Microlensing variability in the gravitationally lensed quasar QSO 2237+0305 $\mathsf{\equiv}$ the Einstein Cross

Eigenbrod, A.; Courbin, F.; Meylan, G.; Agol, Eric; Anguita, T.; Schmidt, R. W.; Wambsganß, J.

doi:10.1051/0004-6361:200810729

Cited by 115 publications

(155 citation statements)

References 50 publications

(77 reference 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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“…The maximum likelihood estimate corresponds to = áñ lt-day. 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%

“…The blue filled square is our Bayesian estimate for the expected value of R 1/2 and p for the hybrid model (the values for the Gaussian and thin disk models are also plotted as green and red filled squares respectively for comparison). The open (filled) circle corresponds to the measurement by Eigenbrod et al (2008) with (without) a velocity prior. Straight lines correspond to the measurements by Poindexter & Kochanek (2010b) …”

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

confidence: 99%

“…The study of the disk temperature profile is more complicated because multi-wavelength observations are needed to detect chromatic microlensing (Anguita et al 2008;Bate et al 2008;Eigenbrod et al 2008;Poindexter et al 2008;Floyd et al 2009;Blackburne et al 2011Blackburne et al , 2015Mediavilla et al 2011b;Muñoz et al 2011;Motta et al 2012;Rojas et al 2014). In this case, it also becomes more important to separate the contributions from strong emission lines.…”

Section: Introductionmentioning

confidence: 99%

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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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“…The microlensing effect on the multiple quasar images, induced by stars in the deflector, provides a quantitative handle on the stellar content of the lens galaxies (e.g., Schechter & Wambsganss 2002;Oguri, Rusu & Falco 2014;Schechter et al 2014;Jiménez-Vicente et al 2015), and can simultaneously provide constraints on the inner structure of the lensed quasar, both the accretion disk size and the thermal profile (e.g. Poindexter, Morgan & Kochanek 2008;Anguita et al 2008;Eigenbrod et al 2008;Motta et al 2012) as well as the geometry of the broad line region (e.g. Sluse et al 2011, Guerras et al 2013, Braibant et al 2014.…”

Section: Introductionmentioning

confidence: 99%

Discovery of two gravitationally lensed quasars in the Dark Energy Survey

Agnello¹,

Treu²,

Ostrovski

et al. 2015

Mon. Not. R. Astron. Soc.

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We present spectroscopic confirmation of two new lensed quasars via data obtained at the 6.5m Magellan/Baade Telescope. The lens candidates have been selected from the Dark Energy Survey (DES) and WISE based on their multi-band photometry and extended morphology in DES images. Images of DES J0115−5244 show two blue point sources at either side of a red galaxy. Our long-slit data confirm that both point sources are images of the same quasar at z s = 1.64. The Einstein Radius estimated from the DES images is 0.51 . DES J2146−0047 is in the area of overlap between DES and the Sloan Digital Sky Survey (SDSS). Two blue components are visible in the DES and SDSS images. The SDSS fiber spectrum shows a quasar component at z s = 2.38 and absorption compatible with Mg II and Fe II at z l = 0.799, which we tentatively associate with the foreground lens galaxy. The long-slit Magellan spectra show that the blue components are resolved images of the same quasar. The Einstein Radius is 0.68 corresponding to an enclosed mass of 1.6 × 10 11 M . Three other candidates were observed and rejected, two being low-redshift pairs of starburst galaxies, and one being a quasar behind a blue star. These first confirmation results provide an important empirical validation of the data-mining and model-based selection that is being applied to the entire DES dataset.

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Microlensing variability in the gravitationally lensed quasar QSO 2237+0305 $\mathsf{\equiv}$ the Einstein Cross

Cited by 115 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

Discovery of two gravitationally lensed quasars in the Dark Energy Survey

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