Initial light curve of Q2237 + 0305

Corrigan, R. T.; Irwin, M. J.; Arnaud, J.; Fahlman, Gregory G.; Fletcher, J. M.; Hewett, Paul C.; Hewitt, Jacqueline N.; Fèvre, O. Le; McClure, R. D.; Pritchet, C. J.; Schneider, Donald P.; Turner, Edwin L.; Webster, R. L.; Yee, H. K. C.

doi:10.1086/115856

Cited by 108 publications

(110 citation statements)

References 7 publications

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“…Since quasar microlensing was first described by Chang & Refsdal (1979) and detected by Corrigan et al (1991), studies have successfully isolated its signal by analyzing observations of lensed quasars over time (e.g., Morgan et al 2010;Mosquera et al 2013), wavelength (e.g., Bate et al 2008;Muñoz et al 2011), or both (e.g., Poindexter et al 2008;Eigenbrod et al 2008a,b). Microlensing by stars in the lens galaxy can (de)magnify individual images in a multiplyimaged system, causing the ratios between the image fluxes to be significantly different from the predictions of strong lens models fit to the observed macroscopic properties of the lens.…”

Section: Introductionmentioning

confidence: 99%

A Consistent Picture Emerges: A Compact X-Ray Continuum Emission Region in the Gravitationally Lensed Quasar SDSS J0924+0219

MacLeod

Morgan

Mosquera

et al. 2015

ApJ

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We analyze the optical, UV, and X-ray microlensing variability of the lensed quasar SDSS J0924+0219 using six epochs of Chandra data in two energy bands (spanning 0.4-8.0 keV, or 1-20 keV in the quasar rest frame), 10 epochs of F275W (rest-frame 1089Å) Hubble Space Telescope data, and high-cadence R-band (rest-frame 2770Å) monitoring spanning eleven years. Our joint analysis provides robust constraints on the extent of the X-ray continuum emission region and the projected area of the accretion disk. The best-fit half-light radius of the soft X-ray continuum emission region is between 5 × 10 13 and 10 15 cm, and we find an upper limit of 10 15 cm for the hard X-rays. The best-fit soft-band size is about 13 times smaller than the optical size, and roughly 7GM BH /c 2 for a 2.8 × 10 8 M ⊙ black hole, similar to the results for other systems. We find that the UV emitting region falls in between the optical and X-ray emitting regions at 10 14 cm < r 1/2,UV < 3 × 10 15 cm. Finally, the optical size is significantly larger, by 1.5σ, than the theoretical thin-disk estimate based on the observed, magnification-corrected I-band flux, suggesting a shallower temperature profile than expected for a standard disk.

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Section: Introductionmentioning

confidence: 99%

A Consistent Picture Emerges: A Compact X-Ray Continuum Emission Region in the Gravitationally Lensed Quasar SDSS J0924+0219

MacLeod

Morgan

Mosquera

et al. 2015

ApJ

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“…The first attempt to build the light curves of the four quasar components was made in 1991 by Corrigan et al (1991). They brought together all the available Q2237 images of sufficient quality, taken with different telescopes and in a variety of passbands, -Mould B, V and R and Gunn g, r and i, -and reprocessed with a single algorithm.…”

Section: Introductionmentioning

confidence: 99%

“…In addition to the data of 1986−89, contained in Corrigan et al (1991), other results were used, taken in 1990 and 1991 by Crane et al (1991), Racine (1992), Rix et al (1992), and Houde et al (1994).…”

Section: Introductionmentioning

confidence: 99%

Color effects associated with the 1999 microlensing brightness peaks in gravitationally lensed quasar Q2237+0305

Vakulik¹,

Schild

Dudinov³

et al. 2004

A&A

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Abstract. We present photometry of the Q2237+0305 gravitational lens system in VRI spectral bands with the 1.5-m telescope of the high-altitude Maidanak observatory in 1995−2000. The time interval includes the epoch of the dramatic brightness peaks discovered previously in the A and C image components (Wozniak et al. 2000a,b). By good luck three nights of observation in 1999 were almost at the time of the strong brightness peak of image C, and approximately in the middle of the ascending slope of the brightness peak of image A. Having reached its brightness maximum at the very end of June 1999, the C component had changed its (V − I) color from 0.3 m to 0.12 m since August 1998, and from 0.56 m to 0.12 m since August 1997. It was the bluest component in the system in 1998 and 1999, but by October 2000 that was no longer the case. We do not know the color of the A component exactly at its brightness peak, but we do know that it became 0.47 m brighter in R and 0.15 m bluer in (V − R) between August 1998 and August 2000, about three months before the peak. More intensive monitoring of Q2237+0305 in July-October 2000, made on a nearly daily basis, did not reveal rapid (night-to-night and intranight) brightness variations of the components during this time period, exceeding the photometry error bars. Rather slow changes of magnitudes of the components were observed, in particular, nearly synchronous 0.08 m fading of B and C components, and 0.05 m brightening of D in the R band during July 23−October 7, 2000, while the B component had become the faintest in all filters by the end of this time period. The behavior of the colors of the components was analyzed on the basis of all our VRI observations, made in 1995−2000 on Maidanak. A qualitative tendency of the components to become bluer as their brightness increases, noted in our previous works, was confirmed quantitatively. A correlation between the color variations and variations of magnitudes of the components is demonstrated to be significant and reaches 0.75 for ∆(V − I) vs. ∆R, with a regression line slope of 0.33± 0.08 for these quantities. A plot of (V − I) vs. (V − R) shows the components settled in a cluster, stretchng along a line with a slope of 1.31 ± 0.14. Both slopes are noticeably less steep than those expected if a standard galactic interstellar reddening law were responsible for the differences between the colors of images and their variations over time. We attribute the brightness and color changes to microlensing of the quasar's structure, which we conclude to be more compact at shorter wavelengths, as predicted by most quasar models featuring an energizing central source.

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“…If one or both of the stars were variable, our photometry would still be accurate to less than 0.02 mag in 65% of the cases, and 0.04 mag in 95% of the cases. We use the r−magnitude determined by Corrigan et al (1991, their The frames are then aligned using the IRAF task "imalign". In this process, all frames are bilinearly interpolated to the positions of one reference frame; 3.…”

Section: Data Reductionmentioning

confidence: 99%

“…Corrigan et al (1991) published the "initial light curve", that was later augmented by other individual and systematical observations (Pen et al 1993;Houde & Racine 1994). In Wambsganss (1992) it was emphasized that without frequent sampling, it would be difficult to extract useful information from the microlensing observations.…”

Section: Introductionmentioning

confidence: 99%

Optical monitoring of the gravitationally lensed quasar Q2237+0305 from APO between June 1995 and January 1998

Schmidt

Kundić²,

Pen

et al. 2002

A&A

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Initial light curve of Q2237 + 0305

Cited by 108 publications

References 7 publications

A Consistent Picture Emerges: A Compact X-Ray Continuum Emission Region in the Gravitationally Lensed Quasar SDSS J0924+0219

A Consistent Picture Emerges: A Compact X-Ray Continuum Emission Region in the Gravitationally Lensed Quasar SDSS J0924+0219

Color effects associated with the 1999 microlensing brightness peaks in gravitationally lensed quasar Q2237+0305

Optical monitoring of the gravitationally lensed quasar Q2237+0305 from APO between June 1995 and January 1998

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