Cross‐Correlation Lensing: Determining Galaxy and Cluster Mass Profiles from Statistical Weak‐Lensing Measurements | Zendy

David E. Johnston | Zendy; E. Sheldon | Zendy; Argyro Tasitsiomi | Zendy; J. Frieman | Zendy; Risa H. Wechsler | Zendy; Timothy A. McKay | Zendy

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Cross‐Correlation Lensing: Determining Galaxy and Cluster Mass Profiles from Statistical Weak‐Lensing Measurements

Author(s) -

David E. Johnston,

E. Sheldon,

Argyro Tasitsiomi,

J. Frieman,

Risa H. Wechsler,

Timothy A. McKay

Publication year - 2007

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/510060

Subject(s) - physics , weak gravitational lensing , astrophysics , halo , galaxy cluster , virial mass , galaxy , cluster (spacecraft) , velocity dispersion , correlation function (quantum field theory) , redshift , computer science , programming language , optoelectronics , dielectric

We present a new non-parametric method for determining mean 3D density andmass profiles from weak lensing measurements around stacked samples of galaxiesor clusters, that is, from measurement of the galaxy-shear or cluster-shearcorrelation functions. Since the correlation function is statisticallyisotropic, this method evades problems, such as projection of large-scalestructure along the line of sight or halo asphericity, that complicate attemptsto infer masses from weak lensing measurements of individual objects. Wedemonstrate the utility of this method in measuring halo profiles, galaxy-massand cluster-mass cross-correlation functions, and cluster virial masses. Wetest this method on an N-body simulation and show that it correctly andaccurately recovers the 3D density and mass profiles of halos. We find noevidence of problems due to a mass sheet degeneracy in the simulation.Cross-correlation lensing provides a powerful method for calibrating themass-observable relation for use in measurement of the cluster mass function inlarge surveys. It can also be used on large scales to measure and remove thehalo bias and thereby provide a direct measurement of Omega_m * sigma_8.Comment: submitted to AP

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