Hubble space telescope combined strong and weak lensing analysis of the CLASH sample

• Verfasst von: Zitrin, Adi [VerfasserIn]
• Verfasst von: Fabris, Agnese [VerfasserIn]
• Verfasst von: Bartelmann, Matthias [VerfasserIn]
• Verfasst von: Carrasco, Mauricio [VerfasserIn]
• Titel: Hubble space telescope combined strong and weak lensing analysis of the CLASH sample
• Titelzusatz: mass and magnification models and systematic uncertainties
• Verf.angabe: Adi Zitrin, Agnese Fabris, Julian Merten, Peter Melchior, Massimo Meneghetti, Anton Koekemoer, Dan Coe, Matteo Maturi, Matthias Bartelmann, Marc Postman, Keiichi Umetsu, Gregor Seidel, Irene Sendra, Tom Broadhurst, Italo Balestra, Andrea Biviano, Claudio Grillo, Amata Mercurio, Mario Nonino, Piero Rosati, Larry Bradley, Mauricio Carrasco, Megan Donahue, Holland Ford, Brenda L. Frye, John Moustakas
• Fussnoten: Gesehen am 19.09.2017
• Titel Quelle: Enthalten in: De.arxiv.org
• Jahr Quelle: 2015
• Band/Heft Quelle: (2015) Artikel-Nummer 1411.1414, 35 Seiten
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1563608898

Abstract

We present results from a comprehensive lensing analysis in HST data, of the complete CLASH cluster sample. We identify new multiple-images previously undiscovered 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 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 NFW 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 $\sim40\%$ in the (dimensionless) mass density, $\kappa$, and $\sim20\%$ in the magnification, $\mu$. We show maps of these differences for each cluster, as well as the mass distributions, critical curves, and 2D integrated mass profiles. For the Einstein radii ($z_{s}=2$) we find that all typically agree within $10\%$ between the two models, and Einstein masses agree, typically, within $\sim15\%$. At larger radii, the total projected, 2D integrated mass profiles of the two models, within $r\sim2\arcmin$, differ by $\sim30\%$. Stacking the surface-density profiles of the sample from the two methods together, we obtain an average slope of