The tau of galaxy clusters

Battaglia, Nicholas

doi:10.1088/1475-7516/2016/08/058

Cited by 106 publications

(174 citation statements)

References 95 publications

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“…Battaglia et al (2016) noted that the incomplete overlap of the cluster samples introduces a bias in the recovered (1 − b SZ ) parameter (Malmquist bias), and we indicate the suggested corrections from Battaglia et al (2016) in Fig. 6.…”

Section: Discussionsupporting

confidence: 50%

“…9 We note, however, that we are unable to use one cluster in our CLASH sample because of its negative signal-to-noise value. Battaglia et al (2016), apart from the most extreme cases. This is satisfying because the samples and the lensing mass extraction methodologies differ significantly.…”

Section: Discussionmentioning

confidence: 89%

“…Malmquist and Eddington bias affect some of the points to an uncertain degree. Battaglia et al (2016) estimated the Malmquist bias corrections on the WtG and CCCP determinations, which we indicate in the figure. Our constraint fully accounts for these, as well as astrophysical effects.…”

Section: Resultsmentioning

confidence: 99%

“…We have used Planck as a follow-up to the CLASH sample and, as a consequence, are not affected by the selection A89, page 10 of 14 (Malmquist 7 ) bias noted by Battaglia et al (2016) 8 . This bias arises in the WtG and CCCP studies because some of their clusters do not have Planck detections 9 .…”

Section: Discussionmentioning

confidence: 99%

“…PXX is the 2013 SZ cluster cosmology analysis by Planck (Planck Collaboration XX 2014) and represents the top-hat range used as a prior in that analysis. The WtG and CCCP points are, respectively, from von der Linden et al (2014) and Hoekstra et al (2015), with the red arrows showing the corrections estimated by Battaglia et al (2016); the error bars increase to include the uncertainty on this correction. The Simet et al (2017), based on lensing stacks of the MCXC catalog, and the LoCUSS results are reproduced as labeled.…”

Section: Discussionmentioning

confidence: 99%

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Calibrating thePlanckcluster mass scale with CLASH

Penna-Lima

Bartlett

Rozo

et al. 2017

A&A

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We determine the mass scale of Planck galaxy clusters using gravitational lensing mass measurements from the Cluster Lensing And Supernova survey with Hubble (CLASH). We have compared the lensing masses to the Planck Sunyaev-Zeldovich (SZ) mass proxy for 21 clusters in common, employing a Bayesian analysis to simultaneously fit an idealized CLASH selection function and the distribution between the measured observables and true cluster mass. We used a tiered analysis strategy to explicitly demonstrate the importance of priors on weak lensing mass accuracy. In the case of an assumed constant bias, b SZ , between true cluster mass, M 500 , and the Planck mass proxy, M PL , our analysis constrains 1 − b SZ = 0.73 ± 0.10 when moderate priors on weak lensing accuracy are used, including a zero-mean Gaussian with standard deviation of 8% to account for possible bias in lensing mass estimations. Our analysis explicitly accounts for possible selection bias effects in this calibration sourced by the CLASH selection function. Our constraint on the cluster mass scale is consistent with recent results from the Weighing the Giants program and the Canadian Cluster Comparison Project. It is also consistent, at 1.34σ, with the value needed to reconcile the Planck SZ cluster counts with Planck's base ΛCDM model fit to the primary cosmic microwave background anisotropies.

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Section: Discussionsupporting

confidence: 50%

Section: Discussionmentioning

confidence: 89%

Section: Resultsmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

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Calibrating thePlanckcluster mass scale with CLASH

Penna-Lima

Bartlett

Rozo

et al. 2017

A&A

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A space mission to map the entire observable universe using the CMB as a backlight

et al. 2021

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This Science White Paper, prepared in response to the ESA Voyage 2050 call for long-term mission planning, aims to describe the various science possibilities that can be realized with an L-class space observatory that is dedicated to the study of the interactions of cosmic microwave background (CMB) photons with the cosmic web. Our aim is specifically to use the CMB as a backlight – and survey the gas, total mass, and stellar content of the entire observable Universe by means of analyzing the spatial and spectral distortions imprinted on it. These distortions result from two major processes that impact on CMB photons: scattering by free electrons and atoms (Sunyaev-Zeldovich effect in diverse forms, Rayleigh scattering, resonant scattering) and deflection by gravitational potential (lensing effect). Even though the list of topics collected in this White Paper is not exhaustive, it helps to illustrate the exceptional diversity of major scientific questions that can be addressed by a space mission that will reach an angular resolution of 1.5 arcmin (goal 1 arcmin), have an average sensitivity better than 1 μK-arcmin, and span the microwave frequency range from roughly 50 GHz to 1 THz. The current paper also highlights the synergy of our Backlight mission concept with several upcoming and proposed ground-based CMB experiments.

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Constraints from thermal Sunyaev-Zel’dovich cluster counts and power spectrum combined with CMB

Salvati

Douspis

Aghanim

2018

A&A

129

122

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The thermal Sunyaev-Zel'dovich (tSZ) effect is one of the recent probes of cosmology and large-scale structures. We update constraints on cosmological parameters from galaxy clusters observed by the Planck satellite in a first attempt to combine cluster number counts and the power spectrum of hot gas; we used a new value of the optical depth and, at the same time, sampling on cosmological and scaling-relation parameters. We find that in the ΛCDM model, the addition of a tSZ power spectrum provides small improvements with respect to number counts alone, leading to the 68% c.l. constraints Ω m = 0.32 ± 0.02, σ 8 = 0.76 ± 0.03, and σ 8 (Ω m /0.3) 1/3 = 0.78 ± 0.03 and lowering the discrepancy with results for cosmic microwave background (CMB) primary anisotropies (updated with the new value of τ) to 1.8σ on σ 8 . We analysed extensions to the standard model, considering the effect of massive neutrinos and varying the equation of state parameter for dark energy. In the first case, we find that the addition of the tSZ power spectrum helps in improving cosmological constraints with respect to number count alone results, leading to the 95% upper limit m ν < 1.88 eV. For the varying dark energy equation of state scenario, we find no important improvements when adding tSZ power spectrum, but still the combination of tSZ probes is able to provide constraints, producing w = −1.0 ± 0.2. In all cosmological scenarios, the mass bias to reconcile CMB and tSZ probes remains low at (1 − b) 0.67 as compared to estimates from weak lensing and X-ray mass estimate comparisons or numerical simulations.

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The tau of galaxy clusters

Cited by 106 publications

References 95 publications

Calibrating thePlanckcluster mass scale with CLASH

Calibrating thePlanckcluster mass scale with CLASH

A space mission to map the entire observable universe using the CMB as a backlight

Constraints from thermal Sunyaev-Zel’dovich cluster counts and power spectrum combined with CMB

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