Gravitational lensing

By M. Bartelmann. 2010

345 citations recorded by the source corpus.

Gravitational lensing has developed into one of the most powerful tools for the analysis of the dark universe. This review summarizes the theory of gravitational lensing, its main current applications and representative results achieved so far. It has two parts. In the first, starting from the equation of geodesic deviation, the equations of thin and extended gravitational lensing are derived. In the second, gravitational lensing by stars and planets, galaxies, galaxy clusters and large-scale structures is discussed and summarized.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/2da6dba6e6b80851a87239531ff3558fe5f4d176

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

HerMES: CANDIDATE GRAVITATIONALLY LENSED GALAXIES AND LENSING STATISTICS AT SUBMILLIMETER WAVELENGTHS (2012, background): “It is exploited to investigate the mass distribution of the foreground lensing structures as well as the properties of the background lensed galaxies (see reviews by Bartelmann 2010; Treu 2010).”
Constraints on the Cosmic Expansion History from GWTC–3 (2021, background): “…masses) of a GW source in the absence of an EM counterpart, is the possible lensing of the GW signal due to the intervening matter distribution (Schneider et al. 1992; Bartelmann 2010; Nakamura 1998; Wang et al. 1996; Takahashi & Nakamura 2003; Dai et al. 2017; Broadhurst et al. 2018; Diego 2019).”
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).”
Calculating black hole shadows: Review of analytical studies (2021, neutral): “Wambsganss, Gravitational Lensing: Strong, Weak and Micro, Springer, Berlin (2006) [6] M.”
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).”
Cosmological Parameters from Observations of Galaxy Clusters (2011, background): “In contrast to X-ray and optical dynamical methods, gravitational lensing offers a way to measure the masses of clusters that is free of assumptions regarding the dynamical state of the gravitating matter (Bartelmann 2010).”
DeepSphere: a graph-based spherical CNN (2020, neutral): “Convergence maps represent the distribution of over- and underdensities of mass in the universe (see Bartelmann, 2010, for a review of gravitational lensing).”
GalSim: The modular galaxy image simulation toolkit (2014, background): “Weak gravitational lensing (for reviews see, e.g., Schneider, 2006; Bartelmann, 2010; Huterer, 2010) is a prime example of a scientiﬁc application that relies on reliable inference regarding the properties of astrophysical objects from imperfect images.”
CLASH: THE ENHANCED LENSING EFFICIENCY OF THE HIGHLY ELONGATED MERGING CLUSTER MACS J0416.1−2403 (2012, background): “…effects generally increase towards the central region of the cluster, where the projected mass density is often high enough to form multiple images of the same background source, depending also on the angular diameter distances involved (for reviews see Bartelmann 2010; Kneib & Natarajan 2011).”
HUBBLE SPACE TELESCOPE COMBINED STRONG AND WEAK LENSING ANALYSIS OF THE CLASH SAMPLE: MASS AND MAGNIFICATION MODELS AND SYSTEMATIC UNCERTAINTIES (2014, background): “…underlying matter distribution of the lens, dominated by an unseen dark matter (DM) component, and thanks to the magnification effect that distorts and enhances faint background objects to be detected through such cosmic lenses (e.g., Bartelmann 2010; Kneib & Natarajan 2011, for recent reviews).”
Formation of Galaxy Clusters (2012, background): “…via its X-ray emission and the Sunyaev-Zel’dovich eff ct and, in the case of Abell 1689, even the presence of invisible DM manifesting itself through gravitational lensi g of background galaxies distorting their images into extended, cluster-centric arcs (Bartelmann 2010, and references therein).”
Masses of Galaxy Clusters from Gravitational Lensing (2013, methodology): “We refer the interested reader to more thorough introductions into the subject by Bartelmann & Schneider (2001), Schneider (2006) or Bartelmann (2010).”
Galaxy Alignments: Observations and Impact on Cosmology (2015, background): “See Bartelmann & Schneider (2001); Hoekstra & Jain (2008); Munshi et al. (2008); Bartelmann (2010) for general reviews of weak lensing.”
The Intrinsic Alignment of Galaxies and its Impact on Weak Gravitational Lensing in an Era of Precision Cosmology (2014, background): “(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); Massey et al.”