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Gravitational Magnification And Cluster Masses

Published online by Cambridge University Press:  25 May 2016

A.N. Taylor
A.N. Taylor*
Affiliation:
Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, UK

Extract

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The shear distortion of galaxies behind a large cluster provides us with only a relative measure of the mass of the cluster (Tyson et al. 1990, Kaiser & Squires 1993) due the invariance of shear to a sheet of matter. Thus we can at best only place lower limits on cluster masses, with the constraint that the surface density, κ(θ)=Σ(θ)/Σc, is non-negative. However, an absolute measurement of the mass can be obtained via the magnification of background galaxies (Broadhurst, Taylor & Peacock 1995, hereafter BTP). Here we describe the magnification effect, its observational consequences and mass reconstruction in the linear and nonlinear regimes. We also describe a number of applications in progress.

Type
Chapter 5: Galaxy Clusters
Information
Symposium - International Astronomical Union , Volume 173: Astrophysical Applications of Gravitational Lensing , 1996 , pp. 149 - 150
Copyright
Copyright © Kluwer 1996 

References

Broadhurst, T.J., Taylor, A.N. & Peacock, J.A., 1995, ApJ, 438, 49 (BTP) Google Scholar
Broadhurst, T.J., 1995, in Dark Matter, eds. Holt, S., & Bennett, C., 320 Google Scholar
Kaiser, N. & Squires, G., 1993, ApJ, 404, 441 CrossRefGoogle Scholar
Tyson, J.A., Valdes, F., & Wenk, R.A., 1990, ApJL, 349, L1 CrossRefGoogle Scholar