COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses

Eigenbrod, A.; Courbin, F.; Dye, S.; Meylan, G.; Sluse, Dominique; Vuissoz, C.; Magain, Pierre

doi:10.1051/0004-6361:20054423

Cited by 62 publications

(76 citation statements)

References 30 publications

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“…Notes: the flux ratio A/B = 0.44±0.04 in H-band (Eigenbrod et al 2006a) is in good agreement with our estimate of M. Although K-band observation of this system exist (Faure et al 2011), they were not able to derive accurate photometry of the lensed images due to the ring. No other NIR/MIR photometric data of this system are available in the literature.…”

Section: Appendix A: Effect Of Intrinsic Variability On the MMDsupporting

confidence: 75%

“…Note that the differences arise because the scientific goal of the original papers was the determination of the redshift of the lensing galaxy, while we are interested here in a detailed study of the unpublished quasar spectra. Like Eigenbrod et al (2006aEigenbrod et al ( , 2007, we use MCS deconvolution algorithm adapted to spectra (Courbin et al 2000) in order to deblend the components of the lens system. This algorithm deconvolves the observed frame into a frame of finite resolution with a Gaussian PSF chosen to have FWHM = 2 pixels.…”

Section: Reduction and Deconvolutionmentioning

confidence: 99%

“…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%

“…(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%

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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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Section: Appendix A: Effect Of Intrinsic Variability On the MMDsupporting

confidence: 75%

Section: Reduction and Deconvolutionmentioning

confidence: 99%

Section: The Extended Samplementioning

confidence: 99%

Section: Accuracy Of the Intrinsic Flux Ratiosmentioning

confidence: 99%

See 2 more Smart Citations

Microlensing of the broad line region in 17 lensed quasars

Sluse

Hutsemékers

Courbin

et al. 2012

A&A

Self Cite

133

184

View full text Add to dashboard Cite

show abstract

“…The algorithm has been implemented in various analysis of quasars (Burud et al 2000(Burud et al , 2002aHjorth et al 2002;Jakobsson et al 2005;Vuissoz et al 2007;Eigenbrod et al 2006a).…”

Section: Photometrymentioning

confidence: 99%

Results of optical monitoring of 5 SDSS double QSOs with the Nordic Optical Telescope

Paraficz¹,

Hjorth²,

Elíasdóttir

2009

A&A

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We present optical R-band light curves of five SDSS double QSOs (SDSS J0903+5028, SDSS J1001+5027, SDSS J1206+4332, SDSS J1353+1138, SDSS J1335+0118) obtained from monitoring at the Nordic Optical Telescope (NOT) between September 2005 and September 2007. We also present analytical and pixelated modeling of the observed systems. For SDSS J1206+4332, we measured the time delay to be Δτ = 116 +4 −5 days, which, for a singular isothermal ellipsoid model, corresponds to a Hubble constant of 73 +3 −4 km s −1 Mpc −1 . Simultaneous pixelated modeling of five other systems for which a time delay has now been previously measured at the NOT leads to H 0 = 61.5 +8 −4 km s −1 Mpc −1 . Finally, by comparing light curves of the two images of each system, suitably shifted by the predicted or observed time-delays, we found no evidence of microlensing variability over the course of the monitoring period.

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