The multiple quasar Q2237+0305 under a microlensing caustic

Anguita, T.; Schmidt, R. W.; Turner, Edwin L.; Wambsganß, J.; Webster, R. L.; Loomis, Karen; Long, Daniel C.; McMillan, R.

doi:10.1051/0004-6361:20078221

Cited by 92 publications

(135 citation statements)

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“…These values agree with the radii obtained for the lensed quasars HE1104−1805 and Q2237+0305 on the basis of their photometric variability due to microlensing (e.g. Poindexter et al 2008;Eigenbrod et al 2008;Anguita et al 2008b).…”

Section: Microlensing Of the Continuum Sourcesupporting

confidence: 88%

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: Microlensing Of the Continuum Sourcesupporting

confidence: 88%

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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“…However, studies of high-magnification events are likely biased toward small quasar size estimates because it is easier to obtain high magnifications with small sources (e.g., Kochanek 2004;Eigenbrod et al 2008;Blackburne et al 2011). It is also interesting to note that without considering any velocity prior (i.e., adopting a uniform prior), the size determinations of Eigenbrod et al (2008) and Anguita et al (2008) increase by a factor ∼4 (see Sluse et al 2011) but would then require cosmologically unrealistic peculiar velocities for the lens/source.…”

Section: The Observed Magnitude Of Image I=(a B C D) Ismentioning

confidence: 99%

Structure of the Accretion Disk in the Lensed Quasar Q2237+0305 From Multi-Epoch and Multi-Wavelength Narrowband Photometry

Muñoz

Vives-Arias

Mosquera

et al. 2016

ApJ

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We present estimates for the size and the logarithmic slope of the disk temperature profile of the lensed quasar Q2237+0305, independent of the component velocities. These estimates are based on six epochs of multiwavelength narrowband images from the Nordic Optical Telescope. For each pair of lensed images and each photometric band, we determine the microlensing amplitude and chromaticity using pre-existing mid-IR photometry to define the baseline for no microlensing magnification. A statistical comparison of the combined microlensing data (6 epochs×5 narrow bands×6 image pairs) with simulations based on microlensing magnification maps gives Bayesian estimates for the half-light radius oflt-day, and p=0.95±0.33 for the exponent of the logarithmic temperature profile µ -T R p 1 . This size estimate is in good agreement with most recent studies. Other works based on the study of single microlensing events predict smaller sizes, but could be statistically biased by focusing on high-magnification events.

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“…After the first detection of microlensing in the continuum and in the broad line (Irwin et al 1989;Filippenko 1989), microlensing has started to be used as a tool to constrain the size of the accretion disc and of the broad line emitting region Wyithe et al 2000b;Yonehara 2001;Wyithe et al 2000a). In the last decade, important progress in observational techniques allowed photometric and spectrophotometric monitoring of the individual lensed images to be successfully carried out (Woźniak et al 2000;Dai et al 2003;Anguita et al 2008b;Eigenbrod et al 2008;Zimmer et al 2011). On the other hand, the development of more advanced numerical techniques allowed quicker calculation of magnification maps and more sophisticated analysis (Kochanek 2004;Poindexter & Kochanek 2010a,b;Bate et al 2010;Mediavilla et al 2011;Garsden et al 2011;Bate & Fluke 2012).…”

Section: Introductionmentioning

confidence: 99%

Microlensing of the broad line region in 17 lensed quasars

Sluse

Hutsemékers

Courbin

et al. 2012

A&A

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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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The multiple quasar Q2237+0305 under a microlensing caustic

Cited by 92 publications

References 50 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

Structure of the Accretion Disk in the Lensed Quasar Q2237+0305 From Multi-Epoch and Multi-Wavelength Narrowband Photometry

Microlensing of the broad line region in 17 lensed quasars

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