Galaxy cluster rotation revealed in the MACSIS simulations with the kinetic Sunyaev–Zeldovich effect

Altamura, Edoardo; Kay, Scott T.; Chluba, Jens; Towler, Imogen

doi:10.1093/mnras/stad1841

Cited by 7 publications

(2 citation statements)

References 103 publications

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“…In a series of recent works, SZ and X-ray studies have been suggested to constrain models of baryonic physics, and specifically the role of AGN feedback in determining the thermodynamic properties of the ICM (e.g., Acharya et al 2021;Eckert et al 2021;Chadayammuri et al 2022;Kar Chowdhury et al 2022;Kim et al 2022;Yang et al 2022;Altamura et al 2023). In a previous study, Brownson et al (2019) proposed using the FABLE cosmological simulations and that ALMA has the potential to constrain AGN feedback models through SZ observations.…”

Section: Discussion Of Resultsmentioning

confidence: 99%

Cosmological Simulations of Galaxy Groups and Clusters. III. Constraining Quasar Feedback Models with the Atacama Large Millimeter Array

Chakraborty,

Chatterjee,

Lacy

et al. 2023

ApJ

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The thermal Sunyaev–Zeldovich (SZ) effect serves as a direct potential probe of the energetic outflows from quasars that are responsible for heating the intergalactic medium. In this work, we use the GIZMO meshless finite mass hydrodynamic cosmological simulation SIMBA, which includes different prescriptions for quasar feedback, to compute the SZ effect arising from different feedback modes. From these theoretical simulations, we perform mock observations of the Atacama Large Millimeter Array (ALMA) in four bands (320, 135, 100, and 42 GHz) to characterize the feasibility of direct detection of the quasar SZ signal. Our results show that for all the systems we get an enhancement of the SZ signal, when there is radiative feedback, while the signal gets suppressed when the jet mode of feedback is introduced in the simulations. Our mock ALMA maps reveal that, with the current prescription of jet feedback, the signal goes below the detection threshold of ALMA. We also find that the signal is higher for high redshift systems, making it possible for ALMA and cross SZ-X-ray studies to disentangle the varying modes of quasar feedback and their relative importance in the cosmological context.

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Section: Discussion Of Resultsmentioning

confidence: 99%

Cosmological Simulations of Galaxy Groups and Clusters. III. Constraining Quasar Feedback Models with the Atacama Large Millimeter Array

Chakraborty,

Chatterjee,

Lacy

et al. 2023

ApJ

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“…When working with real data, this technique will also help in removing the bias due to the CIB, as well as any other foregrounds correlated with the clusters under study. We did not include the effects of the rotational kSZ [78][79][80][81] or the moving-lens effect [82,83], which are also expected to produce a dipole signal. However, the orientation of the dipole will be aligned along the direction of the cluster rotation in the former and the direction of the large-scale velocity field in the latter, which are both not correlated with the direction of the background CMB gradient.…”

Section: Discussionmentioning

confidence: 99%

A foreground-immune CMB-cluster lensing estimator

Levy,

Raghunathan,

Basu

2023

J. Cosmol. Astropart. Phys.

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Galaxy clusters induce a distinct dipole pattern in the cosmic microwave back-ground (CMB) through the effect of gravitational lensing. Extracting this lensing signal will enable us to constrain cluster masses, even for high redshift clusters (z ≳ 1) that are expected to be detected by future CMB surveys. However, cluster-correlated foreground signals, like the kinematic and thermal Sunyaev-Zel'dovich (kSZ and tSZ) signals, present a challenge when extracting the lensing signal from CMB temperature data. While CMB polarization-based lensing reconstruction is one way to mitigate these foreground biases, the sensitivity from CMB temperature-based reconstruction is expected to be similar to or higher than polarization for future surveys. In this work, we extend the cluster lensing estimator developed in [1] to CMB temperature and test its robustness against systematic biases from foreground signals. We find that the kSZ signal only acts as an additional source of variance and provide a simple stacking-based approach to mitigate the bias from the tSZ signal. Additionally, we study the bias induced due to uncertainties in the cluster positions and show that they can be easily mitigated. The estimated signal-to-noise ratio (SNR) of this estimator is comparable to other standard lensing estimators such as the maximum likelihood (MLE) and quadratic (QE) estimators. We predict the cluster mass uncertainties from CMB temperature data for current and future cluster samples to be: 6.6% for SPT-3G with 7,000 clusters, 4.1% for SO and 3.9% for SO + FYST with 25,000 clusters, and 1.8% for CMB-S4 with 100,000 clusters.

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Gas rotation and dark matter halo shape in cool-core clusters of galaxies

Bartalesi,

Ettori,

Nipoti

2024

A&A

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We study the possibility that the gas in cool-core clusters of galaxies has non-negligible rotation support, the impact of gas rotation on mass estimates from current X-ray observations, and the ability of forthcoming X-ray observatories to detect such rotation. We present three representative models of massive cool-core clusters with a rotating intracluster medium (ICM) in equilibrium in cosmologically motivated spherical, oblate, or prolate dark matter halos, represented by physical density-potential pairs. In the models, the gas follows a composite-polytropic distribution, and has rotation velocity profiles consistent with current observational constraints and similar to those found in clusters formed in cosmological simulations. We show that the models are consistent with available measurements of the ICM properties of the massive cluster population: the thermodynamic profiles, the shape of the surface brightness distribution, the hydrostatic mass bias, and the broadening of X-ray emitting lines. Using the configuration for the microcalorimeter onboard the XRISM satellite, we generated a set of mock X-ray spectra for our cluster models, which we then analyzed to make predictions about the rotation speed that will be obtained with such an instrument. We then assessed what fraction of the hydrostatic mass bias of our models could be accounted for by detecting the rotation speed with XRISM spectroscopy over the range $(0.1-1)r_ $, sampled with three nonoverlapping pointings. Current data leave room for the rotating ICM in cool-core clusters, with peaks in the rotation speed as high as $600\ km/s $. We show that such rotation, if present, will be detected with upcoming X-ray facilities such as XRISM and that $60-70<!PCT!>$ of the hydrostatic mass bias due to rotation can be accounted for using the line-of-sight velocity measured from X-ray spectroscopy with XRISM with a residual bias smaller than $3<!PCT!>$ at an overdensity of 500. In this way XRISM will allow us to pin down any mass bias of a different origin from the rotation.

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Galaxy cluster rotation revealed in the MACSIS simulations with the kinetic Sunyaev–Zeldovich effect

Cited by 7 publications

References 103 publications

Cosmological Simulations of Galaxy Groups and Clusters. III. Constraining Quasar Feedback Models with the Atacama Large Millimeter Array

Cosmological Simulations of Galaxy Groups and Clusters. III. Constraining Quasar Feedback Models with the Atacama Large Millimeter Array

A foreground-immune CMB-cluster lensing estimator

Gas rotation and dark matter halo shape in cool-core clusters of galaxies

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