Constraining the cosmological parameters using strong lensing

Golse, G.; Kneib, Jean-Paul; Soucail, G.

doi:10.1051/0004-6361:20020448

Cited by 62 publications

(78 citation statements)

References 44 publications

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“…Gravitational arcs are powerful probes of the mass distribution in galaxies (Koopmans et al 2009;Barnabè et al 2011;Suyu et al 2012) and galaxy clusters (Kovner 1989;Miralda-Escudé 1993a;Hattori et al 1997) and can be used to constrain cosmological models (Bartelmann et al 1998;Oguri et al 2001;Golse et al 2002;Bartelmann et al 2003;Jullo et al 2010). The main techniques employed to extract information from gravitational arcs have been arc statistics (i.e.…”

Section: Introductionmentioning

confidence: 99%

“…counting the number of arcs in lens samples, Wu & Hammer 1993;Grossman & Saha 1994;Bartelmann & Weiss 1994) and inverse modeling (i.e. "deprojecting" the arcs in individual lens systems to determine the lens and the source, Kneib et al 1993;Keeton 2001;Golse et al 2002;Wayth & Webster 2006;Jullo et al 2007Jullo et al , 2010. The first requires large samples of arcs while the second needs detailed information on the lensing systems, typically imaging from space and lens and source redshifts.…”

Section: Introductionmentioning

confidence: 99%

“…For example, several studies using arc simulations have used these models (Oguri 2002;Meneghetti et al 2003Meneghetti et al , 2007. Popular codes for lens inversion (Golse et al 2002;Wayth & Webster 2006;Jullo et al 2007) are implemented using this type of model, too.…”

Section: Introductionmentioning

confidence: 99%

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Domain of validity for pseudo-elliptical NFW lens models

Dúmet-Montoya

Caminha

Makler

2012

A&A

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Context. Owing to their computational simplicity, models with elliptical potentials (pseudo-elliptical) are often used in gravitational lensing applications, in particular for mass modeling using arcs and for arc statistics. However, these models generally lead to negative mass distributions in some regions and to dumbbell-shaped surface density contours for high ellipticities. Aims. We revisit the physical limitations of the pseudo-elliptical Navarro-Frenk-White (PNFW) model, focusing on the behavior of the mass distribution close to the tangential critical curve, where tangential arcs are expected to be formed. We investigate the shape of the mass distribution on this region and the presence of negative convergence. We obtain a mapping from the PNFW to the NFW model with elliptical mass distribution (ENFW). We compare the arc cross section for both models, aiming to determine a domain of validity for the PNFW model in terms of its mass distribution and for the cross section. Methods. We defined a figure of merit to i) measure the deviation of the iso-convergence contours of the PNFW model to an elliptical shape, ii) assigned an ellipticity ε Σ to these contours, iii) defined a corresponding iso-convergence contour for the ENFW model. We computed the arc cross section using the "infinitesimal circular source approximation". Results. We extend previous work by investigating the shape of the mass distribution of the PNFW model for a broad range of the potential ellipticity parameter ε and characteristic convergence κ ϕ s . We show that the maximum value of ε to avoid dumbbellshaped mass distributions is explicitly dependent on κ ϕ s , with higher ellipticities (ε 0.5, i.e., ε Σ 0.65) allowed for small κ ϕ s . We determine a relation between the ellipticity of the mass distribution ε Σ and ε valid for any ellipticity. We also derive the relation of characteristic convergences, obtaining a complete mapping from PNFW to ENFW models, and provide fitting formulae for connecting the parameters of both models. Using this mapping, the cross sections for both models are compared, setting additional constraints on the parameter space of the PNFW model such that it reproduces the ENFW results. We also find that the negative convergence regions occur far from the arc formation region and should therefore not be a problem for studies with gravitational arcs. Conclusions. We conclude that the PNFW model is well-suited to model an elliptical mass distribution on a larger ε-κ ϕ s parameter space than previously expected. However, if we require the PNFW model to reproduce the arc cross section of the ENFW well, the ellipticity is more restricted, particularly for low κ ϕ s . The determination of a domain of validity for the PNFW model and the mapping to ENFW models could have implications for the use of PNFW models for the inverse modeling of lenses and for fast arc simulations, for example.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Domain of validity for pseudo-elliptical NFW lens models

Dúmet-Montoya

Caminha

Makler

2012

A&A

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“…Meanwhile, more than 100 giant arcs systems have been found (Gladders et al 2002, and references therein) and studied both to infer the cluster mass distribution and -using the magnification effect -to investigate the high redshift galaxy population (e.g., Colley et al 1996). The ensemble of arcs was also used for statistical inferences regarding consistency with various cosmological models (e.g., Bartelmann et al 1998;Golse et al 2002;Soucail et al 2004;Wambsganss et al 2004;Sand et al 2005). …”

Section: Introductionmentioning

confidence: 99%

An S-shaped arc in the galaxy cluster RX J0054.0-2823

Fauré

Giraud²,

Melnick

et al. 2006

A&A

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Context. The center of the galaxy cluster RX J0054.0-2823 at z = 0.292 is a dynamically active region that includes an interacting system of three galaxies surrounded by a large halo of intra-cluster light. Aims. We report here the discovery of an S-shaped feature of total length 11 in the central region of this cluster and discuss its physical nature. Methods. We test the gravitational lensing assumption by doing a mass modeling of the central part of the galaxy cluster. Results. We very naturally reproduce position and form of this S-shaped feature as a gravitationally lensed background object at redshift between 0.5 and 1.0. Conclusions. We conclude that the lensing nature is the very probable explanation for this S-shaped arc; the ultimate proof will be the spectroscopic confirmation by measuring the high redshift of this elongated feature with surface brightness V ∼ 24 mag arcsec −2 .

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“…Indeed, the scaling of the critical curves as a function of the source redshift is sensitive to the equation of state of dark energy (Link & Pierce, 1998, Golse, Kneib & Soucail, 2002, Sereno, 2002. A critical issue in the reliability of geometric measurements from cluster lensing is the sensitivity of the results to the mass distribution of the cluster.…”

Section: Introductionmentioning

confidence: 99%

Constraints on Dark Energy from Strong Gravitational Lensing by Galaxy Clusters

et al. 2004

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Abstract. We discuss two methods for constraining the equation of state of dark energy using strong gravitational lensing by galaxy clusters. In the so called "arc statistics" approach, we compare the cluster efficiency for producing giant arcs in several dark-energy cosmologies and in the "standard" ΛCDM and OCDM models. We find that the expected abundance of gravitational arcs depends on the equation of state of dark energy and reflects the dependence of halo concentrations on cosmology. In agreement with results in previous works, the lensing cross section is very sensitive to dynamical processes occurring in the lenses. Then we use gravitational arcs for tracing the position of the lens critical curves and we measure their scaling with the source redshift in a variety of cosmological models. We find that there is a degeneracy between several lens properties and the equation of state of dark energy which can be broken only after an extremely precise modeling of the lens. Instead of using this "golden lens" approach, we check whether combining the information from a statistical sample of clusters we can distinguish among the various cosmologies. We test the method on a sample of numerically simulated clusters and we reproduce the results expected from the analytic models.

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Constraining the cosmological parameters using strong lensing

Cited by 62 publications

References 44 publications

Domain of validity for pseudo-elliptical NFW lens models

Domain of validity for pseudo-elliptical NFW lens models

An S-shaped arc in the galaxy cluster RX J0054.0-2823

Constraints on Dark Energy from Strong Gravitational Lensing by Galaxy Clusters

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