Clash: Joint Analysis of Strong-Lensing, Weak-Lensing Shear, and Magnification Data for 20 Galaxy Clusters*

Abstract

We present a comprehensive analysis of strong-lensing, weak-lensing shear and magnification data for a sample of 16 X-ray-regular and 4 high-magnification galaxy clusters at   z 0.19 0.69 selected from Cluster Lensing And Supernova survey with Hubble (CLASH). Our analysis combines constraints from 16-band Hubble Space Telescope observations and wide-field multi-color imaging taken primarily with Suprime-Cam on the Subaru Telescope, spanning a wide range of cluster radii (10″-16′). We reconstruct surface mass density profiles of individual clusters from a joint analysis of the full lensing constraints, and determine masses and concentrations for all of the clusters. We find the internal consistency of the ensemble mass calibration to be 5%±6% in the one-halo regime ( , which is in excellent agreement with Λ cold dark matter predictions when the CLASH selection function based on X-ray morphological regularity and the projection effects are taken into account. We also derive an ensemble-averaged surface mass density profile for the X-ray-selected subsample by stacking their individual profiles. The stacked lensing signal is detected at 33σ significance over the entire radial range 4000 kpc h −1 , accounting for the effects of intrinsic profile variations and uncorrelated large-scale structure along the line of sight. The stacked mass profile is well described by a family of density profiles predicted for cuspy dark-matter-dominated halos in gravitational equilibrium, namely, the Navarro-Frenk-White (NFW), Einasto, and DARKexp models, whereas the single power-law, cored isothermal and Burkert density profiles are disfavored by the data. We show that cuspy halo models that include the large-scale two-halo term provide improved agreement with the data. , demonstrating consistency between the complementary analysis methods.

Comparing Dark Energy Survey andHST–CLASH observations of the galaxy cluster RXC J2248.7−4431: implications for stellar mass versus dark matter

“…The black points represent the CLASH total stellar mass profile computed in this paper, with our NFW fit (black solid line). The red solid line is the Umetsu et al (2016) NFW best fit for CLASH from a strong lensing, weak lensing and magnification joint analysis. This profile is restricted to the NFW fitting range R < 2Mpc h −1 chosen in Umetsu et al (2016), which is larger than the HST field of view as other data sets were used in a joint analysis.…”

“…For RXJ2248, they also identified filamentary structures of the luminous red-sequence galaxies found with the REDMAPPER (Rykoff et al 2014) algorithm. Umetsu et al (2016) combined HST and wide field imaging (from the Subaru telescope or the ESO/WFI) observations to reconstruct the surface mass density profiles of 20 CLASH clusters. Their analysis jointly uses strong lensing as well as weak lensing with shear and magnification, and for RXJ2248 they found M 200c = 18.78 ± 6.72 × 10 14 M .…”

“…For the DES f , the total mass comes from the nonparametric reconstruction of the weak lensing shear profile done in Melchior et al (2015) (purple points), or from their NFW best fit (green squares). For CLASH, M tot is a result of the Umetsu et al (2016) NFW best fit for CLASH from a strong lensing, weak lensing and magnification joint analysis (red triangles). The mean DES stellar mass fraction from non-parametric weak lensing mass profile is f = (7.3 ± 1.7) × 10 −3 , and is represented by the dashed line.…”

LoCuSS: weak-lensing mass calibration of galaxy clusters

“…Stacking the shear signal from a sample of clusters averages over the distribution of internal structures and halo triaxiality, and thus overcomes the structural biases suffered by some individual cluster mass measurements (e.g. Mandelbaum et al 2006;Johnston et al 2007;Okabe et al 2010aOkabe et al , 2013Umetsu et al 2011Umetsu et al , 2014Umetsu et al , 2015bOguri et al 2012;Leauthaud et al 2012;Miyatake et al 2013;Niikura et al 2015). We compute the average lensing signal in physical length unit centered on the respective BCGs.…”

What if LIGO’s gravitational wave detections are strongly lensed by massive galaxy clusters?

“…We have assembled a list of 130 spectroscopically confirmed strong cluster lenses from the literature, drawing mainly on HST studies of X-ray selected clusters, and strong-lensing clusters from the Sloan Digital Sky Survey (Smith et al 2005(Smith et al , 2009Limousin et al 2007Limousin et al , 2012Richard et al 2010;Christensen et al 2012;Oguri et al 2012;Jauzac et al 2015;Paraficz et al 2016;Umetsu et al 2016). We compare the celestial coordinates of these clusters with the sky localization maps of the BBH merger detections from 2015, finding that none of the known strong-lensing clusters are located The sky localizations of all three GW events intersect the disc of the Milky Way.…”