Next Generation Virgo Cluster Survey. XXI. The Weak Lensing Masses of the CFHTLS and NGVS RedGOLD Galaxy Clusters and Calibration of the Optical Richness

Parroni, Carolina; Mei, S.; Erben, T.; Waerbeke, Ludovic Van; Raichoor, Anand; Ford, Jason C.; Licitra, R.; Meneghetti, M.; Hildebrandt, Hendrik; Miller, L.; Côté, Patrick; Covone, G.; Cuillandre, Jean-Charles; Duc, Pierre–Alain; Ferrarese, Laura; Gwyn, Stephen; Puzia, Thomas H.

doi:10.3847/1538-4357/aa8b6c

Cited by 10 publications

(9 citation statements)

References 124 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…This value is consistent within 1σ with previous analyses performed on CMB weak lensing (Melin & Bartlett 2015), and gives slightly higher results than previous galaxy-galaxy weak-lensing based analyses, but the results are still consistent (see e.g. Medezinski et al 2018;Sereno et al 2017;Jimeno et al 2017;Parroni et al 2017;Battaglia et al 2016;Applegate et al 2016;Smith et al 2016;Hoekstra et al 2015;Simet et al 2015;Israel et al 2015;von der Linden et al 2014;Donahue et al 2014;Gruen et al 2014;Mahdavi et al 2013. This value for b is also consistent with previous results obtained from the tSZ analysis performed in Hurier & Lacasa (2017), but it favours slightly lower values than the combined analysis of CMB and tSZ performed by Salvati et al (2017).…”

Section: Measurement Of the Hydrostatic Mass Biassupporting

confidence: 81%

“…Medezinski et al 2018;Sereno et al 2017;Jimeno et al 2017;Parroni et al 2017;Battaglia et al 2016;Applegate et al 2016;Smith et al 2016;Hoekstra et al 2015;Simet et al 2015;Israel et al 2015;von der Linden et al 2014;Donahue et al 2014;Gruen et al 2014;Mahdavi et al 2013). These studies, mostly relying on assumptions of unbiased weak-lensing mass estimates, obtained b 0.20 ± 0.08.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Measuring the hydrostatic mass bias in galaxy clusters by combining Sunyaev–Zel’dovich and CMB lensing data

Hurier

Angulo

2018

A&A

View full text Add to dashboard Cite

The cosmological parameters preferred by the cosmic microwave background (CMB) primary anisotropies predict many more galaxy clusters than those that have been detected via the thermal Sunyaev-Zeldovich (tSZ) effect. This discrepancy has attracted considerable attention since it might be evidence of physics beyond the simplest ΛCDM model. However, an accurate and robust calibration of the mass-observable relation for clusters is necessary for the comparison, which has been proven difficult to obtain so far. Here, we present new constraints on the mass-pressure relation by combining tSZ and CMB lensing measurements of optically selected clusters. Consequently, our galaxy cluster sample is independent of the data employed to derive cosmological constrains. We estimate an average hydrostatic mass bias of b = 0.26 ± 0.07, with no significant mass or redshift evolution. This value greatly reduces the discrepancy between the predictions of ΛCDM and the observed abundance of tSZ clusters but agrees with recent estimates from tSZ clustering. On the other hand, our value for b is higher than the predictions from hydrodynamical simulations. This suggests mechanisms that drive large departures from hydrostatic equilibrium and that are not included in the latest simulations, and/or unaccounted systematic errors such as biases in the cluster catalogue that are due to the optical selection.

show abstract

Section: Measurement Of the Hydrostatic Mass Biassupporting

confidence: 81%

Section: Introductionmentioning

confidence: 99%

Measuring the hydrostatic mass bias in galaxy clusters by combining Sunyaev–Zel’dovich and CMB lensing data

Hurier

Angulo

2018

A&A

View full text Add to dashboard Cite

show abstract

“…Assuming that WL reconstruction provides unbiased estimates of the true mass, many teams derived bias estimates (e.g. Medezinski et al 2018;Sereno et al 2017;Jimeno et al 2018;Parroni et al 2017;Battaglia et al 2016;Applegate et al 2016;Smith et al 2016;Hoekstra et al 2015;Simet et al 2015;Israel et al 2015;von der Linden et al 2014;Donahue et al 2014;Gruen et al 2014;Mahdavi et al 2013, shown as black dots, from top to bottom, in Fig. 10).…”

Section: Discussionmentioning

confidence: 99%

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

Salvati

Douspis

Aghanim

2018

A&A

133

122

View full text Add to dashboard Cite

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.

show abstract

“…The slopes we derived for the mass-amplitude relation (1.99± 0.10) and the mass-richness relation (1.71 ± 0.08) are significantly larger than typical results in literature about calibration of photometric observables. For example, the logarith- mic dependence of the weak lensing mass on the richness λ provided by redMaPPer has been found to be 1.12 ± 0.26 in Melchior et al (2017) and 1.33 +0.09 −0.10 by Simet et al (2017), while Parroni et al (2017) derived a slope 1.02 ± 0.21 for the calibration of RedGOLD λ. This likely depends on the fact that AMICO uses a fixed radius in the definition of its observables, as already discussed in Section 5.3 of Bellagamba et al (2018): clusters bigger than the model are cut by the kernel, smaller ones are slightly enhanced by correlated large-scale structure.…”

Section: Slope Of the Mass-observable Relationmentioning

confidence: 99%

AMICO galaxy clusters in KiDS-DR3: weak lensing mass calibration

Bellagamba

Sereno

Roncarelli

et al. 2019

Monthly Notices of the Royal Astronomical Society

Self Cite

131

View full text Add to dashboard Cite

We present the mass calibration for galaxy clusters detected with the AMICO code in KiDS DR3 data. The cluster sample comprises ∼ 7000 objects and covers the redshift range 0.1 < z < 0.6. We perform a weak lensing stacked analysis by binning the clusters according to redshift and two different mass proxies provided by AMICO, namely the amplitude A (measure of galaxy abundance through an optimal filter) and the richness λ * (sum of membership probabilities in a consistent radial and magnitude range across redshift). For each bin, we model the data as a truncated NFW profile plus a 2-halo term, taking into account uncertainties related to concentration and miscentring. From the retrieved estimates of the mean halo masses, we construct the A-M 200 and the λ * -M 200 relations. The relations extend over more than one order of magnitude in mass, down to M 200 ∼ 2 (5) × 10 13 M /h at z = 0.2 (0.5), with small evolution in redshift. The logarithmic slope is ∼ 2.0 for the A-mass relation, and ∼ 1.7 for the λ * -mass relation, consistent with previous estimations on mock catalogues and coherent with the different nature of the two observables.

show abstract

Next Generation Virgo Cluster Survey. XXI. The Weak Lensing Masses of the CFHTLS and NGVS RedGOLD Galaxy Clusters and Calibration of the Optical Richness

Cited by 10 publications

References 124 publications

Measuring the hydrostatic mass bias in galaxy clusters by combining Sunyaev–Zel’dovich and CMB lensing data

Measuring the hydrostatic mass bias in galaxy clusters by combining Sunyaev–Zel’dovich and CMB lensing data

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

AMICO galaxy clusters in KiDS-DR3: weak lensing mass calibration

Contact Info

Product

Resources

About