The Canadian Cluster Comparison Project: detailed study of systematics and updated weak lensing masses★

Hoekstra, Henk; Herbonnet, Ricardo; Muzzin, Adam; Babul, Arif; Mahdavi, A.; Viola, Massimo; Cacciato, Marcello

doi:10.1093/mnras/stv275

Cited by 417 publications

(632 citation statements)

References 114 publications

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“…Using the ratio < M P lanck /MW L > as a proxy for the mass bias, von der Linden et al (2014) find < M P lanck /MW L >= 0.688 ± 0.072 for 22 of the clusters in the Planck cosmology sample, and note that adopting this mass bias would substantially reduce the tension. Hoekstra et al (2015) find < M P lanck /MW L >= 0.76 ± 0.05(stat) ± 0.06(sys) for 37 clusters common between the Canadian Cluster Comparison Project and the Planck sample, and conclude that this does not resolve the tension.…”

Section: Comparison With Other Workmentioning

confidence: 89%

Cosmic discordance: are Planck CMB and CFHTLenS weak lensing measurements out of tune?

MacCrann

Zuntz

Bridle

et al. 2015

Monthly Notices of the Royal Astronomical Society

177

192

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We examine the level of agreement between low redshift weak lensing data and the CMB using measurements from the CFHTLenS and Planck+WMAP polarization. We perform an independent analysis of the CFHTLenS six bin tomography results of Heymans et al. (2013). We extend their systematics treatment and find the cosmological constraints to be relatively robust to the choice of non-linear modeling, extension to the intrinsic alignment model and inclusion of baryons. We find that when marginalised in the Ω m -σ 8 plane, the 95% confidence contours of CFHTLenS and Planck+WP only just touch, but the discrepancy is less significant in the full 6-dimensional parameter space of ΛCDM. Allowing a massive active neutrino or tensor modes does not significantly resolve the tension in the full n-dimensional parameter space. Our results differ from some in the literature because we use the full tomographic information in the weak lensing data and marginalize over systematics. We note that adding a sterile neutrino to ΛCDM brings the 2d marginalised contours into greater overlap, mainly due to the extra effective number of neutrino species, which we find to be 0.88 ± 0.43 (68%) greater than standard on combining the datasets. We discuss why this is not a completely satisfactory resolution, leaving open the possibility of other new physics or observational systematics as contributing factors. We provide updated cosmology fitting functions for the CFHTLenS constraints and discuss the differences from ones used in the literature.

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Section: Comparison With Other Workmentioning

confidence: 89%

Cosmic discordance: are Planck CMB and CFHTLenS weak lensing measurements out of tune?

MacCrann

Zuntz

Bridle

et al. 2015

Monthly Notices of the Royal Astronomical Society

177

192

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“…The correction factor, (1 + n non−bkg /n bkg ) is equivalent to the boost factor, under the assumption of a radially uniform distribution of background galaxies (e.g. Applegate et al 2014;Hoekstra et al 2015), that we discuss in Section 4.1.4. Equation 12 shows that the average lensing signal obtained from our formalism is simply underestimated by the fraction of non-background to background galaxies.…”

Section: Selection Of Background Galaxiesmentioning

confidence: 99%

“…attempting to avoid regions of the clusters at which the measured shear exceeds that injected into the STEP simulations (Applegate et al 2014). Hoekstra et al (2015) recently emphasised the importance of carefully matching the properties of the simulated data used for such tests to the observational data. In this article we further develop the shape measurement methods that we developed in Okabe et al (2013) and extend our tests of these methods to include realistic galaxies.…”

Section: Introductionmentioning

confidence: 99%

“…After falling into disuse for a decade since Kneib et al (2003) first proposed the method, boosting the measured shear signal to correct statistically for contamination has enjoyed a renaissance of late (e.g. Applegate et al 2014;Hoekstra et al 2015). This method is applied to both red and blue galaxies, either by excluding the red sequence galaxies or simply selecting faint galaxies, as per Kneib et al (2003).…”

Section: Introductionmentioning

confidence: 99%

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LoCuSS: weak-lensing mass calibration of galaxy clusters

Okabe

Smith

2016

Mon. Not. R. Astron. Soc.

155

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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“…(2013) (see also Hoekstra et al 2012Hoekstra et al , 2015 Table 1). These are all listed as red cored galaxies in (Bildfell et al 2008), except Abell 2204 which is a known blue core BCG.…”

Section: Optical Spectroscopy and Data Reductionmentioning

confidence: 99%

The regulation of star formation in cool-core clusters: imprints on the stellar populations of brightest cluster galaxies

Loubser

Babul

Hoekstra

et al. 2015

Mon. Not. R. Astron. Soc.

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A fraction of brightest cluster galaxies (BCGs) shows bright emission in the UV and the blue part of the optical spectrum, which has been interpreted as evidence of recent star formation. Most of these results are based on the analysis of broadband photometric data. Here, we study the optical spectra of a sample of 19 BCGs hosted by X-ray luminous galaxy clusters at 0.15 < z < 0.3, a subset from the Canadian Cluster Comparison Project (CCCP) sample. We identify plausible star formation histories of the galaxies by fitting Simple Stellar Populations (SSPs) as well as composite populations, consisting of a young stellar component superimposed on an intermediate/old stellar component, to accurately constrain their star formation histories. We detect prominent young (∼ 200 Myr) stellar populations in 4 of the 19 galaxies. Of the four, the BCG in Abell 1835 shows remarkable A-type stellar features indicating a relatively large population of young stars, which is extremely unusual even amongst star forming BCGs. We constrain the mass contribution of these young components to the total stellar mass to be typically between 1% to 3%, but rising to 7% in Abell 1835. We find that the four of the BCGs with strong evidence for recent star formation (and only these four galaxies) are found within a projected distance of 5 kpc of their host cluster's X-ray peak, and the diffuse, X-ray gas surrounding the BCGs exhibit a ratio of the radiative cooling-to-free-fall time (t c /t ff ) of ≤ 10. These are also some of the clusters with the lowest central entropy. Our results are consistent with the predictions of the precipitation-driven star formation and AGN feedback model, in which the radiatively cooling diffuse gas is subject to local thermal instabilities once the instability parameter t c /t ff falls below ∼ 10, leading to the condensation and precipitation of cold gas. The number of galaxies in our sample where the host cluster satisfies all the criteria for recent and ongoing star formation is small, but their stellar populations suggest a timescale for star formation to restart of the order of ∼ 200 Myrs.

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The Canadian Cluster Comparison Project: detailed study of systematics and updated weak lensing masses★

Cited by 417 publications

References 114 publications

Cosmic discordance: are Planck CMB and CFHTLenS weak lensing measurements out of tune?

Cosmic discordance: are Planck CMB and CFHTLenS weak lensing measurements out of tune?

LoCuSS: weak-lensing mass calibration of galaxy clusters

The regulation of star formation in cool-core clusters: imprints on the stellar populations of brightest cluster galaxies

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