Weak Gravitational Lensing and Its Cosmological Applications

By H. Hoekstra, B. Jain. 2008

357 citations recorded by the source corpus.

Weak gravitational lensing is a unique probe of the dark side of the universe: It provides a direct way to map the distribution of dark matter around galaxies and clusters of galaxies as well as on cosmological scales. Furthermore, the measurement of the weak lensing–induced distortions of the shapes of distant galaxies is a potentially powerful probe of dark energy. In this review we discuss how this challenging measurement is made and interpreted. We describe the various systematic effects that can hamper progress and how they may be overcome. We review some of the recent results in weak lensing by galaxies, galaxy clusters, and cosmic shear and discuss the prospects for dark energy measurements from planned surveys.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/4be459aaf8821697d0fc0546ac7a540b5871623c

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Citations in the corpus

Origins of weak lensing systematics, and requirements on future instrumentation (or knowledge of instrumentation) (2012, background): “Statistical measurements of weak gravitational lensing in a large sample of galaxies offer a direct way to probe the dark sector of the Universe (see reviews by Hoekstra & Jain 2008; Massey, Kitching & Richard 2010).”
Galaxy Alignments: Observations and Impact on Cosmology (2015, methodology): “See Bartelmann & Schneider (2001); Hoekstra & Jain (2008); Munshi et al. (2008); Bartelmann (2010) for general reviews of weak lensing.”
Gravitational lensing (2010, background): “Weak gravitational lensing by large-scale structures is covered by several dedicated reviews, highlighting different aspects of this rich and quickly developing subject [27, 201, 205, 320, 322, 355, 399].”
HUBBLE SPACE TELESCOPE COMBINED STRONG AND WEAK LENSING ANALYSIS OF THE CLASH SAMPLE: MASS AND MAGNIFICATION MODELS AND SYSTEMATIC UNCERTAINTIES (2014, background): “…objects observed through the lensing cluster will be (only) slightly sheared and magnified, an effect that could be detected, in principle, only on a statistical basis due to the intrinsic scatter in their source ellipticities (Kaiser et al. 1995; Bartelmann & Schneider 2001; Hoekstra & Jain 2008).”
ABC–CDE: Toward Approximate Bayesian Computation With Complex High-Dimensional Data and Limited Simulations (2018, methodology): “For further background see Hoekstra and Jain (2008), Munshi et al.”
Galaxy Alignments: An Overview (2015, background): “Haloes without substructure displayed significantly stronger alignments than those with substructure, which may support the scenario drawn up by Hopkins et al. (2005) that structure growth tends to destroy alignments.”
Masses of Galaxy Clusters from Gravitational Lensing (2013, background): “The large scale structure (LSS) introduces excess correlations in the shapes of the galaxies, also known as ‘cosmic shear’, which can be used to infer cosmological parameters or study theories of modified gravity (see e.g., Hoekstra & Jain 2008, for a recent review).”
Gravitational Lensing in Presence of Plasma: Strong Lens Systems, Black Hole Lensing and Shadow (2017, background): “Now gravitational lensing is a powerful astrophysical tool for investigations of distant objects, a distribution of dark matter and large scale structure, the cosmic microwave background, discovery of planet and checking of the General Relativity, see some reviews, classical and interesting recent w”
Practical Weak-lensing Shear Measurement with Metacalibration (2017, neutral): “…gravitational lensing is a fascinating phenomenon that has become a useful tool for testing our theories of gravity, measuring the properties and distribution of dark matter, and characterizing the accelerated expansion of the universe known as dark energy (for a review, see Hoekstra & Jain 2008).”
Beyond the Cosmological Standard Model (2014, neutral): “different power spectra—it is evident that if systematic errors can be controlled, upcoming surveys will provide percent level measurements [957].”
The behaviour of dark matter associated with four bright cluster galaxies in the 10 kpc core of Abell 3827 (2015, background): “This enables the distribution of its other- wise invisible dark matter to be mapped (for reviews of gravitational lensing, see Bartelmann & Schneider 2001; Refregier 2003; Hoekstra & Jain 2008; Bartelmann 2010; Massey, Kitching & Richard 2010a; Kneib & Natarajan 2011).”
Cosmological parameter constraints from galaxy-galaxy lensing and galaxy clustering with the SDSS DR7 (2012, background): “…of observing the total matter density (including dark matter), via the deflections of light due to intervening matter along the line-ofsight, which both magnifies and distorts galaxy shapes (for a review, see Bartelmann & Schneider 2001; Refregier 2003; Hoekstra & Jain 2008; Massey et al. 2010).”
CFHTLenS: combined probe cosmological model comparison using 2D weak gravitational lensing (2012, background): “Recent reviews which also summarize past observational results are Bartelmann & Schneider (2001), Van Waerbeke & Mellier (2003), Munshi et al. (2008), Hoekstra & Jain (2008), Bartelmann (2010).”
The Intrinsic Alignment of Galaxies and its Impact on Weak Gravitational Lensing in an Era of Precision Cosmology (2014, background): “on gravitational lensing (e.g., Schneider et al. (1992); Mellier (1999); Bartelmann and Schneider (2001); Wittman (2002); Refregier (2003b); van Waerbeke and Mellier (2003); Schneider et al. (2006b); Hoekstra and Jain (2008); Munshi et al. (2008); Heavens (2009); Bartelmann (2010); Huterer (2010); M”
Weak Lensing Measurement of the Mass--Richness Relation of SDSS redMaPPer Clusters (2016, background): “These effects can be used to measure the relationship between dark matter and visible matter, or more generally to probe cosmological models (Bartelmann & Schneider 2001; Huterer 2002; Hu 2002; Abazajian & Dodelson 2003; Refregier 2003; Schneider 2006; Hoekstra & Jain 2008; Massey et al. 2010).”
Quantifying the effect of baryon physics on weak lensing tomography (2011, background): “For a more extensive revi w of cosmic shear, see for example Hoekstra & Jain (2008) and Munshi et al. (2008).”