Masses of Galaxy Clusters from Gravitational Lensing

By H. Hoekstra, M. Bartelmann, H. Dahle, H. Israel, M. Limousin, Massimo Meneghetti. 2013

140 citations recorded by the source corpus.

Despite consistent progress in numerical simulations, the observable properties of galaxy clusters are difficult to predict ab initio. It is therefore important to compare both theoretical and observational results to a direct measure of the cluster mass. This can be done by measuring the gravitational lensing effects caused by the bending of light by the cluster mass distribution. In this review we discuss how this phenomenon can be used to determine cluster masses and study the mass distribution itself. As sample sizes increase, the accuracy of the weak lensing mass estimates needs to improve accordingly. We discuss the main practical aspects of these measurements. We review a number of applications and highlight some recent results.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8e8ac1d0e1cda5981dd72b13bd0309871015c28d

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Citations in the corpus

Galaxy Alignments: Observations and Impact on Cosmology (2015, methodology): “…clusters (Okabe et al. 2010; Applegate et al. 2014; Hoekstra et al. 2015), where ensemble-averaged tangential shear as a function of cluster-centric radius can be related to the projected mass, or fit by a parametric model for the mass distribution (see Hoekstra et al. 2013, for a recent review).”
The Canadian Cluster Comparison Project: detailed study of systematics and updated weak lensing masses (2015, background): “For a recent review of the use of gravitational lensing to study cluster masses and density profiles, we refer the reader to Hoekstra et al. (2013).”
History of dark matter (2018, unknown): “Today, gravitational lensing is frequently used to study the properties of clusters [see, e.g., Mellier (2010) and Hoekstra et al. (2013) for recent reviews].”