Cosmological constraints from gas mass fractions of massive, relaxed galaxy clusters

Mantz, Adam; Morris, R. Glenn; Allen, S. W.; Canning, Rebecca; Baumont, Lucie; Benson, B. A.; Bleem, Lindsey; Castellano, Simone; Floyd, Benjamin; Herbonnet, Ricardo; Kelly, Patrick L.; Liang, Shuang; Linden, Anja von der; McDonald, Michael; Rapetti, David; Schmidt, Robert W.; Werner, Norbert; Wright, Adam

doi:10.1093/mnras/stab3390

Cited by 35 publications

(25 citation statements)

References 79 publications

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“…The correlation signal identified in our work is relatively moderate. Our work supports the premise that BCG information, such as that indicated in Figure 7, could be used to benefit weak-lensing mass constraints of relaxed clusters for work such as Mantz et al (2022).…”

Section: Discussionsupporting

confidence: 80%

Brightest cluster galaxies trace weak lensing mass bias and halo triaxiality in the three hundred project

Herbonnet

Crawford

Avestruz

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Galaxy clusters have a triaxial matter distribution. The weak-lensing signal, an important part in cosmological studies, measures the projected mass of all matter along the line-of-sight, and therefore changes with the orientation of the cluster. Studies suggest that the shape of the brightest cluster galaxy (BCG) in the centre of the cluster traces the underlying halo shape, enabling a method to account for projection effects. We use 324 simulated clusters at four redshifts between 0.1 and 0.6 from ‘The Three Hundred Project’ to quantify correlations between the orientation and shape of the BCG and the halo. We find that haloes and their embedded BCGs are aligned, with an average ∼20 degree angle between their major axes. The bias in weak lensing cluster mass estimates correlates with the orientation of both the halo and the BCG. Mimicking observations, we compute the projected shape of the BCG, as a measure of the BCG orientation, and find that it is most strongly correlated to the weak-lensing mass for relaxed clusters. We also test a 2-dimensional cluster relaxation proxy measured from BCG mass isocontours. The concentration of stellar mass in the projected BCG core compared to the total stellar mass provides an alternative proxy for the BCG orientation. We find that the concentration does not correlate to the weak-lensing mass bias, but does correlate with the true halo mass. These results indicate that the BCG shape and orientation for large samples of relaxed clusters can provide information to improve weak-lensing mass estimates.

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Section: Discussionsupporting

confidence: 80%

Brightest cluster galaxies trace weak lensing mass bias and halo triaxiality in the three hundred project

Herbonnet

Crawford

Avestruz

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…[169] finds H 0 = (70.1 ± 0.8) km s −1 Mpc −1 at 68% CL, or using another sample containing 38 data points H 0 = (74.6 ± 2.1) km s −1 Mpc −1 at 68% CL. This measurement is very sensitive to the temperature calibration and a more conservative analysis gives H 0 = 67.3 +21.3 −13.3 km s −1 Mpc −1 at 68% CL, where errors are dominated by uncertainties of the temperature calibration [170], and H 0 = 72.2 +6.7 −6.7 km s −1 Mpc −1 at 68% CL [171].…”

Section: A Late H0 Measurementsmentioning

confidence: 95%

Cosmology Intertwined: A Review of the Particle Physics, Astrophysics, and Cosmology Associated with the Cosmological Tensions and Anomalies

Abdalla,

Abellán,

Aboubrahim

et al. 2022

Preprint

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This White Paper has been prepared to fulfill SNOWMASS 2021 requirements and it extends the material previously summarized in the four Letters of Interest [1][2][3][4]. The Particle Physics Community Planning Exercise (a.k.a. SNOWMASS ) is organized by the Division of Particles and Fields of the American Physical Society, and this is an effort to bring together the community of theoretical physicists and cosmologists and identify promising opportunities to address the questions described.This White Paper was initiated with the aim of identifying the opportunities in the cosmological field for the next decade, and strengthening the coordination of the community. It is addressed to identifying the most promising directions of investigation, and rather than attempting a long review of the current status of the whole field of research, it focuses on the upcoming theoretical opportunities and challenges described. The White Paper is a collaborative effort led by Eleonora Di Valentino and Luis Anchordoqui, and it is organized in the topics listed below, each of them coordinated by the scientists indicated (alphabetical order):

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“…Note that these constraints will be improved compared to those obtained in existing cluster counts in X-ray, Microwave, and Optical cluster surveys (Vikhlinin et al 2009;Mantz et al 2010;Benson et al 2013;Mantz et al 2022), the constraints from cross X-ray and SZ power spectrum measurements with ROSAT-Planck (Hurier et al 2015); and they will be comparable with upcoming cluster count constraints from eRASS (Pillepich et al 2018). 5 At this point, it is not clear whether eRASS8 will be completed.…”

Section: Cosmological Forecasts For Erosita All Sky Surveymentioning

confidence: 77%

The X-ray Angular Power Spectrum of Extended Sources in the eROSITA Final Equatorial Depth Survey

Lau¹,

Bogdán²,

Chadayammuri³

et al. 2022

Preprint

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The eROSITA Final Equatorial Depth Survey (eFEDS), with a sky area of 140 square degrees with depth equivalent to the equatorial patch of the final eROSITA all-sky survey, represents the largest continuous non full-sky X-ray fields to-date, making it the premier dataset for measuring the angular power spectrum. In this work, we measure the X-ray angular power spectrum of galaxy clusters and groups in the eFEDS field. We show that the measured power spectrum at large angular scales (multipole ℓ < 2000) is consistent with that of the ROSAT All Sky Survey, as well as the predictions of cluster gas halo model that is calibrated from Chandra observations of galaxy clusters. At small angular scales (ℓ > 2000) , the eFEDS power spectrum is around an order of magnitude higher than the power spectrum of the Chandra/COSMOS field, and the halo model prediction. A follow-up of the impact of point source contamination with the higher angular resolution instruments like Chandra will resolve this tension. If we restrict the angular scales where eFEDS power agrees with observations and model predictions, we show that the X-ray power spectrum from the upcoming eROSITA all sky data can achieve percent-level constraints on Ω 𝑀 and 𝜎8, which are competitive to other cosmological probes.

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Cosmological constraints from gas mass fractions of massive, relaxed galaxy clusters

Cited by 35 publications

References 79 publications

Brightest cluster galaxies trace weak lensing mass bias and halo triaxiality in the three hundred project

Brightest cluster galaxies trace weak lensing mass bias and halo triaxiality in the three hundred project

Cosmology Intertwined: A Review of the Particle Physics, Astrophysics, and Cosmology Associated with the Cosmological Tensions and Anomalies

The X-ray Angular Power Spectrum of Extended Sources in the eROSITA Final Equatorial Depth Survey

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