A Simple Physical Model for the Gas Distribution in Galaxy Clusters

Patej, Anna; Loeb, Abraham

doi:10.1088/2041-8205/798/1/l20

Cited by 18 publications

(16 citation statements)

References 28 publications

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“…Note that Tomooka et al (2020) also measured a sharp radial transition at the edge of galaxy clusters in the line-of-sight velocity dispersion of tracer galaxies around RM clusters in the SDSS spectroscopic survey. Also note that splashback-like features in individual clusters were discussed in previous studies (Rines et al 2013;Patej & Loeb 2015;Tully 2015).…”

Section: Introductionmentioning

confidence: 53%

The mass and galaxy distribution around SZ-selected clusters

Shin

Jain

Adhikari

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present measurements of the radial profiles of the mass and galaxy number density around Sunyaev-Zel’dovich (SZ)-selected clusters using both weak lensing and galaxy counts. The clusters are selected from the Atacama Cosmology Telescope Data Release 5 and the galaxies from the Dark Energy Survey Year 3 dataset. With signal-to-noise of 62 (45) for galaxy (weak lensing) profiles over scales of about 0.2 − 20h−1 Mpc, these are the highest precision measurements for SZ-selected clusters to date. Because SZ selection closely approximates mass selection, these measurements enable several tests of theoretical models of the mass and light distribution around clusters. Our main findings are: 1. The splashback feature is detected at a consistent location in both the mass and galaxy profiles and its location is consistent with predictions of cold dark matter N-body simulations. 2. The full mass profile is also consistent with the simulations. 3. The shapes of the galaxy and lensing profiles are remarkably similar for our sample over the entire range of scales, from well inside the cluster halo to the quasilinear regime. We measure the dependence of the profile shapes on the galaxy sample, redshift and cluster mass. We extend the Diemer & Kravtsov model for the cluster profiles to the linear regime using perturbation theory and show that it provides a good match to the measured profiles. We also compare the measured profiles to predictions of the standard halo model and simulations that include hydrodynamics. Applications of these results to cluster mass estimation, cosmology and astrophysics are discussed.

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Section: Introductionmentioning

confidence: 53%

The mass and galaxy distribution around SZ-selected clusters

Shin

Jain

Adhikari

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…In cross-correlation the combinations X-ray and tSZ observations have yielded stacked gas density profiles that go beyond R 500 (e.g., Planck Collaboration et al 2013a; Eckert et al 2012), for a sub-set of massive clusters. Beyond R 500 there are theoretical gas density profiles from analytic calculations (e.g., Komatsu & Seljak 2001;Ostriker et al 2005;Patej & Loeb 2015) and predictions from numerical simulations (e.g., Roncarelli et al 2006;Nagai et al 2007;Vazza et al 2010;Pike et al 2014), with some of simulations provided a fitting function to their results. Like most halo profiles simulations show that the gas density profile is close to self-similar, but recently it was shown that at large radii self-similarity is broken by the mass accretion history of the halo (Lau et al 2015).…”

Section: Agn Feedbackmentioning

confidence: 99%

The tau of galaxy clusters

Battaglia

2016

J. Cosmol. Astropart. Phys.

109

161

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The recent emergence of detections of the kinetic Sunyaev-Zel'dovich (kSZ) effect through crosscorrelation techniques is encouraging for the prospects of future cosmic microwave background (CMB) experiments. Extracting information on the large-scale velocity fields and constraining cosmological parameters from such kSZ measurements requires an understanding of the optical depth to CMB photons through halos. Using cosmological hydrodynamic simulations we find that there exists a low-scatter relation between the optical depth and thermal Sunyaev-Zel'dovich (tSZ) signal of halos within a physical aperture. We propose that such a relation can be used to break the degeneracy between optical depth and line-of-sight velocity in kSZ measurements. The limiting factors in our proposal are systematic uncertainties associated with the sub-grid physics models in the simulations, which we calculate to be less than 10 percent. We discuss future observational measurements that could potentially be used to mitigate the systematic uncertainties in this scaling relation.

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“…Meanwhile, the gas density profile ρ gas (r) is described with the model proposed by Patej & Loeb (2015) ρ gas (r) = Γf gas r r shock…”

Section: Spatial Distributions Of Gas Mass and Total Gravitational Massmentioning

confidence: 99%

The Merger Dynamics of the Galaxy Cluster Abell 1775: New Insights from Chandra and XMM-Newton for a Cluster Simultaneously Hosting a WAT and a NAT Radio Sources

Hu,

Xu,

Zhu

et al. 2021

Preprint

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We present a new study of the merger dynamics of Abell 1775 by analyzing the high-quality Chandra and XMM-Newton archival data. We confirm/identify an arc-shaped edge (i.e., the head) at ∼ 48 kpc west of the X-ray peak, a split cold gas tail that extends eastward to ∼ 163 kpc, and a plume of spiral-like X-ray excess (within about 81 − 324 kpc northeast of the cluster core) that connects to the end of the tail. The head, across which the projected gas temperature rises outward from 3.39 +0.28 −0.18 keV to 5.30 +0.54 −0.43 keV, is found to be a cold front with a Mach number of M ∼ 0.79. Along the surfaces of the cold front and tail, typical KHI features (noses and wings, etc.) are found and are used to constrain the upper limit of the magnetic field (∼ 11.2 µG) and the viscosity suppression factor (∼ 0.01). Combining optical and radio evidence we propose a two-body merger (instead of systematic motion in a large-scale gas environment) scenario and have carried out idealized hydrodynamic simulations to verify it. We find that the observed X-ray emission and temperature distributions can be best reproduced with a merger mass ratio of 5 after the first pericentric passage. The NAT radio galaxy is thus more likely to be a single galaxy falling into the cluster center at a relative velocity of 2800 km s −1 , a speed constrained by its radio morphology. The infalling subcluster is expected to have a relatively low gas content, because only a gas-poor subcluster can cause central-only disturbances as observed in such an off-axis merger.

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A Simple Physical Model for the Gas Distribution in Galaxy Clusters

Cited by 18 publications

References 28 publications

The mass and galaxy distribution around SZ-selected clusters

The mass and galaxy distribution around SZ-selected clusters

The tau of galaxy clusters

The Merger Dynamics of the Galaxy Cluster Abell 1775: New Insights from Chandra and XMM-Newton for a Cluster Simultaneously Hosting a WAT and a NAT Radio Sources

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