The mass profile of early-type galaxies in overdense environments: the case of the double source-plane gravitational lens SL2SJ02176-0513

Tu, Hong; Gavazzi, R.; Limousin, M.; Cabanac, R.; Marshall, Phil; Fort, B.; Treu, Tommaso; Pelló, R.; Jullo, Eric; Kneib, Jean-Paul; Sygnet, J.-F.

doi:10.1051/0004-6361/200911963

Cited by 35 publications

(55 citation statements)

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“…Note also that Tu et al (2009) found that another system of images is associated with this lens. These images correspond to a more distant source, and the light from this second source is influenced by the potential of the first source.…”

Section: Previous Workmentioning

confidence: 74%

“…Another possibility is to assume that the two images are not merged and that the yellow contour in Fig. 1 corresponds to the image of the second bright spot, as considered by Tu et al (2009). Still since the separation between the images is large the slope of the local model would have to be small.…”

Section: General Properties Of the Solutionmentioning

confidence: 99%

“…The first re-construction of a gravitational lens by the perturbative approach is described in Alard (2009), this work offers an overview presentation of the methods and algorithms that will be used in this paper. The lens SL2S02176-0513 was already modeled by Tu et al (2009) with conventional methods. Tu et al (2009) identified three components in the lens: the stellar component, the dark matter halo associated with the galaxy, and an external influence from a nearby group of galaxies.…”

Section: Introductionmentioning

confidence: 99%

“…The lens SL2S02176-0513 was already modeled by Tu et al (2009) with conventional methods. Tu et al (2009) identified three components in the lens: the stellar component, the dark matter halo associated with the galaxy, and an external influence from a nearby group of galaxies. The surface density of the bright part is modeled as a Sersic profile, while the dark component is represented with an elliptical pseudo isothermal sphere.…”

Section: Introductionmentioning

confidence: 99%

“…The position of the SIS is not a free parameter, it is derived from X-ray observations (Geach et al 2007). The model proposed by Tu et al (2009) is physically motivated, although it has a considerable number of free parameters, and the exploration of the parameter space is always a difficult task. The minimization surface in the parameter space is complex, with the usual presence of several minima of similar depth resulting in a degeneracy of the solution.…”

Section: Introductionmentioning

confidence: 99%

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Separating inner and outer contributions in gravitational lenses with the perturbative method

Alard¹

2010

A&A

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Context. This paper presents a reconstruction of the gravitational lens SL2S02176-0513 with the singular perturbative method presented in Alard (2007, MNRAS, 382, L58) and Alard (2008, MNRAS, 388, 375). Aims. The ability of the perturbative method to separate the inner and outer contributions of the potential in gravitational lenses is tested using SL2S02176-0513. The gravitational field of the central galaxy is dominated by a nearby group of galaxies located at a distance of a few critical radius in this lens. Methods. The perturbative functionals are re-constructed using local polynomials. The polynomial interpolation is smoothed by Fourier series, and numerically fitted to the Hubble Space Telescope data with a non linear minimization procedure. The potential inside and outside the critical circle is derived from the reconstruction of the perturbative fields. Results. The inner and outer potential contours are very different. The inner contours are consistent with the central galaxy, while the outer contours are fully consistent with the perturbation introduced by the group of galaxies. Conclusions. The ability of the perturbative method to separate the inner and outer contribution is confirmed, and indicates that in the perturbative approach the field of the central deflector can be separated from outer perturbations. The separation of the inner and outer contribution is especially important to study the shape of dark matter halos and for the statistical analysis of the effect of dark matter substructures.

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Section: Previous Workmentioning

confidence: 74%

Section: General Properties Of the Solutionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Separating inner and outer contributions in gravitational lenses with the perturbative method

Alard¹

2010

A&A

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Extended surface brightness modeling of three sources strongly lensed by an ultra-massive elliptical galaxy

Bolamperti

2022

Proc. IAU

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Rare systems with multiple sources strongly lensed by a single galaxy provide the most robust way to explore the geometry of the Universe and to study the inner mass structure of lens galaxies. We present here a study of the SDSS J0100+1818 deflector, analyzing its total and baryonic mass distributions. The system comprises an ultra-massive early-type galaxy, surrounded by ten multiple images of three background sources. Exploiting high-resolution HST photometry and VLT/X-shooter spectroscopy we conduct a strong lensing analysis with the software GLEE to reconstruct the complex surface brightness distributions of the background sources over approximately 7200 HST pixels. These results are presented in our recent paper, Bolamperti et al. (2023). Finally, we present some preliminary results from new VLT/MUSE observations, that will allow us to build a new strong lensing+dynamics joint model and measure the values of the total matter density and of the cosmological constant parameters, Ωm and ΩΛ.

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Strong lensing as a probe of the mass distributionbeyondthe Einstein radius

Limousin

Jullo

Richard

et al. 2010

A&A

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Strong lensing has been employed extensively to obtain accurate mass measurements within the Einstein radius. We here use strong lensing to probe mass distributions beyond the Einstein radius. We consider SL2S J08544-0121, a galaxy group at redshift z = 0.35 with a bimodal light distribution and with a strong lensing system located at one of the two luminosity peaks separated by ∼54 . The main arc and the counter-image of the strong lensing system are located at ∼5 and ∼8 from the lens galaxy centre. We find that a simple elliptical isothermal potential cannot satisfactorily reproduce the strong lensing observations. However, with a mass model for the group built from its light-distribution with a smoothing factor s and a mass-to-light ratio M/L, we obtain an accurate reproduction of the observations. We find M/L = 98 ± 27 (i band, solar units, not corrected for evolution) and s = 20 ± 9 (2σ confidence level). Moreover, we use weak lensing to independently estimate the mass of the group, and find a consistent M/L in the range 66-146 (1-σ confidence level). This suggests that light is a good tracer of mass. Interestingly, this also shows that a strong lensing-only analysis (on scales of ∼10 ) can constrain the properties of nearby objects (on scales of ∼100 ). We characterise the type of perturbed strong lensing system that allows such an analysis: a non dominant strong lensing system used as a test particle to probe the main potential. This kind of analysis needs to be validated with other systems because it could provide a quick way of probing the mass distribution of clusters and groups. This is particularly relevant in the context of forthcoming wide-field surveys, which will yield thousands of strong lenses, some of which perturbed enough to pursue the analysis proposed in this paper.

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The mass profile of early-type galaxies in overdense environments: the case of the double source-plane gravitational lens SL2SJ02176-0513

Cited by 35 publications

References 58 publications

Separating inner and outer contributions in gravitational lenses with the perturbative method

Separating inner and outer contributions in gravitational lenses with the perturbative method

Extended surface brightness modeling of three sources strongly lensed by an ultra-massive elliptical galaxy

Strong lensing as a probe of the mass distributionbeyondthe Einstein radius

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