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

Hurier, G.; Angulo, Raúl E.

doi:10.1051/0004-6361/201731999

Cited by 27 publications

(20 citation statements)

References 41 publications

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“…A similar offset between the Planck clusters and the fable relation persists to higher redshift, although at z ≥ 0.6 we rely on the extrapolation of the best-fitting relation as there are few, if any, fable systems as massive as the Planck clusters. This suggests that the X-ray mass bias remains at a similar level with increasing redshift, as found for example in Nagai et al (2007a), Henson et al (2017) and Hurier & Angulo (2018).…”

Section: Comparison With Planck and Sptsupporting

confidence: 68%

“…Gruen et al 2014;Israel et al 2014;Smith et al 2016;Applegate et al 2016) while others find that X-ray hydrostatic masses are biased low compared to weak lensing masses by ∼ 25-30 per cent within r500 (e.g. Donahue et al 2014;von der Linden et al 2014;Hoekstra et al 2015;Sereno et al 2017;Simet et al 2017;Hurier & Angulo 2018). In addition, cosmological constraints from cluster abundance studies seem to require an even larger X-ray mass bias of ∼ 40 per cent in order to reconcile their results with Planck measurements of the primary CMB (Planck Collaboration XXIV 2016; Salvati et al 2018).…”

Section: Comparison To Observationsmentioning

confidence: 99%

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The redshift evolution of X-ray and Sunyaev–Zel’dovich scaling relations in the fable simulations

Henden

Puchwein

Sijacki

2019

Monthly Notices of the Royal Astronomical Society

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We study the redshift evolution of the X-ray and Sunyaev-Zel'dovich (SZ) scaling relations for galaxy groups and clusters in the fable suite of cosmological hydrodynamical simulations. Using an expanded sample of 27 high-resolution zoom-in simulations, together with a uniformly-sampled cosmological volume to sample low-mass systems, we find very good agreement with the majority of observational constraints up to z ∼ 1. We predict significant deviations of all examined scaling relations from the simple self-similar expectations. While the slopes are approximately independent of redshift, the normalisations evolve positively with respect to self-similarity, even for commonly-used mass proxies such as the Y X parameter. These deviations are due to a combination of factors, including more effective AGN feedback in lower mass haloes, larger binding energy of gas at a given halo mass at higher redshifts and larger nonthermal pressure support from kinetic motions at higher redshifts. Our results have important implications for cluster cosmology from upcoming SZ surveys such as SPT-3G, ACTpol and CMB-S4, as relatively small changes in the observable-mass scaling relations (within theoretical uncertainties) have a large impact on the predicted number of high-redshift clusters and hence on our ability to constrain cosmology using cluster abundances. In addition, we find that the intrinsic scatter of the relations, which agrees well with most observational constraints, increases at lower redshifts and for lower mass systems. This calls for a more complex parametrization than adopted in current observational studies to be able to accurately account for selection biases.

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Section: Comparison With Planck and Sptsupporting

confidence: 68%

Section: Comparison To Observationsmentioning

confidence: 99%

The redshift evolution of X-ray and Sunyaev–Zel’dovich scaling relations in the fable simulations

Henden

Puchwein

Sijacki

2019

Monthly Notices of the Royal Astronomical Society

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“…The primary bias is not actually the hydrostatic equilibrium assumption, but rather that the pressure gradient used only accounts for thermal pressure. Thus, the lack of account for non-thermal pressure under-estimates the mass by 10% to 30% (see also Biffi et al 2016;Khatri & Gaspari 2016;Hurier & Angulo 2018;Ettori et al 2019).…”

Section: Mass Estimatesmentioning

confidence: 99%

Pressure Profiles and Mass Estimates Using High-resolution Sunyaev–Zel’dovich Effect Observations of Zwicky 3146 with MUSTANG-2

