Combining strong lensing and dynamics in galaxy clusters: integrating MAMPOSSt within LENSTOOL

Verdugo, T.; Limousin, M.; Motta, V.; Mamon, G. A.; Foëx, G.; Gastaldello, F.; Jullo, Eric; Biviano, A.; Rojas, Karina; Muñoz, Roberto P.; Cabanac, R.; Magaña, Juan; Fernández-Trincado, J. G.; Adame, L.; Leo, M. A. De

doi:10.1051/0004-6361/201628629

Cited by 12 publications

(16 citation statements)

References 77 publications

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“…MAMPOSSt assumes a shape for the 3D velocity distribution (a Gaussian in the current implementation of the method). It has been successfully tested on simulated halos from cosmological simulations that included both dynamically relaxed and unrelaxed halos, and it has already been applied to several data sets (e.g., Biviano et al 2013Biviano et al , 2017bGuennou et al 2014;Munari et al 2014;Verdugo et al 2016;Pizzuti et al 2017;Mamon et al 2019;Sartoris et al 2020).…”

Section: Methodology: Mamposstmentioning

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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Section: Methodology: Mamposstmentioning

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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“…Fig. 5) observed at zspec = 1.017 ± 0.001 (Verdugo et al 2011(Verdugo et al , 2016. The apparent Einstein radius amounts to θE ∼ 7.1".…”

Section: Selection Of Known Lensesmentioning

confidence: 84%

“…The apparent Einstein radius amounts to θE ∼ 7.1". A combined dynamical and parametric lensing mass reconstruction carried out by Verdugo et al 2016 suggests that the centers and orientations of the main dark matter halo, the intracluster gas halo and the luminosity contours are in good agreement if fitting an NFW profile for the main group halo and pseudo-isothermal ellipses to the central galaxy halos.…”

Section: Selection Of Known Lensesmentioning

confidence: 99%

EasyCritics – I. Efficient detection of strongly lensing galaxy groups and clusters in wide-field surveys

Stapelberg

Carrasco

Maturi

2018

Monthly Notices of the Royal Astronomical Society

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We present EasyCritics, an algorithm to detect strongly-lensing groups and clusters in wide-field surveys without relying on a direct recognition of arcs. EasyCritics assumes that light traces mass in order to predict the most likely locations of critical curves from the observed fluxes of luminous red early-type galaxies in the line of sight. The positions, redshifts and fluxes of these galaxies constrain the idealized gravitational lensing potential as a function of source redshift up to five free parameters, which are calibrated on few known lenses. From the lensing potential, EasyCritics derives the critical curves for a given, representative source redshift. The code is highly parallelized, uses fast Fourier methods and, optionally, GPU acceleration in order to process large datasets efficiently. The search of a 1 deg 2 field of view requires less than 1 minute on a modern quad-core CPU, when using a pixel resolution of 0.25 /px. In this first part of a paper series on EasyCritics, we describe the main underlying concepts and present a first demonstration on data from the Canada-France-Hawaii-Telescope Lensing Survey. We show that EasyCritics is able to identify known groupand cluster-scale lenses, including a cluster with two giant arc candidates that were previously missed by automated arc detectors.

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“…MAMPOSSt assumes a shape for the 3D velocity distribution (a Gaussian in the current implementation of the method). It has been successfully tested on simulated halos from cosmological simulations that included both dynamically relaxed and unrelaxed halos, and it has already been applied to several data sets (e.g., Biviano et al 2013;Guennou et al 2014;Munari et al 2014;Verdugo et al 2016;Biviano et al 2017a;Pizzuti et al 2017;Mamon et al 2019;Sartoris et al 2020).…”

Section: Methodology: Mamposstmentioning

confidence: 99%

The GOGREEN survey: the internal dynamics of clusters of galaxies at redshift 0.9-1.4

Biviano,

van der Burg,

Balogh

et al. 2021

Preprint

Self Cite

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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 M 200 ≥ 10 14 M ⊙ at redshifts 0.9 ≤ z ≤ 1.4. We constructed an ensemble cluster by stacking 581 spectroscopically identified cluster members with stellar mass M ⋆ ≥ 10 9.5 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 c 200 of the ensemble cluster mass profile is in excellent agreement with predictions from Lambda 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.

show abstract

Combining strong lensing and dynamics in galaxy clusters: integrating MAMPOSSt within LENSTOOL

Cited by 12 publications

References 77 publications

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

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

EasyCritics – I. Efficient detection of strongly lensing galaxy groups and clusters in wide-field surveys

The GOGREEN survey: the internal dynamics of clusters of galaxies at redshift 0.9-1.4

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