Multi-wavelength study of the gravitational lens system RXS J1131-1231

Sluse, Dominique; Claeskens, Jean-François; Hutsemékers, Damien; Surdej, Jean

doi:10.1051/0004-6361:20066821

Cited by 105 publications

(121 citation statements)

References 44 publications

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“…(7)). This is equivalent to adopt a value of μ c as close as possible to 1, thus ensuring that the macro-and microamplifications are best separated (see also Sluse et al 2007). Unless M A, this method provides a reasonably accurate estimate of M, and then of μ c .…”

Section: Discussionmentioning

confidence: 99%

Microlensing in H1413+117: disentangling line profile emission and absorption in a broad absorption line quasar

Hutsemékers

Borguet

Sluse

et al. 2010

A&A

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On the basis of 16 years of spectroscopic observations of the four components of the gravitationally lensed broad absorption line (BAL) quasar H1413+117, covering the ultraviolet to visible rest-frame spectral range, we analyze the spectral differences observed in the P Cygni-type line profiles and have used the microlensing effect to derive new clues to the BAL profile formation. We first find that the absorption gradually decreases with time in all components and that this intrinsic variation is accompanied by a decrease in the intensity of the emission. We confirm that the spectral differences observed in component D can be attributed to a microlensing effect lasting at least a decade. We show that microlensing magnifies the continuum source in image D, leaving the emission line region essentially unaffected. We interpret the differences seen in the absorption profiles of component D as the result of an emission line superimposed onto a nearly black absorption profile. We also find that the continuum source and a part of the broad emission line region are likely de-magnified in component C, while components A and B are not affected by microlensing. Differential dust extinction is measured between the A and B lines of sight. We show that microlensing of the continuum source in component D has a chromatic dependence compatible with the thermal continuum emission of a standard Shakura-Sunyaev accretion disk. Using a simple decomposition method to separate the part of the line profiles affected by microlensing and coming from a compact region from the part unaffected by this effect and coming from a larger region, we disentangle the true absorption line profiles from the true emission line profiles. The extracted emission line profiles appear double-peaked, suggesting that the emission is occulted by a strong absorber, narrower in velocity than the full absorption profile, and emitting little by itself. We propose that the outflow around H1413+117 is constituted by a high-velocity polar flow and a denser, lower velocity disk seen nearly edge-on. Finally, we report on the first ground-based polarimetric measurements of the four components of H1413+117.

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Section: Discussionmentioning

confidence: 99%

Microlensing in H1413+117: disentangling line profile emission and absorption in a broad absorption line quasar

Hutsemékers

Borguet

Sluse

et al. 2010

A&A

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“…In order to provide a more global overview of the variety of signals which may be observed, we completed our main sample with five systems we studied elsewhere: SDSS J0924+0219 (Eigenbrod et al 2006a), H1413+117 (Hutsemékers et al 2010), J1131-1231 (Sluse et al 2007), HE 2149-2745 (Burud et al 2002), and Q2237+0305 (Eigenbrod et al 2008;Sluse et al 2011). This is not a complete list of known microlensed quasars (see e.g.…”

Section: The Extended Samplementioning

confidence: 99%

“…Pooley et al 2007;Floyd et al 2009;Hutsemékers et al 2010;Dai et al 2010;Blackburne et al 2011;Muñoz et al 2011). Studies of BLR microlensing are more sparse and detections have been reported only for a handful of systems (Richards et al 2004;Wayth et al 2005; Keeton et al 2006;Sluse et al 2007;Hutsemékers et al 2010). In this paper, we present a careful re-extraction and analysis of archive spectra of a sample of 13 lensed quasars initially observed with the aim of measuring the redshift of the lensing galaxy.…”

Section: Introductionmentioning

confidence: 99%

Microlensing of the broad line region in 17 lensed quasars

Sluse

Hutsemékers

Courbin

et al. 2012

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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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“…We then used additional observations of the standard star GD140 to calibrate the flux scale, and thus, derived wavelength-and flux-calibrated spectra. There are several approaches to extract individual spectra of quasar images and galaxies in lens systems on a long slit (e.g., Fassnacht & Cohen 1998;Ofek et al 2006;Sluse et al 2007). In particular, Sluse et al (2007) extracted spectra of three close quasar images along a slit by fitting three 1D PSF profiles in the spatial direction for each wavelength bin.…”

Section: Gtc Optical Spectroscopymentioning

confidence: 99%

“…There are several approaches to extract individual spectra of quasar images and galaxies in lens systems on a long slit (e.g., Fassnacht & Cohen 1998;Ofek et al 2006;Sluse et al 2007). In particular, Sluse et al (2007) extracted spectra of three close quasar images along a slit by fitting three 1D PSF profiles in the spatial direction for each wavelength bin. Our extraction method relies on the scheme of Sluse et al, but it incorporates some procedures to accurately account for off-axis quasar images and galaxies.…”

Section: Gtc Optical Spectroscopymentioning

confidence: 99%

Deep optical imaging and spectroscopy of the lens system SDSS J1339+1310

Shalyapin

Goicoechea

2014

A&A

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We present deep I-band imaging (NOT-ALFOSC) and spectroscopic (GTC-OSIRIS) observations of the gravitational lens system SDSS J1339+1310. This consists of two images of a lensed quasar, A and B, and a lensing galaxy G between the two quasar images. Our observations led to the following main results: (1) We obtained new accurate positions for B and G (relative to A), as well as structure parameters for the light distribution of G. The new position angle for G is separated by ∼50 • from the previously determined value. (2) The spectrum of G is typical for early-type galaxies, and we measured its redshift (0.609 ± 0.001) for the first time. (3) We determined the flux ratio B/A for the cores of the emission lines in the two quasar spectra. They were used to constrain the macrolens flux ratio M BA and dust extinction parameters. (4) The continuum flux ratio was appropriately corrected to obtain the microlensing magnification ratio of the continuum μ BA . This μ BA indicates that B is amplified (relative to A) by a factor of about 3−5, with larger amplifications at shorter wavelengths. The observed microlensing chromaticity coincides with a sharp drop in the r-band flux of B.(5) We reconstructed the lensing mass from the new observational constraints on the relative astrometry, M BA and the luminous structure of G. We also used the redshift of G to predict the time delay between quasar images (43 ± 5 d, A is leading).

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Multi-wavelength study of the gravitational lens system RXS J1131-1231

Cited by 105 publications

References 44 publications

Microlensing in H1413+117: disentangling line profile emission and absorption in a broad absorption line quasar

Microlensing in H1413+117: disentangling line profile emission and absorption in a broad absorption line quasar

Microlensing of the broad line region in 17 lensed quasars

Deep optical imaging and spectroscopy of the lens system SDSS J1339+1310

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