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 BVR(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 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 northwest-southeast (NW-SE), aligned with the cluster and its brightest galaxy shapes, showing elongation with a similar to 2:1 axis ratio in the plane of the sky. Our full-lensing mass profile exhibits a shallow profile slope d ln Sigma/d ln R similar to -1 at cluster outskirts (R greater than or similar to 1 Mpc h(-1)), whereas the mass distribution excluding the NW-SE excess regions steepens farther 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) x 10(15) M-circle dot h(-1) and a halo concentration c(vir) = 6.9 +/- 1.0 +/- 1.2 (c(vir) similar to 5.7 when the central 50 kpc h(-1) is excluded), which falls in the range 4 less than or similar to < c > less than or similar to 7 of average c(M, z) predictions for relaxed clusters from recent. 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, they yield a cumulative gas mass fraction of 13.7(-3.0)(+4.5)% at 0.7 Mpc h(-1) (approximate to 1.7 r(2500)), a typical value observed for high-mass clusters.

CLASH: MASS DISTRIBUTION IN AND AROUND MACS J1206.2-0847 FROM A FULL CLUSTER LENSING ANALYSIS

ROSATI, Piero;
2012

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 BVR(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 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 northwest-southeast (NW-SE), aligned with the cluster and its brightest galaxy shapes, showing elongation with a similar to 2:1 axis ratio in the plane of the sky. Our full-lensing mass profile exhibits a shallow profile slope d ln Sigma/d ln R similar to -1 at cluster outskirts (R greater than or similar to 1 Mpc h(-1)), whereas the mass distribution excluding the NW-SE excess regions steepens farther 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) x 10(15) M-circle dot h(-1) and a halo concentration c(vir) = 6.9 +/- 1.0 +/- 1.2 (c(vir) similar to 5.7 when the central 50 kpc h(-1) is excluded), which falls in the range 4 less than or similar to < c > less than or similar to 7 of average c(M, z) predictions for relaxed clusters from recent. 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, they yield a cumulative gas mass fraction of 13.7(-3.0)(+4.5)% at 0.7 Mpc h(-1) (approximate to 1.7 r(2500)), a typical value observed for high-mass clusters.
2012
Umetsu, K; Medezinski, E; Nonino, M; Merten, J; Zitrin, A; Molino, A; Grillo, C; Carrasco, M; Donahue, M; Mahdavi, A; Coe, D; Postman, M; Koekemoer, A; Czakon, N; Sayers, J; Mroczkowski, T; Golwala, S; Koch, Pm; Lin, Ky; Molnar, Sm; Rosati, Piero; Balestra, I; Mercurio, A; Scodeggio, M; Biviano, A; Anguita, T; Infante, L; Seidel, G; Sendra, I; Jouvel, S; Host, O; Lemze, D; Broadhurst, T; Meneghetti, M; Moustakas, L; Bartelmann, M; Benitez, N; Bouwens, R; Bradley, L; Ford, H; Jimenez Teja, Y; Kelson, D; Lahav, O; Melchior, P; Moustakas, J; Ogaz, S; Seitz, S; Zheng, W.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11392/1853998
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