CLASH-VLT: The mass, velocity-anisotropy, and pseudo-phase-space density profiles of the z = 0.44 galaxy cluster MACS J1206.2-0847

By A. Biviano, Piero Rosati, I. Balestra, A. Mercurio, M. Girardi, M. Nonino, C. Grillo, M. Scodeggio, D. Lemze, D. Kelson and 37 more. 2013

145 citations recorded by the source corpus.

Aims. We constrain the mass, velocity-anisotropy, and pseudo-phase-space density profiles of the z = 0.44 CLASH cluster MACS J1206.2-0847, using the projected phase-space distribution of cluster galaxies in combination with gravitational lensing.Methods. We use an unprecedented data-set of ≃600 redshifts for cluster members, obtained as part of a VLT/VIMOS large program, to constrain the cluster mass profile over the radial range ~0–5 Mpc (0–2.5 virial radii) using the MAMPOSSt and Caustic methods. We then add external constraints from our previous gravitational lensing analysis. We invert the Jeans equation to obtain the velocity-anisotropy profiles of cluster members. With the mass-density and velocity-anisotropy profiles we then obtain the first determination of a cluster pseudo-phase-space density profile.Results. The kinematics and lensing determinations of the cluster mass profile are in excellent agreement. This is very well fitted by a NFW model with mass M200 = (1.4 ± 0.2) × 1015 M⊙ and concentration c200 = 6 ± 1, only slightly higher than theoretical expectations. Other mass profile models also provide acceptable fits to our data, of (slightly) lower (Burkert, Hernquist, and Softened Isothermal Sphere) or comparable (Einasto) quality than NFW. The velocity anisotropy profiles of the passive and star-forming cluster members are similar, close to isotropic near the center and increasingly radial outside. Passive cluster members follow extremely well the theoretical expectations for the pseudo-phase-space density profile and the relation between the slope of the mass-density profile and the velocity anisotropy. Star-forming cluster members show marginal deviations from theoretical expectations.Conclusions. This is the most accurate determination of a cluster mass profile out to a radius of 5 Mpc, and the only determination of the velocity-anisotropy and pseudo-phase-space density profiles of both passive and star-forming galaxies for an individual cluster. These profiles provide constraints on the dynamical history of the cluster and its galaxies. Prospects for extending this analysis to a larger cluster sample are discussed.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f55a6c527934cc2ef59478c46c245742a9891ad6

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Atomic and Molecular Physics, and Optics

In Instrumentation

Citations in the corpus

LoCuSS: THE SLOW QUENCHING OF STAR FORMATION IN CLUSTER GALAXIES AND THE NEED FOR PRE-PROCESSING (2015, background): “…as well as to constrain the masses, density profiles, and dynamical states of the clusters themselves (e.g., Moss & Dickens 1977; Binggeli et al. 1987; Biviano et al. 1997, 2013; Diaferio & Geller 1997; Diaferio 1999; Biviano & Katgert 2004; Gill et al. 2005; Serra et al. 2011; Mahajan et al.…”
HUBBLE SPACE TELESCOPE COMBINED STRONG AND WEAK LENSING ANALYSIS OF THE CLASH SAMPLE: MASS AND MAGNIFICATION MODELS AND SYSTEMATIC UNCERTAINTIES (2014, methodology): “Our profile was found to agree well also with an independent WL analysis by Umetsu et al. (2012) and a dynamical analysis by Biviano et al. (2013).”
The first and second data releases of the Kilo-Degree Survey (2015, methodology): “…has been successfully used in many experiments on different data sets, often composed through accurate cross-matching among public surveys (SDSS for galaxies: Brescia et al. 2014; UKIDSS, SDSS, GALEX and WISE for quasars: Brescia et al. 2013; CLASH-VLT data for galaxies: Biviano et al. 2013).”
CLASH: JOINT ANALYSIS OF STRONG-LENSING, WEAK-LENSING SHEAR, AND MAGNIFICATION DATA FOR 20 GALAXY CLUSTERS (2015, methodology): “…sets of multiple images (Zitrin et al. 2012a, 2015), whose spectroscopic redshifts have been determined from a dedicated spectroscopic survey conducted with the VIMOS spectrograph on the Very Large Telescope (VLT; Biviano et al. 2013; Balestra et al. 2013; Rosati et al. 2014; Girardi et al. 2015).”
CLASH: WEAK-LENSING SHEAR-AND-MAGNIFICATION ANALYSIS OF 20 GALAXY CLUSTERS (2014, methodology): “…the results of our weak-lensing cluster mass estimates, where we employ the robust biweight estimators of Beers et al. (1990) for the central location (average) and scale (dispersion) of the marginalized posterior probability distributions (e.g., Sereno & Umetsu 2011; Biviano et al. 2013).”