Analysis of the Q2237+0305 light-curve variability with regularization technique

Koptelova, E.; Shimanovskaya, E. V.; Артамонов, Б. П.; Yagola, A. G.

doi:10.1111/j.1365-2966.2007.12335.x

Cited by 9 publications

(12 citation statements)

References 35 publications

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“…We find that the amplitude of the brightness peak is more pronounced in the g -band than in the r -band. This is also consistent with the observations by Vakulik et al (2004) (see also the recent analysis by Koptelova et al 2007).…”

Section: Discussionsupporting

confidence: 93%

The multiple quasar Q2237+0305 under a microlensing caustic

Anguita

Schmidt

Turner

et al. 2008

A&A

115

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We use the high magnification event seen in the 1999 OGLE campaign light curve of image C of the quadruply imaged gravitational lens Q2237+0305 to study the structure of the quasar engine. We have obtained g -and r -band photometry at the Apache Point Observatory 3.5 m telescope where we find that the event has a smaller amplitude in the r -band than in the gand OGLE V-bands. By comparing the light curves with microlensing simulations we obtain constraints on the sizes of the quasar regions contributing to the g -and r -band flux. Assuming that most of the surface mass density in the central kiloparsec of the lensing galaxy is due to stars and by modeling the source with a Gaussian profile, we obtain for the Gaussian width −0.25 (all values at 68 percent confidence). Additionally, from our microlensing simulations we find that, during the chromatic microlensing event observed, the continuum emitting region of the quasar crossed a caustic at ≥72 percent confidence.

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Section: Discussionsupporting

confidence: 93%

The multiple quasar Q2237+0305 under a microlensing caustic

Anguita

Schmidt

Turner

et al. 2008

A&A

115

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“…This accurate microlensing curve (from October 1999 to early February 2000) has been discussed by several other groups (e.g. Kochanek 2004;Bogdanov & Cherepashchuk 2004;Vakulik et al 2004;Moreau et al 2005;Udalski et al 2006;Koptelova et al 2007;Alexan-drov & Zhdanov 2011;Abolmasov & Shakura 2012;Mediavilla et al 2015).…”

Section: Quasar Accretion Flowssupporting

confidence: 65%

New database for a sample of optically bright lensed quasars in the northern hemisphere

Gil-Merino

Goicoechea

Shalyapin

et al. 2018

A&A

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In the framework of the Gravitational LENses and DArk MAtter (GLENDAMA) project, we present a database of nine gravitationally lensed quasars (GLQs) that have two or four images brighter than r = 20 mag and are located in the northern hemisphere. This new database consists of a rich variety of follow-up observations included in the GLENDAMA global archive, which is publicly available online and contains 6557 processed astronomical frames of the nine lens systems over the period 1999−2016. In addition to the GLQs, our archive also incorporates binary quasars, accretion-dominated radio-loud quasars, and other objects, where about 50% of the non-GLQs were observed as part of a campaign to identify GLQ candidates. Most observations of GLQs correspond to an ongoing long-term macro-programme with 2−10 m telescopes at the Roque de los Muchachos Observatory, and these data provide information on the distribution of dark matter at all scales. We outline some previous results from the database, and we additionally obtain new results for several GLQs that update the potential of the tool for astrophysical studies.

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“…Even more dramatic brightness changes of the lensed components due to micro-lensing have been reported for Q2237+0305 (Udalski et al 2006;Koptelova et al 2007). These findings support the view of Witt et al (1995) about the general nature of quadrupole systems and the inevitability of micro-lensing events in them.…”

Section: Micro-lensing Eventsmentioning

confidence: 99%

Adaptive PSF fitting – a highly performing photometric method and light curves of the GLS H1413+117: time delays and micro-lensing effects

Akhunov

Wertz

Elyiv

et al. 2016

Mon. Not. R. Astron. Soc.

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We present new photometric observations of H1413+117 acquired during seasons between 2001 and 2008 in order to estimate the time delays between the lensed quasar images and to characterize at best the on-going micro-lensing events. We propose a highly performing photometric method called the adaptive point spread function fitting and have successfully tested this method on a large number of simulated frames. This has enabled us to estimate the photometric error bars affecting our observational results. We analysed the V-and R-band light curves and V-R colour variations of the A-D components which show short-and long-term brightness variations correlated with colour variations. Using the χ 2 and dispersion methods, we estimated the time delays on the basis of the R-band light curves over the seasons between 2003 and 2006. We have derived the new values: t AB = −17.4 ± 2.1, t AC = −18.9 ± 2.8 and t AD = 28.8 ± 0.7 d using the χ 2 method (B and C are leading, D is trailing) with 1σ confidence intervals. We also used available observational constraints (resp. the lensed image positions, the flux ratios in mid-IR and two sets of time delays derived in the present work) to update the lens redshift estimation. We obtained z l = 1.95 +0.06 −0.10 which is in good agreement with previous estimations. We propose to characterize two kinds of micro-lensing events: micro-lensing for the A,

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Analysis of the Q2237+0305 light-curve variability with regularization technique

Cited by 9 publications

References 35 publications

The multiple quasar Q2237+0305 under a microlensing caustic

The multiple quasar Q2237+0305 under a microlensing caustic

New database for a sample of optically bright lensed quasars in the northern hemisphere

Adaptive PSF fitting – a highly performing photometric method and light curves of the GLS H1413+117: time delays and micro-lensing effects

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