PG 1115+080: variations of the A2/A1 flux ratio and new values of the time delays

Tsvetkova, V. S.; Vakulik, V. G.; Shulga, V. M.; Schild, Rudolph E.; Dudinov, V. N.; Минаков, А. А.; Nuritdinov, S. N.; Артамонов, Б. П.; Kochetov, A. Y.; Smirnov, Georgi; Sergeyev, A.; Konichek, V. V.; Sinelnikov, I. Ye.; Zheleznyak, A. P.; Bruevich, V. V.; Gaisin, R.; Akhunov, T.; Бурхонов, О.

doi:10.1111/j.1365-2966.2010.16882.x

Cited by 12 publications

(13 citation statements)

References 66 publications

(170 reference statements)

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“…The micro-lensing rate measured for the A, B, C components, on average, corresponds to the characteristic rate of micro-lensing 10 −4 mag d −1 reported for other known gravitationally lensed quasars (Gaynullina et al 2005;Vakulik et al 2006;Goicoechea & Shalyapin 2010;Tsvetkova et al 2010;Ricci et al 2011). …”

Section: Micro-lensing Eventssupporting

confidence: 75%

“…The long-term light curves indicate the presence of micro-lensing effects, sometimes displaying a large amplitude with respect to by micro-lensing with induced variability at the level of 10 −4 mag d −1 (Gaynullina et al 2005;Vakulik et al 2006;Goicoechea & Shalyapin 2010;Tsvetkova et al 2010). But here we found out one of the fastest micro-lensing effects with a rate of 10 −3 mag d The flux slope of the B component in 2003 is smaller than those of the other components.…”

Section: I C Ro -L E N S I N G a N D C O L O U R Va R I At I O N Smentioning

confidence: 44%

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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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Section: Micro-lensing Eventssupporting

confidence: 75%

Section: I C Ro -L E N S I N G a N D C O L O U R Va R I At I O N Smentioning

confidence: 44%

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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“…Schechter et al 1997). In this work, we use recent estimates of the time delays by Tsvetkova et al (2010) that differ from previously found values by e.g. Barkana (1997).…”

Section: The Individual Lensesmentioning

confidence: 99%

Light versus dark in strong-lens galaxies: dark matter haloes that are rounder than their stars

Bruderer

Read

Coles

et al. 2015

Mon. Not. R. Astron. Soc.

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We measure the projected density profile, shape and alignment of the stellar and dark matter mass distribution in 11 strong-lens galaxies. We find that the projected dark matter density profile -under the assumption of a Chabrier stellar initial mass function -shows significant variation from galaxy to galaxy. Those with an outermost image beyond ∼ 10 kpc are very well fit by a projected NFW profile; those with images within 10 kpc appear to be more concentrated than NFW, as expected if their dark haloes contract due to baryonic cooling. We find that over several half-light radii, the dark matter haloes of these lenses are rounder than their stellar mass distributions. While the haloes are never more elliptical than e dm = 0.2, their stars can extend to e * > 0.2. Galaxies with high dark matter ellipticity and weak external shear show strong alignment between light and dark; those with strong shear (γ 0.1) can be highly misaligned. This is reassuring since isolated misaligned galaxies are expected to be unstable. Our results provide a new constraint on galaxy formation models. For a given cosmology, these must explain the origin of both very round dark matter haloes and misaligned strong-lens systems.

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“…However, as stated above, A1 produces 56% of the total emission detected at Earth at Å 7500 (Tsvetkova et al 2010). We assume, in the absence of any other information, that »56% of the Mg II and C IV line strength is also from A1.…”

Section: Hst Observationsmentioning

confidence: 92%

The Extreme Ultraviolet Variability of Quasars

Punsly

Marziani

Zhang

et al. 2016

ApJ

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We study the extreme ultraviolet (EUV) variability (rest frame wavelengths 500-920 Å) of high-luminosity quasars using Hubble Space Telescope (HST) (low to intermediate redshift sample) and Sloan Digital sky Survey (SDSS) (high redshift sample) archives. The combined HST and SDSS data indicates a much more pronounced variability when the sampling time between observations in the quasar rest frame is >2 10 s 7 compared to <1.5 10 7 s. Based on an excess variance analysis, for time intervals <2 10 s 7 in the quasar rest frame, 10% of the quasars (4/40) show evidence of EUV variability. Similarly, for time intervals >2 10 s 7 in the quasar rest frame, 55% of the quasars (21/38) show evidence of EUV variability. The propensity for variability does not show any statistically significant change between2.5 10 s 7 and3.16 10 s 7 (1 year). The temporal behavior is one of a threshold time interval for significant variability as opposed to a gradual increase on these timescales. A threshold timescale can indicate a characteristic spatial dimension of the EUV region. We explore this concept in the context of the slim disk models of accretion. We find that for rapidly spinning black holes, the radial infall time to the plunge region of the optically thin surface layer of the slim disk that is responsible for the preponderance of the EUV flux emission (primarily within 0-7 black hole radii from the inner edge of the disk) is consistent with the empirically determined variability timescale.

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PG 1115+080: variations of the A2/A1 flux ratio and new values of the time delays

Cited by 12 publications

References 66 publications

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

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

Light versus dark in strong-lens galaxies: dark matter haloes that are rounder than their stars

The Extreme Ultraviolet Variability of Quasars

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