Weak Gravitational Lensing by Large-Scale Structure

By Alexandre Refregier. 2003

463 citations recorded by the source corpus.

▪ Abstract Weak gravitational lensing provides a unique method to map directly the distribution of dark matter in the universe and to measure cosmological parameters. This cosmic-shear technique is...

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/25ff12513e1266587bee0a8d9ac70adc9c0ca87e

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Citations in the corpus

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 [320, 27, 205, 322, 399, 201, 355].”
The Shear TEsting Programme 2: Factors affecting high precision weak lensing analyses (2006, methodology): “They are modelled using shapelets (Bernstein & Jarvis 2002; Refregier 2003; Refregier & Bacon 2003; Massey & Refregier 2005), a (complete) set of orthogonal basis functions that can be used to describe the shape of any isolated object.”
Systematic bias in cosmic shear: extending the Fisher matrix (2007, background): “Weak gravitational lensing, or ‘cosmic shear’, is undergoing a phase of rapid expansion (see Refregier 2003; Munshi et al. 2006; Hoekstra 2003, for reviews) with many future surveys and instruments being planned (e.g. DUNE1, PanSTARRS2, DES3, SNAP4 and LSST5).”
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).”
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).”
Galaxy–galaxy weak lensing in the Sloan Digital Sky Survey: intrinsic alignments and shear calibration errors (2004, methodology): “1 I N T RO D U C T I O N Weak gravitational lensing has emerged as a powerful tool for directly measuring the matter distribution in the Universe (e.g. Bartelmann & Schneider 2001; Refregier 2003a).”
Systematic errors in weak lensing: application to SDSS galaxy-galaxy weak lensing (2005, methodology): “The re-Gaussianization scheme is exact to first order in PSF nonGaussianity, however higher order approaches have been proposed based on expansions of the galaxy and PSF in orthogonal functions (Bernstein & Jarvis 2002; Refregier 2003a).”
Detection of large-scale intrinsic ellipticity—density correlation from the Sloan Digital Sky Survey and implications for weak lensing surveys (2005, methodology): “…as a powerful method for directly mea- c© 0000 RAS suring the matter distribution in the universe (e.g. Mellier 1999; Bartelmann & Schneider 2001; Refregier 2003a) following detection of the two-point function of the lensing-induced shear by several groups (Bacon et al. 2000; Van Waerbeke et…”
Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Implications for Cosmology (2006, unknown): “…al. 2005); much larger samples of highredshift supernova (Riess et al. 2004; Astier et al. 2005; Nobili et al. 2005; Clocchiatti et al. 2006; Krisciunas et al. 2005); and significant improvements in the lensing data (Refregier 2003; Heymans et al. 2005; Semboloni et al. 2006; Hoekstra et al. 2006).”
Calibrating the nonlinear matter power spectrum: Requirements for future weak lensing surveys (2004, background): “Current accuracy in the matter power spectrum at mildly nonlinear scales is about 5-10% (White & Vale 2004; Heitmann et al. 2004) which is sufficiently small for current surveys (for reviews of weak lensing, see e.g., Bartelmann & Schneider 2001, Van Waerbeke & Mellier 2003, Refregier 2003).”
The Intrinsic Alignment of Galaxies and its Impact on Weak Gravitational Lensing in an Era of Precision Cosmology (2014, background): “…(1991); Kaiser (1992); Blandford and Narayan (1992); 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);…”
The WiggleZ Dark Energy Survey: Direct constraints on blue galaxy intrinsic alignments at intermediate redshifts (2009, background): “As a result, in the past decade, weak gravitational lensing (Bartelmann & Schneider 2001; Refregier 2003) has become a powerful tool for addressing outstanding questions related to cosmology and galaxy formation.”
COSMOS: Three-dimensional Weak Lensing and the Growth of Structure (2007, background): “It is therefore a uniquely powerful probe of the dark matter distribution, directly and simply linked to theories of structure formation that may be ill-equipped to predict the distribution of light (for reviews, see Bartelmann & Schneider 2001; Wittman 2002; Refregier 2003).”