZ signal-to-noise greater than five the average weak lensing mass is (4.8 ± 0.8) × 10 14 M , consistent with the tSZ mass estimate of (4.70 ± 1.0) × 10 14 M which assumes a universal pressure profile for the cluster gas. Our results are consistent with previous weaklensing measurements of tSZ-detected clusters from the Planck satellite. When comparing our results, we estimate the Eddington bias correction for the sample intersection of Planck and weak-lensing clusters which was previously excluded.

show abstract

“…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.

View full text Add to dashboard Cite

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.

show abstract

Weak lensing analysis of SZ-selected clusters of galaxies from the SPT and Planck surveys

Cited by 122 publications

References 164 publications

LoCuSS: weak-lensing mass calibration of galaxy clusters

LoCuSS: weak-lensing mass calibration of galaxy clusters

Weak-lensing mass calibration of the Atacama Cosmology Telescope equatorial Sunyaev-Zeldovich cluster sample with the Canada-France-Hawaii telescope stripe 82 survey

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

Contact Info

Product

Resources

About