Time delay cosmography

By T. Treu, P. J. Marshall. The Astronomy and Astrophysics Review, 2016

190 citations recorded by the source corpus.

Gravitational time delays, observed in strong lens systems where the variable background source is multiply imaged by a massive galaxy in the foreground, provide direct measurements of cosmological distance that are very complementary to other cosmographic probes. The success of the technique depends on the availability and size of a suitable sample of lensed quasars or supernovae, precise measurements of the time delays, accurate modeling of the gravitational potential of the main deflector, and our ability to characterize the distribution of mass along the line of sight to the source. We review the progress made during the last 15 years, during which the first competitive cosmological inferences with time delays were made, and look ahead to the potential of significantly larger lens samples in the near future.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/5fab7f69bfef048c63630d99dcd95624da66291c

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Citations in the corpus

H0LiCOW - IV. Lens mass model of HE 0435-1223 and blind measurement of its time-delay distance for cosmology (2016, background): “The time-delay distance is primarily sensitive to H0, with weaker dependence on other cosmological parameters (e.g., Coe & Moustakas 2009; Treu & Marshall 2016).”
TDCOSMO. I. An exploration of systematic uncertainties in the inference of $H_0$ from time-delay cosmography (2019, background): “While investigating potential sources of systematic uncertainties was an important first step, meeting the goal of 1% precision and accuracy with time-delay cosmography (e.g., Suyu 2012; Treu & Marshall 2016), requires additional and continued efforts over the coming years.”
H0LiCOW – I. H0 Lenses in COSMOGRAIL's wellspring: program overview (2016, methodology): “…method was first proposed by Refsdal (1964) even before the discovery of the first strong gravitational lens system (Walsh et al. 1979), consisting of a foreground mass distribution that is located close along the line of sight to a background source (see Treu & Marshall 2016, for a recent review).”