Liverpool-Maidanak monitoring of the Einstein Cross over 2006-2019. I. Light curves in the gVrRI optical bands and microlensing signatures

Goicoechea, L.J.; Artamonov, B.P.; Shalyapain, V.N.; Sergeyev, A.V.; Burkhonov, O.A.; Akhunov, T.A.; Asfandiyarov, I.M.; Bruevich, V.V.; Ehgamberdiev, S.A.; Shimanovskaya, E.V.; Zheleznyak, A.P.

Статья опубликована в высокорейтинговом журнале

Информация о цитировании статьи получена из Web of Science, Scopus
Статья опубликована в журнале из списка Web of Science и/или Scopus
Дата последнего поиска статьи во внешних источниках: 24 сентября 2020 г.

Авторы: Goicoechea L.J., Artamonov B.P., Shalyapain V.N., Sergeyev A.V., Burkhonov O.A., Akhunov T.A., Asfandiyarov I.M., Bruevich V.V., Ehgamberdiev S.A., Shimanovskaya E.V., Zheleznyak A.P.
Журнал: Astronomy and Astrophysics
Том: 637
Год издания: 2020
Издательство: Springer Verlag
Местоположение издательства: Germany
Номер статьи: A89
DOI: 10.1051/0004-6361/202037902
Аннотация: Quasar microlensing offers a unique opportunity to resolve tiny sources in distant active galactic nuclei and study compact object populations in lensing galaxies. We therefore searched for microlensing-induced variability of the gravitationally lensed quasar QSO 2237+0305 (Einstein Cross) using 4 374 optical frames taken with the 2.0 m Liverpool Telescope and the 1.5 m Maidanak Telescope.These gVrRI frames over the 2006−2019 period were homogeneously processed to generate accurate long-term multi-band lightcurves of the four quasar images A-D. Through difference light curves, we found strong microlensing signatures. We then focused on the analytical modelling of two putative caustic-crossing events in image C, finding compelling evidence that this image experienced a double caustic crossing. Additionally, our overall results indicate that a standard accretion disc accounts reasonably well for the brightness profile of UV continuum emission sources and for the growth in source radius when the emission wavelength increases: R_λ ∝ λ^α, α = 1.33 ± 0.09. However, we caution that numerical microlensing simulations are required before firm conclusions can be reached on the UV emission scenario because the VRI-band monitoring during the first caustic crossing and one of our two αindicators lead to a few good solutions with α ≈ 1.
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Liverpool-Maidanak monitoring of the Einstein Cross over 2006-2019. I. Light curves in the gVrRI optical bands and microlensing signaturesстатья

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