Clash: Mass Distribution in and Around Macs J1206.2-0847 From a Full Cluster Lensing Analysis

Abstract

We derive an accurate mass distribution of the galaxy cluster MACS J1206.2-0847 (z = 0.439) from a combined weak-lensing distortion, magnification, and strong-lensing analysis of wide-field Subaru BV R c I c z ′ imaging and our recent 16-band Hubble Space Telescope observations taken as part of the Cluster Lensing And Supernova survey with Hubble (CLASH) program. We find good agreement in the regions of overlap between several weak and strong lensing mass reconstructions using a wide variety of modeling methods, ensuring consistency. The Subaru data reveal the presence of a surrounding large scale structure with the major axis running approximately north-west south-east (NW-SE), aligned with the cluster and its brightest galaxy shapes, showing elongation with a ∼ 2 : 1 axis ratio in the plane of the sky. Our full-lensing mass profile exhibits a shallow profile slope d ln Σ/d ln R ∼ −1 at cluster outskirts (R > ∼ 1 Mpc h −1 ), whereas the mass distribution excluding the NW-SE excess regions steepens further out, well described by the Navarro-Frenk-White form. Assuming a spherical halo, we obtain a virial mass M vir = (1.1±0.2±0.1)×10 15 M ⊙ h −1 and a halo concentration c vir = 6.9±1.0±1.2 (c vir ∼ 5.7 when the central 50 kpc h −1 is excluded), which falls in the range 4 < ∼ c < ∼ 7 of average c(M, z) predictions for relaxed clusters from recent Λ cold dark matter simulations. Our full lensing results are found to be in agreement with X-ray mass measurements where the data overlap, and when combined with Chandra gas mass measurements, yield a cumulative gas mass fraction of 13.7 +4.5 −3.0 % at 0.7 Mpc h −1 (≈ 1.7 r 2500 ), a typical value observed for high mass clusters.

Clash: The Enhanced Lensing Efficiency of the Highly Elongated Merging Cluster Macs J0416.1–2403

“…model-independent manner, effectively breaking the mass-sheet degeneracy. The WL analysis pipeline is described in Umetsu et al (2012). The image-plane reproduction rms(χ 2 ) is 1.…”

The projected gravitational potential of the galaxy cluster MACS J1206 derived from galaxy kinematics

“…The parameter values are summarised in Table 1. We can compare the results for the scales s c in case of the softened isothermal sphere and r s in case of NFW with Umetsu et al (2012). They obtain s c = 0.000028 ± 0.000006 (12) r s = 0.345 ± 0.050.…”

“…The observational input data for the relaxed and massive galaxy cluster MACS J1206, Ebeling et al (2001Ebeling et al ( , 2009 Umetsu et al 2012) investigated here consist of a catalogue of member galaxies ) observed in the context of the CLASH project (Postman et al 2012) as part of a large spectroscopic campaign carried out with the Very Large Telescope (VLT; CLASH-VLT Large Programme; Rosati et al 2014). According to Biviano et al (2013) and Annunziatella et al (2014), the spatial incompleteness of the spectroscopic sample varies with position in the cluster by less than 20%.…”

Calibrating thePlanckcluster mass scale with CLASH

“…Masses were derived with the SaWLens code (Merten et al 2009) that consistently combines weak and strong lensing in a non-parametric fashion on adaptively refined grids. The method was thoroughly tested with realistic lensing scenarios and numerically simulated clusters (Meneghetti et al 2010;Rasia et al 2012), and has been used multiple times for the reconstruction of real galaxy clusters (Merten et al 2009(Merten et al , 2011Umetsu et al 2012;Patel et al 2014). For the CLASH analysis, SaWLens combines constraints from HST strong lensing, HST weak lensing and wide-field groundbased weak lensing (except for CLJ1226+3332 whose mass was reconstructed using HST data only) into a single reconstruction of the cluster's gravitational potential from which it derives the surface-mass density.…”