The Nature and Size of the Optical Continuum Source in QSO 2237+0305

Shalyapin, V. N.; Goicoechea, L. J.; Alcalde, D.; Mediavilla, E.; Muñoz, J. A.; Gil-Merino, R.

doi:10.1086/342753

Cited by 53 publications

(106 citation statements)

References 29 publications

(49 reference statements)

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“…2. It is clear that whereas components A and C show a small but significant variability (see Shalyapin et al 2002 andGoicoechea et al 2003, for the interpretation of the variation in the component A as the peak of a high-magnification event), images B and D remain relative flat, showing no signs of strong microlensing during the monitoring period. As the expected time delays between the images are short (≤1 day, see Schneider et al 1988;Wambsganss & Paczyński 1994), intrinsic fluctuations would show up in all 4 images almost simultaneously.…”

Section: Monitoring Observations Of Q2237+0305mentioning

confidence: 99%

Limits on the transverse velocity of the lensing galaxy in Q2237+0305 from the lack of strong microlensing variability

Gil-Merino

Wambsganß

Goicoechea

et al. 2005

A&A

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Abstract. We present a method for the determination of upper limits on the transverse velocity of the lensing galaxy in the quadruple quasar system Q2237+0305, based on the lack of strong microlensing signatures in the quasar lightcurves. The limits we derive here are based on four months of high quality monitoring data, by comparing the low amplitudes of the lightcurves of the four components with extensive numerical simulations. We make use of the absence of strong variability of the components (especially components B and D) to infer that a "flat" time interval of such a length is only compatible with an effective transverse velocity of the lensing galaxy of v bulk ≤ 630 km s −1 for typical microlenses masses of M µlens = 0.1 M (or v bulk ≤ 2160 km s −1 for M µlens = 1.0 M ) at the 90% confidence level. This method may be applicable in the future to other systems.

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Section: Monitoring Observations Of Q2237+0305mentioning

confidence: 99%

Limits on the transverse velocity of the lensing galaxy in Q2237+0305 from the lack of strong microlensing variability

Gil-Merino

Wambsganß

Goicoechea

et al. 2005

A&A

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“…8), leading to best-fit values of p in the range 2.3−2.4. It is very remarkable that p ∼ 2−3 is close to the power-law index for a standard accretion disk (p = 8/3; e.g., Shalyapin et al 2002). Very recently, Guerras et al (2013) have claimed that a significant part of the UV Fe ii and Fe iii emissions may originate in the accretion disk.…”

Section: Microlensing Factorymentioning

confidence: 78%

“…The intensity distribution I(λ, r), r = (x 2 + y 2 ) 1/2 , was then convolved with μ B (x, y) to obtain (e.g., Jaroszyński et al 1992;Shalyapin et al 2002) …”

Section: Microlensing Factorymentioning

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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“…This makes possible some estimations of certain GLS characteristics, in particular, the source size [25]. For example, in case of the well-known GLS Q2237+0305 (Einstein Cross), several HAEs was observed [26][27][28] and the estimates of the source size have been obtained within different source models [16,[29][30][31][32][33][34].…”

Section: Preliminary Commentsmentioning

confidence: 99%

Analytical Methods in Gravitational Microlensing

Жданов

Alexandrov

Fedorova

et al. 2012

ISRN Astronomy and Astrophysics

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We discuss analytical results dealing with photometric and astrometric gravitational microlensing. The first two sections concern approximation methods that allow us to get solutions of the general lens equation near fold caustics and cusp points up to any prescribed accuracy. Two methods of finding approximate solutions near the fold are worked out. The results are applied to derive new corrections to total amplifications of critical source images. Analytic expressions are obtained in case of the Gaussian, power-law, and limb-darkening extended source models; here we present the first nonzero corrections to the well-known linear caustic approximation. Possibilities to distinguish different source models in observations are discussed on the basis of statistical simulations of microlensed light curves. In the next section, we discuss astrometric microlensing effects in various cases of extended sources and extended lenses, including a simple model of weak statistical microlensing by extended dark matter clumps. Random walks of a distant source image microlensed by stochastic masses are estimated. We note that the bulk motion of foreground stars induces a small apparent rotation of the extragalactic reference frame. Compact analytical relations describing the statistics of such motions are presented.

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The Nature and Size of the Optical Continuum Source in QSO 2237+0305

Cited by 53 publications

References 29 publications

Limits on the transverse velocity of the lensing galaxy in Q2237+0305 from the lack of strong microlensing variability

Limits on the transverse velocity of the lensing galaxy in Q2237+0305 from the lack of strong microlensing variability

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

Analytical Methods in Gravitational Microlensing

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