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|Title:||Hubble Space Telescope Combined Strong and Weak Lensing Analysis of the CLASH Sample: Mass and Magnification Models and Systematic Uncertainties||Authors:||Zitrin, Adi
Frye, Brenda L.
|Issue Date:||2015||Journal:||THE ASTROPHYSICAL JOURNAL||Number:||801||Issue:||1||First Page:||44||Abstract:||We present results from a comprehensive lensing analysis in Hubble Space Telescope (HST) data of the complete Cluster Lensing And Supernova survey with Hubble cluster sample. We identify previously undiscovered multiple images, allowing improved or first constraints on the cluster inner mass distributions and profiles. We combine these strong lensing constraints with weak lensing shape measurements within the HST field of view (FOV) to jointly constrain the mass distributions. The analysis is performed in two different common parameterizations (one adopts light-traces-mass for both galaxies and dark matter while the other adopts an analytical, elliptical Navarro-Frenk-White form for the dark matter) to provide a better assessment of the underlying systematics—which is most important for deep, cluster-lensing surveys, especially when studying magnified high-redshift objects. We find that the typical (median), relative systematic differences throughout the central FOV are ~40% in the (dimensionless) mass density, κ, and ~20% in the magnification, μ. We show maps of these differences for each cluster, as well as the mass distributions, critical curves, and two-dimensional (2D)-integrated mass profiles. For the Einstein radii (z<SUB>s</SUB> = 2) we find that all typically agree within 10% between the two models, and Einstein masses agree, typically, within ~15%. At larger radii, the total projected, 2D-integrated mass profiles of the two models, within r ~ 2', differ by ~30%. Stacking the surface-density profiles of the sample from the two methods together, we obtain an average slope of dlog (Σ)/dlog (r) ~ -0.64 ± 0.1, in the radial range  kpc. Last, we also characterize the behavior of the average magnification, surface density, and shear differences between the two models as a function of both the radius from the center and the best-fit values of these quantities. All mass models and magnification maps are made publicly available for the community.||Acknowledgments:||We thank the reviewer of this work for valuable comments. A.Z. is grateful for useful discussions with Carrie Bridge and Drew Newman. This work is based on observations made with the NASA/ESA Hubble Space Telescope . Support for Program 12065 was provided by NASA from the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA Contract NAS 5-26555. Support for this work was provided by NASA through Hubble Fellowship Grant HST-HF2-51334.001-A awarded by STScI. K.U. acknowledges support from the Ministry of Science and Technology of Taiwan through Grant MOST 103-2112-M-001-030-MY3. The research was in part carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA.||URI:||http://hdl.handle.net/20.500.12386/23361||URL:||https://iopscience.iop.org/article/10.1088/0004-637X/801/1/4||ISSN:||0004-637X||DOI:||10.1088/0004-637X/801/1/44||Bibcode ADS:||2015ApJ...801...44Z||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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checked on Sep 21, 2020
checked on Sep 21, 2020
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