Cosmological Applications of Gravitational Lensing

Blandford, R. D.; Narayan, Ramesh

doi:10.1146/annurev.aa.30.090192.001523

Cited by 409 publications

(322 citation statements)

References 0 publications

Supporting

Mentioning

316

Contrasting

Unclassified

Order By: Relevance

“…The most direct ones involve gravitational lensing (Zwicky 1937), which is a unique observational technique that allows to probe both the nature and distribution of dark matter (e.g., Van Waerbeke et al 2000;Metcalf & Madau 2001;Moustakas & Metcalf 2003;Hoekstra et al 2004;Massey et al 2007;Fu et al 2008;Rines et al 2013). The gravitational lensing observations, however, are usually possible only for a special set of circumstances, as the objects available for exploration are limited by the geometry of lens and sources (see, e.g., Blandford & Narayan 1992;Meylan et al 2006). Other methods for studying dark-luminous matter relations are applied on the scales of individual galaxies, where e.g., studies of rotation curves (Rubin et al 1978) of stars or gas clouds within individual galaxies are used to explore the hosting dark matter halo masses and density profiles, improving the understanding of the role of dark matter haloes in galaxy formation and evolution (e.g., Genzel et al 2017;Dekel et al 2017;Katz et al 2017).…”

Section: Introductionmentioning

confidence: 99%

The VIMOS Ultra Deep Survey

Durkalec

Fèvre

Pollo

et al. 2018

A&A

View full text Add to dashboard Cite

We present the study of the dependence of galaxy clustering on luminosity and stellar mass in the redshift range 2 < z < 3.5 using 3236 galaxies with robust spectroscopic redshifts from the VIMOS Ultra Deep Survey (VUDS), covering a total area of 0.92 deg 2 . We measure the two-point real-space correlation function w p (r p ) for four volume-limited sub-samples selected by stellar mass and four volume-limited sub-samples selected by M UV absolute magnitude. We find that the scale dependent clustering amplitude r 0 significantly increases with increasing luminosity and stellar mass. For the least luminous galaxies (M UV < −19.0) we measure a correlation length r 0 = 2.87 ± 0.22 h −1 Mpc and slope γ = 1.59 ± 0.07, while for the most luminous (M UV < −20.2) r 0 = 5.35 ± 0.50 h −1 Mpc and γ = 1.92 ± 0.25. This corresponds to a strong relative bias between these two sub-samples of ∆b/b * = 0.43. Fitting a 5-parameter HOD model we find that the most luminous (M UV < −20.2) and massive (M > 10 10 h −1 M ) galaxies occupy the most massive dark matter haloes with M h = 10 12.30 h −1 M . Similar to the trends observed at lower redshift, the minimum halo mass M min depends on the luminosity and stellar mass of galaxies and grows from M min = 10 9.73 h −1 M to M min = 10 11.58 h −1 M from the faintest to the brightest among our galaxy sample, respectively. We find the difference between these halo masses to be much more pronounced than is observed for local galaxies of similar properties. Moreover, at z ∼ 3, we observe that the masses at which a halo hosts, on average, one satellite and one central galaxy is M 1 ≈ 4M min over all luminosity ranges, significantly lower than observed at z ∼ 0 indicating that the halo satellite occupation increases with redshift. The luminosity and stellar mass dependence is also reflected in the measurements of the large scale galaxy bias, which we model as b g,HOD (> L) = 1.92 + 25.36(L/L * ) 7.01 . We conclude our study with measurements of the stellar-to-halo mass ratio (SHMR). We observe a significant model-observation discrepancy for low-mass galaxies, suggesting a higher than expected star formation efficiency of these galaxies.

show abstract

Section: Introductionmentioning

confidence: 99%

The VIMOS Ultra Deep Survey

Durkalec

Fèvre

Pollo

et al. 2018

A&A

View full text Add to dashboard Cite

show abstract

“…Therefore its measurement is useful to determine at first the length scale for a gravitational lensing system and its mass. Measuring the time delays in cosmological contexts, it is possible to determine the cosmological distance scale and hence the Hubble parameter [19,20,21]. This fact has drawn a great attention by the scientific community towards this kind of measurements.…”

Section: Introductionmentioning

confidence: 99%

Time Delay in Black Hole Gravitational Lensing as a Distance Estimator

Bozza

Mancini

2004

General Relativity and Gravitation

115

171

View full text Add to dashboard Cite

We calculate the time delay between different relativistic images formed by black hole gravitational lensing in the strong field limit. For spherically symmetric black holes, it turns out that the time delay between the first two images is proportional to the minimum impact angle. Their ratio gives a very interesting and precise measure of the distance of the black hole. Moreover, using also the separation between the images and their luminosity ratio, it is possible to extract the mass of the black hole. The time delay for the black hole at the center of our Galaxy is just few minutes, but for supermassive black holes with M = 10 8 ÷ 10 9 M⊙ in the neighbourhood of the Local Group the time delay amounts to few days, thus being measurable with a good accuracy.

show abstract

“…The study of multiply imaged quasars is one of the most promising way to measure cosmological parameters such as the Hubble parameter H 0 (Refsdal 1964;Blandford & Narayan 1992). Indeed, H 0 is related to two observables: the time-delay between the light curves of the quasar images and the mass distribution in the lens.…”

Section: Introductionmentioning

confidence: 99%

The lensing system towards the doubly imaged quasar SBS 1520+530

Fauré

Courbin

Kneib

et al. 2002

A&A

View full text Add to dashboard Cite

Abstract. The gravitational potential responsible for the lensing effect in SBS 1520+530 is studied over length scales from a few arc-seconds to a few arc-minutes. For this purpose, we use sharply deconvolved Hubble Space Telescope images in the optical and near-IR, in combination with ground based optical data obtained over a wider field-of-view. In particular, we have carried out a multi-color analysis in order to identify groups or clusters of galaxies along the line of sight. Photometric redshifts are measured for 139 galaxies unveiling significant excesses of galaxies 1.0 NW and 1.7 SW of the main lensing galaxy. The photometric redshift inferred both for the main lensing galaxy and for the galaxy concentrations is z = 0.9 +0.10 −0.25 . This is in rough agreement with the measured spectroscopic redshift of the main lensing galaxy, z = 0.71 (Burud et al. 2002), suggesting that it is part of a larger group or cluster. We investigate the impact of including the galaxy cluster, first on the modelling of the lensing system, and second on the expected time-delay between the two quasar images.

show abstract

Cosmological Applications of Gravitational Lensing

Cited by 409 publications

References 0 publications

The VIMOS Ultra Deep Survey

The VIMOS Ultra Deep Survey

Time Delay in Black Hole Gravitational Lensing as a Distance Estimator

The lensing system towards the doubly imaged quasar SBS 1520+530

Contact Info

Product

Resources

About