CLASH-VLT: a full dynamical reconstruction of the mass profile of Abell S1063 from 1 kpc out to the virial radius

Sartoris, B.; Biviano, A.; Rosati, P.; Mercurio, A.; Grillo, C.; Ettori, S.; Nonino, M.; Umetsu, Keiichi; Bergamini, P.; Caminha, G. B.; Girardi, M.

doi:10.1051/0004-6361/202037521

Cited by 41 publications

(80 citation statements)

References 135 publications

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“…Meneghetti et al 2007;Li et al 2016). Recently, Sartoris et al (2020) have estimated a value of −0.99 for the dark matter density slope at the centre of Abell S1063 -in excellent agreement with CDM predictions -from analysis of a large sample of stars in the central galaxy with spectroscopic data and a model allowing for variable velocity dispersion anisotropy.…”

Section: Introductionmentioning

confidence: 61%

Constraining the inner density slope of massive galaxy clusters

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We determine the inner density profiles of massive galaxy clusters (M200 > 5 × 1014 M⊙) in the Cluster-EAGLE (C-EAGLE) hydrodynamic simulations, and investigate whether the dark matter density profiles can be correctly estimated from a combination of mock stellar kinematical and gravitational lensing data. From fitting mock stellar kinematics and lensing data generated from the simulations, we find that the inner density slopes of both the total and the dark matter mass distributions can be inferred reasonably well. We compare the density slopes of C-EAGLE clusters with those derived by Newman et al. for seven massive galaxy clusters in the local Universe. We find that the asymptotic best-fitting inner slopes of ‘generalized’ Navarro–Frenk–White (gNFW) profiles, γgNFW, of the dark matter haloes of the C-EAGLE clusters are significantly steeper than those inferred by Newman et al. However, the mean mass-weighted dark matter density slopes of the simulated clusters are in good agreement with the Newman et al. estimates. We also find that the estimate of γgNFW is very sensitive to the constraints from weak lensing measurements in the outer parts of the cluster and a bias can lead to an underestimate of γgNFW.

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Section: Introductionmentioning

confidence: 61%

Constraining the inner density slope of massive galaxy clusters

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Determinations of the central slope of the dark-matter density profile q DM ðrÞ in clusters require additional constraints on the total mass in the innermost region, such as from stellar kinematics of the BCG (Newman et al 2013a). 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).…”

Section: Cluster Mass Distributionmentioning

confidence: 99%

“…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%

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Cluster–galaxy weak lensing

Umetsu

2020

Astron Astrophys Rev

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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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“…There have been many determinations of the M(r) of clusters of galaxies using cluster galaxies as tracers of the potential, both for individual clusters (e.g., Geller et al 1999;Rines et al 2000Rines et al , 2003Łokas & Mamon 2003;Łokas et al 2006;Rines & Diaferio 2006;Wojtak & Łokas 2010;Biviano et al 2013Biviano et al , 2017aGuennou et al 2014;Munari et al 2014;Balestra et al 2016;Maughan et al 2016;Sartoris et al 2020) and for stacks of several clusters (e.g., Carlberg et al 1997a;van der Marel et al 2000;Biviano & Girardi 2003;Katgert et al 2004). Results from these studies have been used to constrain the concentration-mass relation, in most cases by adopting the NFW model (Groener et al 2016;Biviano et al 2017b).…”

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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CLASH-VLT: a full dynamical reconstruction of the mass profile of Abell S1063 from 1 kpc out to the virial radius

Cited by 41 publications

References 135 publications

Constraining the inner density slope of massive galaxy clusters

Constraining the inner density slope of massive galaxy clusters

Cluster–galaxy weak lensing

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

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