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Direct measurement of the magnification produced by galaxy clusters as gravitational lenses

posted Jul 25, 2011, 12:13 PM by Marco Lombardi   [ updated Feb 1, 2012, 4:58 AM ]
A&A 532, A37, by A. Sonnenfeld, G. Bertin, and M. Lombardi  

Abstract. 
Context: Weak lensing is one of the most readily available diagnostic tools to measure the total density profiles of distant clusters of galaxies. Unfortunately, it suffers from the well-known mass-sheet degeneracy, so that weak lensing analyses cannot lead to fully reliable determinations of the total mass of the clusters. One possible way to set the relevant scale of the density profile would be to make a direct measurement of the magnification produced by the clusters as gravitational lenses; in the past, this objective has been addressed in a number of ways, but with no significant success. 

Aims: We revisit a suggestion made a few years ago for this general purpose, based on the use of the fundamental plane as a standard rod for early-type galaxies. Here we move one step further, beyond the simple outline of the idea given earlier, and quantify some statistical properties of this innovative diagnostic tool, with the final goal of identifying clear guidelines for a future observational test of concrete cases, which turns out to be well within the current instrument capabilities. 

Methods: The study is carried out by discussing the statistical properties of fundamental plane measurements for a sample of early-type source galaxies behind a massive cluster, for which a weak lensing analysis is assumed to be available. Some general results are first obtained analytically and then tested and extended by means of dedicated simulations. 

Results: We proceed with determining the optimal way of using fundamental plane measurements to determine the mass scale of a given cluster, which we find to be the study of a sample of early-type galaxies behind the cluster distributed approximately uniformly on the sky. We discuss the role of the redshift distribution of the source galaxies, in relation to the redshift of the lensing cluster and to the limitations of fundamental plane measurements. Simple simulations are carried out for clusters with intrinsic properties similar to those of the Coma cluster. We also show that, within a realistic cosmological scenario, substructures do not contribute much to the magnification signal that we are looking for, but add only a modest amount of scatter. 

Conclusions: We find that for a massive cluster (M200 > 1015 Mȯ) located at redshift 0.3 ± 0.1, a set of about 20 fundamental plane measurements, combined with a robust weak lensing analysis, should be able to lead to a mass determination with a precision of 20% or better.
Simulated Fundamental Plane measurements.  The straight line is the Fundamental Plane expected in the
absence of lensing, viewed edge-on.

Contour plot of the difference between the true and the reconstructed dimensionless mass density from a weak-lensing analysis. In the central region the reconstructed profile underestimates the surface mass density, while in a significant region of the image plane the opposite case occurs.
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