Cluster Outskirts and Their Connection to the Cosmic Web

Walker, Stephen; Lau, Erwin T.

doi:10.1007/978-981-16-4544-0_120-1

Handbook of X-Ray and Gamma-Ray Astrophysics 2022

DOI: 10.1007/978-981-16-4544-0_120-1

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Cluster Outskirts and Their Connection to the Cosmic Web

Stephen Walker

Erwin T. Lau

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Cited by 5 publications

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“…This concept of gas clumping is supported by simulations, which have shown that the distribution of the density of the ICM in the outskirts tends to be non-uniform (Nagai & Lau 2011 ). While interfering with the ability to accurately measure entropy, gas clumping in the outskirts is also of interest due to its likely role in the physics and evolution of galaxy clusters (Walker & Lau 2022 ). It is therefore important for gas clumps to be directly identified, characterized, and ultimately masked out to reco v er the true entropy profile of the diffuse gas and properly test our current understanding of the evolution of the ICM in galaxy clusters.…”

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confidence: 96%

Gas clumping in the outskirts of galaxy clusters, an assessment of the sensitivity ofSTAR-X

Norseth,

Wik,

ZuHone

et al. 2023

RAS Techniques and Instruments

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In the outskirts of galaxy clusters, entropy profiles measured from X-ray observations of the hot intracluster medium (ICM) drops off unexpectedly. One possible explanation for this effect is gas clumping, where pockets of cooler and denser structures within the ICM are present. Current observatories are unable to directly detect these hypothetical gas clumps. One of the science drivers of the proposed STAR-X observatory is to resolve these or similar structures. Its high spatial resolution, large effective area, and low instrumental background make STAR-X ideal for directly detecting and characterizing clumps and diffuse emission in cluster outskirts. The aim of this work is to simulate observations of clumping in clusters to determine how well STAR-X will be able to detect clumps, as well as what clumping properties reproduce observed entropy profiles. This is achieved by using yt, pyXSIM, SOXS, and other tools to inject ideally modeled clumps into three-dimensional models derived from actual clusters using their observed profiles from other X-ray missions. Radial temperature and surface brightness profiles are then extracted from mock observations using concentric annuli. We find that in simulated observations for STAR-X, a parameter space of clump properties exists where gas clumps can be successfully identified using wavdetect and masked, and are able to recover the true cluster profiles. This demonstrates that STAR-X could be capable of detecting substructure in the outskirts of nearby clusters and that the properties of both the outskirts and the clumps will be revealed.

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mentioning

confidence: 96%

Gas clumping in the outskirts of galaxy clusters, an assessment of the sensitivity ofSTAR-X

Norseth,

Wik,

ZuHone

et al. 2023

RAS Techniques and Instruments

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Cosmic accretion shocks as a tool to measure the dark matter mass of galaxy clusters

Vallés-Pérez,

Quilis,

Planelles

2024

Nat Astron

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X-ray surface brightness and gas density profiles of galaxy clusters up to 3 × R500c with SRG/eROSITA

Lyskova

Churazov

Khabibullin

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Using the data of the SRG/eROSITA all-sky survey, we stacked a sample of ∼40 galaxy cluster images in the 0.3–2.3 keV band, covering the radial range up to 10 × R500c. The excess emission on top of the Galactic and extragalactic X-ray backgrounds and foregrounds is detected up to ∼3 × R500c. At these distances, the surface brightness of the stacked image drops below ∼1% of the background. The density profile reconstructed from the X-ray surface brightness profile agrees well (within ∼30%) with the mean gas profile found in numerical simulations, which predict the local gas overdensity of ∼ 20–30 at 3 × R500c and the gas fraction close to the universal value of $\frac{\Omega _b}{\Omega _m}\approx 0.15$ in the standard ΛCDM model. Taking at face value, this agreement suggests that up to ∼3 × R500c the X-ray signal is not strongly boosted by the gas clumpiness, although a scenario with a moderately inhomogeneous gas cannot be excluded. A comparison of the derived gas density profile with the electron pressure profile based on the SZ measurements suggests that by r ∼ 3 × R500c the gas temperature drops by a factor of ∼ 4–5 below the characteristic temperature of a typical cluster in the sample within R500c, while the entropy keeps growing up to this distance. Better constraints on the gas properties just beyond 3 × R500c should be possible with a sample larger than used for this pilot study.

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Cluster Outskirts and Their Connection to the Cosmic Web

Cited by 5 publications

References 94 publications

Gas clumping in the outskirts of galaxy clusters, an assessment of the sensitivity ofSTAR-X

Gas clumping in the outskirts of galaxy clusters, an assessment of the sensitivity ofSTAR-X

Cosmic accretion shocks as a tool to measure the dark matter mass of galaxy clusters

X-ray surface brightness and gas density profiles of galaxy clusters up to 3 × R500c with SRG/eROSITA

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