Three-dimensional Multi-probe Analysis of the Galaxy Cluster A1689

Keiichi Umetsu; Mauro Sereno; Elinor Medezinski; Mario Nonino; Tony Mroczkowski; Jose M. Diego; Stefano Ettori; Nobuhiro Okabe; Tom Broadhurst; Doron Lemze

doi:10.1088/0004-637X/806/2/207

paper

Three-dimensional Multi-probe Analysis of the Galaxy Cluster A1689

arXiv:1503.01482 · doi:10.1088/0004-637X/806/2/207

Abstract

We perform a 3D multi-probe analysis of the rich galaxy cluster A1689 by combining improved weak-lensing data from new BVRi'z' Subaru/Suprime-Cam observations with strong-lensing, X-ray, and Sunyaev-Zel'dovich effect (SZE) data sets. We reconstruct the projected matter distribution from a joint weak-lensing analysis of 2D shear and azimuthally integrated magnification constraints, the combination of which allows us to break the mass-sheet degeneracy. The resulting mass distribution reveals elongation with axis ratio ~0.7 in projection. When assuming a spherical halo, our full weak-lensing analysis yields a projected concentration of $c_{200 c}^{2 D} = 8.9 \pm 1.1$ ( $c_{v i r}^{2 D} \sim 11$ ), consistent with and improved from earlier weak-lensing work. We find excellent consistency between weak and strong lensing in the region of overlap. In a parametric triaxial framework, we constrain the intrinsic structure and geometry of the matter and gas distributions, by combining weak/strong lensing and X-ray/SZE data with minimal geometric assumptions. We show that the data favor a triaxial geometry with minor-major axis ratio 0.39+/-0.15 and major axis closely aligned with the line of sight (22+/-10 deg). We obtain $M_{200 c} = (1.2 \pm 0.2) \times 1 0^{15} M_{⊙} / h$ and $c_{200 c} = 8.4 \pm 1.3$ , which overlaps with the $> 1 σ$ tail of the predicted distribution. The shape of the gas is rounder than the underlying matter but quite elongated with minor-major axis ratio 0.60+/-0.14. The gas mass fraction within 0.9Mpc is 10^{+3}_{-2}%. The thermal gas pressure contributes to ~60% of the equilibrium pressure, indicating a significant level of non-thermal pressure support. When compared to Planck's hydrostatic mass estimate, our lensing measurements yield a spherical mass ratio of $M_{P l an c k} / M_{G L} = 0.70 \pm 0.15$ and $0.58 \pm 0.10$ with and without corrections for lensing projection effects, respectively.

arXiv commentAccepted by ApJ. Minor textual changes to improve clarity (e.g., 5. HST STRONG-LENSING ANALYSIS). 26 pages, 17 figures. A version with high-resolution figures is available at http://www.asiaa.sinica.edu.tw/~keiichi/upfiles/Umetsu15/umetsu15.pdf

Three-dimensional Multi-probe Analysis of the Galaxy Cluster A1689

Abstract

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