Constraining the inner density slope of massive galaxy clusters

He, Qiuhan; Li, Hongyu; Li, Ran; Frenk, Carlos S.; Schaller, Matthieu; Barnes, David J.; Bahé, Yannick M.; Kay, Scott T.; Gao, Liang; Vecchia, Claudio Dalla

doi:10.1093/mnras/staa1769

Cited by 26 publications

(21 citation statements)

References 68 publications

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“…In general, it is non-trivial to infer the DM distribution from observations (e.g. Kowalczyk et al 2013;Harvey et al 2018;Oman et al 2019;Genina et al 2020;He et al 2020) and it is important to test how these difficulties impact the inferred SIDM cross-section when isothermal Jeans modelling is applied to observations. This was recently done in the context of galaxy cluster observations by Sagunski et al (2020), who found that the inferred cross-section from isothermal Jeans modelling using mock observations of simulated clusters was in agreement with the crosssection used in the simulations.…”

Section: Discussion a N D O U T L O O Kmentioning

confidence: 99%

The surprising accuracy of isothermal Jeans modelling of self-interacting dark matter density profiles

Robertson

Massey

Eke

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Recent claims of observational evidence for self-interacting dark matter (SIDM) have relied on a semi-analytic method for predicting the density profiles of galaxies and galaxy clusters containing SIDM. We present a thorough description of this method, known as isothermal Jeans modelling, and then test it with a large ensemble of haloes taken from cosmological simulations. Our simulations were run with cold and collisionless dark matter (CDM) as well as two different SIDM models, all with dark matter only variants as well as versions including baryons and relevant galaxy formation physics. Using a mix of different box sizes and resolutions, we study haloes with masses ranging from 3 × 1010 to $3 \times 10^{15} \mathrm{\, M_\odot }$. Overall, we find that the isothermal Jeans model provides as accurate a description of simulated SIDM density profiles as the Navarro–Frenk–White profile does of CDM haloes. We can use the model predictions, compared with the simulated density profiles, to determine the input DM–DM scattering cross-sections used to run the simulations. This works especially well for large cross-sections, while with CDM our results tend to favour non-zero (albeit fairly small) cross-sections, driven by a bias against small cross-sections inherent to our adopted method of sampling the model parameter space. The model works across the whole halo mass range we study, although including baryons leads to DM profiles of intermediate-mass ($10^{12} - 10^{13} \mathrm{\, M_\odot }$) haloes that do not depend strongly on the SIDM cross-section. The tightest constraints will therefore come from lower and higher mass haloes: dwarf galaxies and galaxy clusters.

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Section: Discussion a N D O U T L O O Kmentioning

confidence: 99%

The surprising accuracy of isothermal Jeans modelling of self-interacting dark matter density profiles

Robertson

Massey

Eke

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…To constrain q DM ðrÞ, one needs to carefully model the different contributions to the cluster total mass profile, coming from the stellar mass of member galaxies, the hot gas component, the BCG stellar mass, and dark matter (Sartoris et al 2020). Moreover, it is important to take into account the velocity anisotropy on the interpretation of the line-of-sight stellar velocity dispersion profile of the BCG (Schaller et al 2015;Sartoris et al 2020;He et al 2020). For these reasons, current measurements and interpretations of the asymptotic central slope of q DM ðrÞ in galaxy clusters appear to be controversial (e.g., Newman et al 2013a;Sartoris et al 2020;He et al 2020).…”

Section: Cluster Mass Distributionmentioning

confidence: 99%

“…Moreover, it is important to take into account the velocity anisotropy on the interpretation of the line-of-sight stellar velocity dispersion profile of the BCG (Schaller et al 2015;Sartoris et al 2020;He et al 2020). For these reasons, current measurements and interpretations of the asymptotic central slope of q DM ðrÞ in galaxy clusters appear to be controversial (e.g., Newman et al 2013a;Sartoris et al 2020;He et al 2020). 18 The NFW and Einasto profiles represent phenomenological models for cuspy dark halos motivated by numerical simulations.…”

Section: Cluster Mass Distributionmentioning

confidence: 99%

Cluster–galaxy weak lensing

Umetsu

2020

Astron Astrophys Rev

101

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Weak gravitational lensing of background galaxies provides a direct probe of the projected matter distribution in and around galaxy clusters. Here, we present a self-contained pedagogical review of cluster–galaxy weak lensing, covering a range of topics relevant to its cosmological and astrophysical applications. We begin by reviewing the theoretical foundations of gravitational lensing from first principles, with a special attention to the basics and advanced techniques of weak gravitational lensing. We summarize and discuss key findings from recent cluster–galaxy weak-lensing studies on both observational and theoretical grounds, with a focus on cluster mass profiles, the concentration–mass relation, the splashback radius, and implications from extensive mass-calibration efforts for cluster cosmology.