Romero

Sievers

Ghirardini

et al. 2020

ApJ

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The galaxy cluster Zwicky 3146 is a sloshing cool core cluster at z = 0.291 that in X-ray imaging does not appear to exhibit significant pressure substructure in the intracluster medium (ICM). The published M 500 values range between 3.88 +0.62 −0.58 to 22.50 ± 7.58 × 10 14 M , where ICM-based estimates with reported errors < 20% suggest that we should expect to find a mass between 6.53 +0.44 −0.44 × 10 14 M (from Planck, with an 8.4σ detection) and 8.52 +1.77 −1.47 × 10 14 M (from ACT, with a 14σ detection). This broad range of masses is suggestive that there is ample room for improvement for all methods. Here, we investigate the ability to estimate the mass of Zwicky 3146 via the Sunyaev-Zel'dovich (SZ) effect with data taken at 90 GHz by MUSTANG-2 to a noise level better than 15 µK at the center, and a cluster detection of 104σ. We derive a pressure profile from our SZ data which is in excellent agreement with that derived from X-ray data. From our SZ-derived pressure profiles, we infer M 500 and M 2500 via three methods -Y -M scaling relations, the virial theorem, and hydrostatic equilibrium -where we employ X-ray constraints from XMM-Newton on the electron density profile when assuming hydrostatic equilibrium. Depending on the model and estimation method, our M 500 estimates range from 6.23 ± 0.59 to 10.6 ± 0.95 × 10 14 M , where our estimate from hydrostatic equilibrium, is 8.29 +1.93 −1.24 (±19.1% stat) +0.74 −0.68 (±8.6% sys, calibration) ×10 14 M . Our fiducial mass, derived from a Y -M relation is 8.16 +0.44 −0.54 (±5.5% stat) +0.46 −0.43 (±5.5% sys, Y -M ) +0.59 −0.55 (±7.0% sys, cal.) ×10 14 M . We investigate the consistency of our mass estimates and potential for otherwise unaddressed systematic errors within the MUSTANG-2 data. The inconsistencies among our mass estimates are not well explained by a potential systematic error in the MUSTANG-2 data.

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“…Instead, at the virial radius, the analysis with the gas density not corrected for clumpiness gives an underestimation of ∼ 40%, while is ∼ 20% using the gas density corrected for clumpiness. The last value is in the range (10-30)% usually reported in literature (see Biffi et al 2016;Khatri & Gaspari 2016: Hurier & Angulo 2018.…”

Section: Discussionmentioning

confidence: 59%

SuperModel predictions in the outskirts of the galaxy cluster Zwicky 3146

Fusco-Femiano

2020

Monthly Notices of the Royal Astronomical Society

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The relaxed galaxy cluster Zwicky 3146 is analyzed via the SuperModel, a tool already tested on many clusters since 2009. In particular, this analysis is focused on the intracluster medium X-ray temperature data measured by XMM-Newton up to r 500 . A previous analysis was based on the temperature profile derived from the Sunyaev-Zeld ′ ovich effect pressure data. The gas mass fraction f gas is obtained from the resulting SuperModel temperature profile extrapolated up to the virial radius R, that turns out in agreement with the steep temperature profiles observed by Suzaku, and from the gas density profile observed by XMM-Newton. The comparison between f gas with the universal value indicates a non-thermal pressure component, p nth , in the cluster outskirts. The SuperModel analysis shows a ratio α(R) (≃ 50%) of p nth to the total pressure greater than the values found by simulations, highlighting the possible presence of accreting substructures and inhomogeneities in the gas density profile. Once that this profile is corrected for clumpiness, the level of p nth is considerably reduced. However, a significant turbulence (α(R) ≃ 20%) and entropy flattening are still present in the outskirts of the galaxy cluster Zwicky 3146.

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

Cited by 27 publications

References 41 publications

The redshift evolution of X-ray and Sunyaev–Zel’dovich scaling relations in the fable simulations

The redshift evolution of X-ray and Sunyaev–Zel’dovich scaling relations in the fable simulations

Pressure Profiles and Mass Estimates Using High-resolution Sunyaev–Zel’dovich Effect Observations of Zwicky 3146 with MUSTANG-2

SuperModel predictions in the outskirts of the galaxy cluster Zwicky 3146

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