Gravitational Imaging of CDM Substructure

By Leon V. E. Koopmans. 2005

162 citations recorded by the source corpus.

We propose the novel method of ``gravitational imaging'' to detect and quantify luminous and dark-matter substructure in gravitational-lens galaxies. The method utilizes highly-magnified Einstein rings and arcs as sensitive probes of small perturbations in the lens potential (due to the presence of mass substructure), reconstructing the gravitational lens potential non-parametrically. Numerical simulations show that the implemented algorithm can reconstruct the smooth mass distribution of a typical lens galaxy - exhibiting reasonable signal-to-noise Einstein rings - as well as compact substructure with masses as low as M_sub~10^-3 M_lens, if present. ``Gravitational imaging'' of pure dark-matter substructure around massive galaxies can provide a new window on the standard cold-dark-matter paradigm, using very different physics than ground-based direct-detection experiments, and probe the hierarchical structure-formation model which predicts this substructure to exist in great abundance.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/3be8a3abb9788d44e10a32fee24515d04e48e509

How researchers see this paper

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In Astronomy and Astrophysics

1. T. Treu
2. P. J. Marshall
3. Leon V. E. Koopmans
4. T. Collett
5. Dominique Sluse
6. M. Auger
7. A. Bolton
8. R. Gavazzi

In Nuclear and High Energy Physics

1. S. Vegetti
2. T. Treu
3. A. Bolton
4. P. J. Marshall
5. M. Auger
6. R. Gavazzi
7. L. A. Moustakas
8. S. Burles

Citations in the corpus

• DETECTION OF LENSING SUBSTRUCTURE USING ALMA OBSERVATIONS OF THE DUSTY GALAXY SDP.81 (2016, background): “…completely devoid of baryons (e.g., Mao & Schneider 1998; Metcalf & Madau 2001; Dalal & Kochanek 2002; Moustakas & Metcalf 2003; Kochanek & Dalal 2004; Koopmans 2005; Keeton et al. 2006; Vegetti & Koopmans 2009; Vegetti et al. 2012; Nierenberg et al. 2014; Xu et al. 2015b; Cyr-Racine et al. 2015).”
• H0LiCOW – I. H0 Lenses in COSMOGRAIL's wellspring: program overview (2016, background): “…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 et al. 2016).”
• A Bayesian approach to strong lensing modelling of galaxy clusters (2007, background): “Since 1997, non-parametric modelling has been intensively tested and greatly improved to overcome the lack of constraints very common in strong lensing (e.g. Koopmans 2005; Diego et al. 2005; Kochanek 2006).”
• 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).”
• Bayesian strong gravitational-lens modelling on adaptive grids: objective detection of mass substructure in Galaxies (2008, methodology): “Both d ands are vectors that describe the surface brightness distributions on a set of spatial pointsxdi andy s j in the lens and source plane, respectively (e.g., Warren & Dye 2003; Koopmans 2005; Suyu et al. 2006).”
• 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): “…process of finding the best-fitting pixellated source brightness distribution given a lens potential model and an observed image has been studied by, for examples, Wallington et al. (1996), Warren & Dye (2003), Treu & Koopmans (2004), Koopmans (2005), Dye & Warren (2005) and Brewer & Lewis (2006).”
• Inference of the cold dark matter substructure mass function at z = 0.2 using strong gravitational lenses (2014, methodology): “The gravitational imaging technique allows the detection of mass substructure in lens galaxies as linear localized and pixelized corrections to the overall smooth analytic lens potential, as described in Section 4.1 (Koopmans 2005; Vegetti & Koopmans 2009a).”
• Detection of a dark substructure through gravitational imaging (2009, background): “As described by Koopmans (2005) and Vegetti & Koopmans (2009a), the information contained in multiple images and Einstein rings of extended sources, can also be used.”