Multi-wavelength study of the gravitational lens system RXS J113155.4-123155

Sluse, Dominique; Claeskens, Jean-François; Altiéri, B.; Cabanac, R.; Garcet, O.; Hutsemékers, Damien; Jean, C.; Smette, A.; Surdej, Jean

doi:10.1051/0004-6361:20053148

Cited by 29 publications

(24 citation statements)

References 55 publications

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“…Photometry is also affected by the presence of the ring. We derive an absolute photometry about 0.4 mag brighter than Sluse et al (2006) but obtain compatible flux ratios. The remnant systematic structures in the final residual map are also caused by this very bright ring, which affects the PSFs and degrades their quality.…”

Section: Discussionmentioning

confidence: 73%

“…Preliminary time delays have been proposed by Morgan et al (2006) and revised estimates will be published in Kozłovski et al (in prep.). The system was characterized in details in terms of astrometry and photometry by Sluse et al (2006). Claeskens et al (2006) modeled it and also reconstructed the source, which appears to be a type 1 Seyfert spiral galaxy.…”

Section: An Overview Of Our Samplementioning

confidence: 99%

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COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses

Chantry¹,

Sluse²,

Magain³

2010

A&A

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Aims. We attempt to place very accurate positional constraints on seven gravitationally lensed quasars currently being monitored by the COSMOGRAIL collaboration, and shape parameters for the light distribution of the lensing galaxy. We attempt to determine simple mass models that reproduce the observed configuration and predict time delays. We finally test, for the quads, whether there is evidence of astrometric perturbations produced by substructures in the lensing galaxy, which may preclude a good fit with the simple models. Methods. We apply the iterative MCS deconvolution method to near-IR HST archival data of seven gravitationally lensed quasars. This deconvolution method allows us to differentiate the contributions of the point sources from those of extended structures such as Einstein rings. This method leads to an accuracy of 1-2 mas in the relative positions of the sources and lens. The limiting factor of the method is the uncertainty in the instrumental geometric distortions. We then compute mass models of the lensing galaxy using state-of-the-art modeling techniques. Results. We determine the relative positions of the lensed images and lens shape parameters of seven lensed quasars: HE 0047-1756, RX J1131-1231, SDSS J1138+0314, SDSS J1155+6346, SDSS J1226-0006, WFI J2026-4536, and HS 2209+1914. The lensed image positions are derived with 1-2 mas accuracy. Isothermal and de Vaucouleurs mass models are calculated for the whole sample. The effect of the lens environment on the lens mass models is taken into account with a shear term. Doubly imaged quasars are equally well fitted by each of these models. A large amount of shear is necessary to reproduce SDSS J1155+6346 and SDSS J1226-006. In the latter case, we identify a nearby galaxy as the dominant source of shear. The quadruply imaged quasar SDSS J1138+0314 is reproduced well by simple lens models, which is not the case for the two other quads, RX J1131-1231 and WFI J2026-4536. This might be the signature of astrometric perturbations caused by massive substructures in the galaxy, which are unaccounted for by the models. Other possible explanations are also presented.

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Section: Discussionmentioning

confidence: 73%

Section: An Overview Of Our Samplementioning

confidence: 99%

COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses

Chantry¹,

Sluse²,

Magain³

2010

A&A

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“…In order to derive the luminosity of J1131-1231 and H1413+117 as for the other systems, we performed an approximate flux calibration of their spectra, by matching the broad-band magnitudes derived from the spectra with published absolute photometry. We used the I-band magnitude of Sluse et al (2006) for J1131-1231 and the H-band 2MASS photometry H = 14.531 ± 0.054 for H1413+117.…”

Section: The Extended Samplementioning

confidence: 99%

“…(1) Wisotzki et al (2004); (2) Fadely & Keeton (2011); (3) Courbin et al (2011); (4) Schechter et al (1998); (5) Oguri et al (2004); (6) Morgan et al (2004); (7) Vuissoz et al (2008); (8) CASTLES; (9) Chantry et al (2010); (10) Sluse et al (2012); (11) Lehár et al (2000); (12) Inada et al (2005); (13) Sluse et al (2008b); (14) Falco et al (1999); (15) Burud et al (2002); (16) Blackburne et al (2011); (17) Eigenbrod et al (2006a); (18) Sluse et al (2006); (19) Falco et al (1996); (20) Chantry & Magain (2007); (21) MacLeod et al (2009). associated to intrinsic variability and, in a few cases, systematic errors associated to differential extinction and microlensing.…”

