Photometric Variability of the Gravitational Lens 0142−100 (UM 673)

Sinachopoulos, D.; Nakos, Theodoros; Boumis, P.; Dessel, E. van; Burger, M.; Rodríguez‐Gil, P.

doi:10.1086/323306

Cited by 5 publications

(5 citation statements)

References 12 publications

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“…The colors of the lens galaxy were found to match those of a passively evolving earlytype galaxy at z ≈ 0.5 (Muñoz et al 1998). Lehár et al (2000Lehár et al ( , 2002 reported Hubble Space Telescope (HST) observations of UM673 at optical and infrared wavelengths, and Sinachopoulos et al (2001) observed the lensed quasar in the R filter for six seasons (1995)(1996)(1997)(1998)(1999)(2000), detecting a significant increase by 0.3 mag of the combined system (lensed components) with respect to the values reported at discovery, with a peak of 0.5 mag during the period 1995-1997. Lehár et al (2000) performed photometric measurements on HST data taken in the R filter, and obtained magnitudes of 16.67, 18.96, and 19.35 for the "A", "B" components and the lens galaxy, respectively.…”

Section: Introductionmentioning

confidence: 71%

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Flux and color variations of the doubly imaged quasar UM673

Ricci

Elyiv

Finet

et al. 2013

A&A

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Aims. With the aim of characterizing the flux and color variations of the multiple components of the gravitationally lensed quasar UM673 as a function of time, we have performed multiepoch and multiband photometric observations with the Danish 1.54 m telescope at the La Silla Observatory. Methods. The observations were carried out in the VRi spectral bands during four seasons (2008)(2009)(2010)(2011). We reduced the data using the point spread function photometric technique as well as aperture photometry. Results. Our results show for the brightest lensed component some significant decrease in flux between the first two seasons (+0.09/+0.11/+0.05 mag) and a subsequent increase during the following ones (−0.11/−0.11/−0.10 mag) in the V/R/i spectral bands, respectively. Comparing our results with previous studies, we find smaller color variations between these seasons as compared with previous ones. We also separate the contribution of the lensing galaxy from that of the fainter and close lensed component.

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Section: Introductionmentioning

confidence: 71%

“…However, star "V" is closer to the lens system, and it is therefore better to use its shape as a reference PSF for the lens fitting. Also, it had been found to be photometrically stable by Sinachopoulos et al (2001) and Nakos et al (2003); finally it was already used by Nakos et al (2005) as a reference for the PSF fitting of UM673.…”

Section: Starmentioning

confidence: 99%

Flux and color variations of the doubly imaged quasar UM673

Ricci

Elyiv

Finet

et al. 2013

A&A

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“…Daulie et al (1993) observed it in the B band from 1987 to 1993 but their observations were of modest quality, concluding that no significant variability was seen at the quasar. Some years later, Sinachopoulos et al (2001) presented 29 R band observations taken from 1995 to 2000, detecting variations of 0.2 mag in their data and a global variation of ∼ 0.5 mag since the system was discovered. Nakos et al (2005) performed two-band, V (23 points) and i (18 points), photometry during three years, October 1998 to December 2001.…”

Section: Introductionmentioning

confidence: 99%

Long-Term Monitoring, Time Delay, and Microlensing in the Gravitational Lens System Q0142-100

Oscoz

Serra-Ricart

Mediavilla

et al. 2013

ApJ

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We present 12 yr of monitoring of the gravitational lens Q0142-100 from the Teide Observatory. The data, taken from 1999 to 2010, comprise 105 observing nights with the IAC80 Telescope. The application of the δ 2 method to the dataset leads to a value for the time delay between both components of the system of 72 ± 22 days (68% confidence level), consistent within uncertainties with the most recent results. With this value in mind a possible microlensing event is detected in Q0142-100.

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“…′′ 2. UM673 has been extensively observed since its discovery (Daulie et al 1993;Sinachopoulos et al 2001). However, earlier studies measured only relative or integral photometry of the two of UM673 images, so the detected brightness variations could be explained by both intrinsic quasar variability and microlensing.…”

Section: Introductionmentioning

confidence: 99%

Time delay between images of the lensed quasar UM673

Koptelova¹,

Chen²,

Chiueh³

et al. 2012

A&A

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Aims. We study brightness variations in the double lensed quasar UM673 (Q0142-100) with the aim of measuring the time delay between its two images. Methods. We combined our previously published observational data of UM673 obtained during the 2003-2005 seasons at the Maidanak Observatory with archival and recently observed Maidanak and CTIO UM673 data. We analyzed the V, R and I-band light curves of the A and B images of UM673, which cover ten observational seasons from August 2001 to November 2010. We also analyzed the time evolution of the difference in magnitudes (flux ratio) between images A and B of UM673 over more than ten years. Results. We find that the quasar exhibits both short-term (with an amplitude of ∼0.1 mag in the R band) and long-term (with an amplitude of ∼0.3 mag) variability on timescales of about several months and several years, respectively. These brightness variations are used to constrain the time delay between the images of UM673. From a cross-correlation analysis of the A and B quasar light curves and an error analysis we measure a mean time delay of 89 days with an rms error of 11 days. Given the input time delay of 88 days, the most probable value of the delay that can be recovered from light curves with the same statistical properties as the observed R-band light curves of UM673, is 95 +5 −16 +14−29 days (68% and 95% confidence intervals). Analysis of the V − I color variations and the V, R and I-band magnitude differences of the quasar images does not show clear evidence for microlensing variations between 1998 and 2010.

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Photometric Variability of the Gravitational Lens 0142−100 (UM 673)

Cited by 5 publications

References 12 publications

Flux and color variations of the doubly imaged quasar UM673

Flux and color variations of the doubly imaged quasar UM673

Long-Term Monitoring, Time Delay, and Microlensing in the Gravitational Lens System Q0142-100

Time delay between images of the lensed quasar UM673

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