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Published August 10, 2012 | Published
Journal Article Open

CLASH: Mass Distribution in and around MACS J1206.2-0847 from a Full Cluster Lensing Analysis


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_cz' 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 ~2:1 axis ratio in the plane of the sky. Our full-lensing mass profile exhibits a shallow profile slope dln Σ/dln R ~ –1 at cluster outskirts (R ≳ 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) × 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, they 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.

Additional Information

© 2012 American Astronomical Society. Received 2012 April 4; accepted 2012 June 5; published 2012 July 26. Based in part on data collected at the Subaru Telescope, which is operated by the National Astronomical Society of Japan. We thank our referee for a careful reading of the manuscript and for providing useful comments. We acknowledge useful discussions with Nobuhiro Okabe, Masamune Oguri, and Mauro Sereno. We are grateful for comments by Cheng-Jiun Ma. We thank Nick Kaiser for making the IMCAT package publicly available. We thank G. Mark Voit for having contributed to the ACCEPT-based X-ray mass measurements in advance of publication. We are grateful for the hospitality of the Spitzer Science Center at Caltech, where part of this work was done. The CLASH Multi-Cycle Treasury Program is based on observations made with the NASA/ESA Hubble Space Telescope. The Space Telescope Science Institute is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. ACS was developed under NASA contract NAS 5-32864. This research is supported in part by NASA grant HST-GO-12065.01-A, National Science Council of Taiwan grant NSC100-2112-M-001-008-MY3, and PRIN INAF 2010. K.U. acknowledges support from the Academia Sinica Career Development Award. Part of this work is based on data collected at the Very Large Telescope at the ESO Paranal Observatory, under Programme ID 186.A-0798. P.R., C.G., I.B., and S.S. acknowledge partial support by the DFG cluster of excellence Origin and Structure of the Universe. The Bolocam observations were partially supported by the Gordon and Betty Moore Foundation. J.S. was supported by NSF/AST0838261 and NASA/NNX11AB07G; N.C. was partially supported by a NASA Graduate Student Research Fellowship. A.Z. is supported by the "Internationale Spitzenforschung II/2" of the Baden-Württemberg Stiftung. C.G. acknowledges support from the Dark Cosmology Centre, which is funded by the Danish National Research Foundation. I.S. holds a PhD FPI Fellowship contract from the Spanish Ministry of Economy and Competitiveness and is also supported by the mentioned ministry through research project FIS2010-15492. Support for T.M. was provided by NASA through the Einstein Fellowship Program, grant PF0-110077.

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