Strong Lensing by Galaxies

By T. Treu. 2010

383 citations recorded by the source corpus.

Strong lensing is a powerful tool to address three major astrophysical issues: understanding the spatial distribution of mass at kiloparsec and subkiloparsec scale, where baryons and dark matter interact to shape galaxies as we see them; determining the overall geometry, content, and kinematics of the Universe; and studying distant galaxies, black holes, and active nuclei that are too small or too faint to be resolved or detected with current instrumentation. After summarizing strong gravitational lensing fundamentals, I present a selection of recent important results. I conclude by discussing the exciting prospects of strong gravitational lensing in the next decade.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/2b08a6e566e504fc66222abee3826d7c454b3f52

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In Astronomy and Astrophysics

In Atomic and Molecular Physics, and Optics

Citations in the corpus

THE SLOAN LENS ACS SURVEY. X. STELLAR, DYNAMICAL, AND TOTAL MASS CORRELATIONS OF MASSIVE EARLY-TYPE GALAXIES (2010, background): “…profile and time delays (e.g., Wucknitz 2002), if one assumes an isothermal prior then the inferred Hubble Constant will typically be biased low by 10% if no other direct measure of the mass slope is available (see Oguri 2007; Dobke & King 2006; Kochanek 2006; Treu 2010, and references therein).”
GRAVITATIONAL LENS MODELS BASED ON SUBMILLIMETER ARRAY IMAGING OF HERSCHEL-SELECTED STRONGLY LENSED SUB-MILLIMETER GALAXIES AT z > 1.5 (2013, methodology): “To represent the lens mass profile, we use Nlens singular isothermal ellipsoid (SIE) profiles, where Nlens is the number of lensing galaxies found from the best available optical or near-IR imaging (a multitude of evidence supports the SIE as a reasonable choice; for a recent review, see Treu 2010).”
PRISM (Polarized Radiation Imaging and Spectroscopy Mission): an extended white paper (2013, background): “uring the mass distribution of dark matter halos as a function of redshift. Samples of thousands strongly lensed galaxies are also essential for many other astrophysical and cosmological applications [210]. Further constraints on the evolution of large scale structure, hence on cosmological paramete”
CMU DeepLens: deep learning for automatic image-based galaxy–galaxy strong lens finding (2017, background): “See, e.g., Treu (2010) for a review of results using strong lensing by galaxies.”
Mining for Dark Matter Substructure: Inferring Subhalo Population Properties from Strong Lenses with Machine Learning (2019, methodology): “This approach scales well to the expected large number of lenses expected in upcoming surveys (Oguri & Marshall 2010; Treu 2010; Collett 2015).”
Galaxy Masses: A Review (2013, background): “This section is neither complete nor unbiased and we refer to Schneider (2006a) or Treu (2010) for more thorough theoretical and observational overviews.”
The distribution of dark matter in galaxies (2018, background): “…R. 4.10 Strong lensing Gravitational lensing occurring in very aligned galaxy-galaxy-observer structures magnifies and distorts the images of a distant galaxy providing us with relevant information on the mass structure of the intervening galaxy so as of the background source (see Treu 2010).”
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).”
TWO ACCURATE TIME-DELAY DISTANCES FROM STRONG LENSING: IMPLICATIONS FOR COSMOLOGY (2012, methodology): “More details on the subject can be found in, e.g., Schneider et al. (2006), Jackson (2007), Treu (2010), and Suyu et al. (2010).”
THE GRISM LENS-AMPLIFIED SURVEY FROM SPACE (GLASS). I. SURVEY OVERVIEW AND FIRST DATA RELEASE (2015, background): “Exploiting lensing magnification (Treu 2010; Coe et al. 2014) is one of the motivations behind many HST cluster surveys (e.g., Smith et al. 2001; Postman et al. 2012; Bayliss et al. 2014) and the main driver of the ongoing Hubble Frontier Field (HFF) initiative (J. Lotz et al. 2015, in preparation).”
H0LiCOW - V. New COSMOGRAIL time delays of HE 0435-1223: H0 to 3.8 per cent precision from strong lensing in a flat ΛCDM model (2016, methodology): “In this case, the analysis benefits greatly from independent measurements of H0 from observations of distance probes such as the distance ladder or water masers (see e.g. Treu 2010; Weinberg et al. 2013; Treu & Marshall 2016, for a review).”
PICO: Probe of Inflation and Cosmic Origins (2019, background): “1%, more than two orders of magnitude lower [187].”
Theoretical Challenges in Galaxy Formation (2016, background): “…have contributed to our knowledge of the dark matter content of massive galaxies, which have typical contributions of 5% to 20% within their stellar half-light radii (e.g. Koopmans et al. 2009, Treu 2010, see also lensing measurements of the stellar-to-halo mass ratio, Mandelbaum et al. 2006).”
Gravitational probes of dark matter physics (2017, background): “However, in this regime of halo mass, we usually discuss strong gravitational lensing as a probe of the abundance of small halos [303, 305, 304].”
Two Remarkably Luminous Galaxy Candidates at z ≈ 10–12 Revealed by JWST (2022, background): “Here we make a simple estimate of how lensed our sources are by assuming their neighbors are singular isothermal spheres (e.g., Fort & Mellier 1994; Schneider et al. 2006; Treu 2010) following e.g., McLure et al. (2006); Oesch et al. (2014); Matthee et al. (2017).”
Time delay cosmography (2016, background): “We refer the readers to recent (Bartelmann 2010; Ellis 2010; Treu 2010; Treu et al. 2012; Jackson 2013, 2015; Treu and Ellis 2015) and not-so-recent (Blandford and Narayan 1992; Courbin et al. 2002; Kochanek et al. 2004; Falco 2005; Schneider et al. 2006) excellent reviews and textbooks (Schneider…”