Section: Accuracy Of the Intrinsic Flux Ratiosmentioning

confidence: 99%

Microlensing of the broad line region in 17 lensed quasars

Sluse

Hutsemékers

Courbin

et al. 2012

A&A

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184

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When an image of a strongly lensed quasar is microlensed, the different components of its spectrum are expected to be differentially magnified owing to the different sizes of the corresponding emitting region. Chromatic changes are expected to be observed in the continuum while the emission lines should be deformed as a function of the size, geometry and kinematics of the regions from which they originate. Microlensing of the emission lines has been reported only in a handful of systems so far. In this paper we search for microlensing deformations of the optical spectra of pairs of images in 17 lensed quasars with bolometric luminosities between 10 44.7−47.4 erg/s and black hole masses 10 7.6−9.8 M . This sample is composed of 13 pairs of previously unpublished spectra and four pairs of spectra from literature. Our analysis is based on a simple spectral decomposition technique which allows us to isolate the microlensed fraction of the flux independently of a detailed modeling of the quasar emission lines. Using this technique, we detect microlensing of the continuum in 85% of the systems. Among them, 80% show microlensing of the broad emission lines. Focusing on the most common emission lines in our spectra (C iii] and Mg ii) we detect microlensing of either the blue or the red wing, or of both wings with the same amplitude. This observation implies that the broad line region is not in general spherically symmetric. In addition, the frequent detection of microlensing of the blue and red wings independently but not simultaneously with a different amplitude, does not support existing microlensing simulations of a biconical outflow. Our analysis also provides the intrinsic flux ratio between the lensed images and the magnitude of the microlensing affecting the continuum. These two quantities are particularly relevant for the determination of the fraction of matter in clumpy form in galaxies and for the detection of dark matter substructures via the identification of flux ratio anomalies.

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“…For example, the statistics of lensed quasars or galaxies lensed by clusters into giant arcs can be used to study the population of lenses, their distribution in redshift space, mass, and hence the cosmological model. Stronglensing systems may also be studied individually, in order to obtain a detailed understanding of the structure and the distribution of matter in the lensing object and the source (see, e.g., Claeskens et al 2000Claeskens et al , 2006Broadhurst et al 2000;Shapiro & Iliev 2000;Cohn et al 2001;Belokurov et al 2001;Patnaik & Narasimha 2001;Inada et al 2003;Fassnacht et al 2006;Sluse et al 2006;Wayth et al 2005). In this paper we are mostly interested in the former problem, namely, the statistics of strong-lensing events.…”

Section: Introductionmentioning

confidence: 99%

Testing a New Analytic Model for Gravitational Lensing Probabilities

Das¹,

Ostriker²

2006

ApJ

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We study gravitational lensing with a multiple lens plane approach, proposing a simple analytical model for the probability density function ( pdf ) of the dark matter convergence, , for the different lens planes in a given cosmology as a function of redshift and smoothing angle, . The model is fixed solely by the variance of , which in turn is fixed by the amplitude of the power spectrum, 8 . We test the pdf against a high-resolution tree particle-mesh simulation and find that it is far superior to the Gaussian or the lognormal, especially for small values of T1 0 and at large values of relevant to strong lensing. With this model, we predict the probabilities of strong lensing by a single plane or by multiple planes. We find that for $ 10 00 , a single plane accounts for almost all ($98%) of the stronglensing cases for source redshift unity. However, for a more typical source redshift of 4, about 12% of the stronglensing cases will result from the contribution of a secondary clump of matter along the line of sight, introducing a systematic error in the determination of the surface density of clusters, typically overestimating it by about 2%-5%. We also find that matter inhomogeneities introduce a dispersion in the value of the angular diameter distance about its cosmological mean. The probable error relative to the mean increases with redshift to a value of about 8% for z ' 6 and $ 10 00 .

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Multi-wavelength study of the gravitational lens system RXS J113155.4-123155

Cited by 29 publications

References 55 publications

COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses

COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses

Microlensing of the broad line region in 17 lensed quasars

Testing a New Analytic Model for Gravitational Lensing Probabilities

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