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“…Alternative models of this universal profile have been proposed (e.g., Moore et al 1998;Ricotti et al 2007;Del Popolo 2010;Navarro et al 2004;Stadel et al 2009). The inner slope of the mass distribution might deviate from the NFW model because of several processes such as dynamical friction, central condensation of cooled gas, and active galactic nucleus (AGN) feedback (e.g., Blumenthal et al 1986;Martizzi et al 2012;Schaller et al 2015;Laporte & White 2015;Peirani et al 2017;He et al 2020). The external slope of the mass distribution in individual clusters might deviate from the NFW model depending on the mass accretion rate in the cluster outskirts (e.g., Diemer & Kravtsov 2014;More et al 2015;Vallés-Pérez et al 2020).…”

Section: Introductionmentioning

confidence: 99%

The GOGREEN survey: Internal dynamics of clusters of galaxies at redshift 0.9–1.4

Biviano

Burg

Balogh

et al. 2021

A&A

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Context. The study of galaxy cluster mass profiles (M(r)) provides constraints on the nature of dark matter and on physical processes affecting the mass distribution. The study of galaxy cluster velocity anisotropy profiles (β(r)) informs the orbits of galaxies in clusters, which are related to their evolution. The combination of mass profiles and velocity anisotropy profiles allows us to determine the pseudo phase-space density profiles (Q(r)); numerical simulations predict that these profiles follow a simple power law in cluster-centric distance. Aims. We determine the mass, velocity anisotropy, and pseudo phase-space density profiles of clusters of galaxies at the highest redshifts investigated in detail to date. Methods. We exploited the combination of the GOGREEN and GCLASS spectroscopic data-sets for 14 clusters with mass M200 ≥ 1014 M⊙ at redshifts 0.9 ≤ z ≤ 1.4. We constructed an ensemble cluster by stacking 581 spectroscopically identified cluster members with stellar mass M⋆ ≥ 109.5 M⊙. We used the MAMPOSSt method to constrain several M(r) and β(r) models, and we then inverted the Jeans equation to determine the ensemble cluster β(r) in a non-parametric way. Finally, we combined the results of the M(r) and β(r) analysis to determine Q(r) for the ensemble cluster. Results. The concentration c200 of the ensemble cluster mass profile is in excellent agreement with predictions from Λ cold dark matter (ΛCDM) cosmological numerical simulations, and with previous determinations for clusters of similar mass and at similar redshifts, obtained from gravitational lensing and X-ray data. We see no significant difference between the total mass density and either the galaxy number density distributions or the stellar mass distribution. Star-forming galaxies are spatially significantly less concentrated than quiescent galaxies. The orbits of cluster galaxies are isotropic near the center and more radial outside. Star-forming galaxies and galaxies of low stellar mass tend to move on more radially elongated orbits than quiescent galaxies and galaxies of high stellar mass. The profile Q(r), determined using either the total mass or the number density profile, is very close to the power-law behavior predicted by numerical simulations. Conclusions. The internal dynamics of clusters at the highest redshift probed in detail to date are very similar to those of lower-redshift clusters, and in excellent agreement with predictions of numerical simulations. The clusters in our sample have already reached a high degree of dynamical relaxation.

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Constraining the inner density slope of massive galaxy clusters

Cited by 26 publications

References 68 publications

The surprising accuracy of isothermal Jeans modelling of self-interacting dark matter density profiles

The surprising accuracy of isothermal Jeans modelling of self-interacting dark matter density profiles

Cluster–galaxy weak lensing

The GOGREEN survey: Internal dynamics of clusters of galaxies at redshift 0.9–1.4

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