Semilinear Gravitational Lens Inversion

By S. Warren, S. Dye. 2003

177 citations recorded by the source corpus.

We describe a new method for analyzing gravitational lens images, for the case in which the source light distribution is pixelized. The method is suitable for high-resolution, high signal-to-noise ratio (S/N) data of a multiply imaged extended source. For a given mass distribution, we show that the step of inverting the image to obtain the deconvolved pixelized source light distribution, and the uncertainties, is a linear one. This means that the only parameters of the nonlinear problem are those required to model the mass distribution. This greatly simplifies the search for a minimum χ2 fit to the data and speeds up the inversion. The method is extended in a straightforward way to include linear regularization. We apply the method to simulated Einstein ring images and demonstrate the effectiveness of the inversion for both the unregularized and regularized cases.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/5d62a5da80ec22e0068932dc8e4ebf935459ea2e

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In Astronomy and Astrophysics

Citations in the corpus

H0LiCOW – I. H0 Lenses in COSMOGRAIL's wellspring: program overview (2016, background): “…extended images to constrain precisely within a few percent the lens potential at the location of the multiple images (e.g., Kochanek et al. 2001; Warren & Dye 2003; Treu & Koopmans 2004; Koopmans 2005; Dye et al. 2008; Vegetti & Koopmans 2009; Suyu et al. 2009, 2013; Birrer et al. 2015b; Chen…”
Mining for Dark Matter Substructure: Inferring Subhalo Population Properties from Strong Lenses with Machine Learning (2019, methodology): “…using shapelet basis sets(Birrer et al. 2015; Tagore & Jackson 2016; Birrer & Amara 2018) and methods based on regularized linear inversion on grids(Warren & Dye 2003; Suyu et al. 2006; Tagore & Keeton 2014; Nightingale et al. 2018) have been introduced as ways to model more complicated source…”
The Sloan Lens ACS Survey. VI. Discovery and Analysis of a Double Einstein Ring (2008, methodology): “The second approach is the linear source inversion and parametric potential fitting method described by Warren & Dye (2003), Treu & Koopmans (2004), Koopmans (2005) and Suyu et al. (2006).”
The CFHTLS strong lensing legacy survey - I. Survey overview and T0002 release sample (2006, unknown): “A large number of algorithms of gravitational lens modelling are available (e.g. Kneib et al. 1993; Saha & Williams 1997; Keeton 2001; Warren & Dye 2003; Brewer & Lewis 2006).”
DETECTION OF LENSING SUBSTRUCTURE USING ALMA OBSERVATIONS OF THE DUSTY GALAXY SDP.81 (2016, background): “The source reconstruction that maximizes the unmarginalized posterior (at fixed lens model) is also analytic, and is given by (Warren & Dye 2003; Suyu et al. 2006) S = A−1B. (4) We note that the above formalism is general to multifrequency data.”
Bayesian strong gravitational-lens modelling on adaptive grids: objective detection of mass substructure in Galaxies (2008, methodology): “A semilinear technique for the reconstruction of grid-based sources, given a parametric lens potential, was first introduced by Warren & Dye (2003).”
H0LiCOW - IV. Lens mass model of HE 0435-1223 and blind measurement of its time-delay distance for cosmology (2016, background): “Deep, high-resolution imaging is required to accurately model the lens using the extended source images, which is needed to break degeneracies between the mass profile and the underlying cosmology (e.g., Kochanek 2002; Warren & Dye 2003).”
HerMES: CANDIDATE GRAVITATIONALLY LENSED GALAXIES AND LENSING STATISTICS AT SUBMILLIMETER WAVELENGTHS (2012, methodology): “For simplicity in the modeling and to avoid computational costs associated with pixelized inversion techniques (Warren & Dye 2003; Treu & Koopmans 2004; Suyu et al. 2006), we make use of an analytical description of the source plane light distribution by assuming a Gaussian radial profile with…”
Time delay cosmography (2016, background): “and others are complex (Warren and Dye 2003; Treu and Koopmans 2004; Brewer and Lewis 2006; Suyu et al. 2006; Suyu and Halkola 2010), or where flexibly parametrized “corrections” are added to simply parametrized models (Koopmans 2005; Vegetti and”
Gravitational Imaging of CDM Substructure (2005, methodology): “…can then be expressed as the set of linear equations BL(ψ)~s = ~d, (1) 2 We note that the implementation of the semi-linear inversion technique in Warren & Dye (2003) is similar to that in Treu & Koopmans (2004) and does not require the inversion of the lens equation as previously suggested.”
Two-dimensional kinematics of SLACS lenses – III. Mass structure and dynamics of early-type lens galaxies beyond z ≃ 0.1 (2011, methodology): “By employinga pixelated source reconstruction method (see e.g. Warren & Dye 2003, Koopmans 2005, Suyu et al. 2006) for the lensing and some flavour of the Schwarzschild orbit superposition method (Schwarzschild 1979; see Thomas 2010 for a review of the developments of this technique) for the…”
A Bayesian analysis of regularized source inversions in gravitational lensing (2006, unknown): “As the first example to demonstrate the Bayesian approach to source inversion, we use the same lens potential and source brightness distribution as that in Warren & Dye (2003).”
THE SLOAN LENS ACS SURVEY. X. STELLAR, DYNAMICAL, AND TOTAL MASS CORRELATIONS OF MASSIVE EARLY-TYPE GALAXIES (2010, background): “Nevertheless, additional external information on the mass density slope, such as that inferred from multiply-imaged extended sources (Warren & Dye 2003; Suyu et al. 2006) and from stellar kinematics (Treu & Koopmans 2002; Koopmans et al. 2003), can help to break these degeneracies and provide…”