A catalog of secondary photometric standard stars around gravitational lenses

Nakos, Theodoros; Ofek, E. O.; Boumis, P.; Cuypers, J.; Sinachopoulos, D.; Dessel, E. van; Gal‐Yam, A.; Papamastorakis, I.

doi:10.1051/0004-6361:20030310

Cited by 9 publications

(22 citation statements)

References 5 publications

(5 reference statements)

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“…Figure 2 shows the differential R magnitude for comparison stars. The final results are in good concordance with the values obtained by Nakos et al (2003), who gave R3 − R1 = 1.20 ± 0.02 and R2 − R1 = 0.73 ± 0.02.…”

Section: Observations and Data Reductionsupporting

confidence: 91%

“…Five stars in the vicinity of Q0142-100-defined as 1, 2, 3, 4, and 5 in Nakos et al (2003)-are used. These stars were examined differentially in sets of four versus one star.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…Finally, the apparent magnitudes of the A and B components were derived by comparing the instrumental fluxes with the star labeled as 1 (see Nakos et al 2003) The mean difference in magnitude among both components, ΔM = M B −M A , is 2.00 for the two datasets. For the 1999-2005 data, the photometric errors (derived using the 1 and 3 field stars) of the A component data are of the order of 0.02 mag, while those of the B component are around 0.2 mag (see Figure 6).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

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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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Section: Observations and Data Reductionsupporting

confidence: 91%

“…Five stars in the vicinity of Q0142-100-defined as 1, 2, 3, 4, and 5 in Nakos et al (2003)-are used. These stars were examined differentially in sets of four versus one star.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Section: Observations and Data Reductionmentioning

confidence: 99%

See 1 more Smart Citation

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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“…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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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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“…All three methods were developed at the Two reference stars are indicated (S1 and S2). Star S1, whose absolute photometry is well known (Nakos et al 2003) has been used to normalize the CCD frames. Star S2 was taken as a comparison star.…”

Section: Data Reduction Techniquesmentioning

confidence: 99%

Photometric monitoring of the doubly imaged quasar UM 673: possible evidence for chromatic microlensing

Nakos¹,

Courbin

Poels

et al. 2005

A&A

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Abstract. We present the results of two-band CCD photometric monitoring of the gravitationally lensed quasar Q 0142−100 (UM 673). The data, obtained at ESO-La Silla with the 1.54 m Danish telescope in the Gunn i-band (October 1998−September 1999) and in the Johnson V-band (October 1998 to December 2001), were analyzed using three different photometric methods. The light-curves obtained with all methods show variations, with a peak-to-peak amplitude of 0.14 mag in V. Although it was not possible to measure the time delay between the two lensed QSO images, the brighter component displays possible evidence for microlensing: it becomes bluer as it gets brighter, as expected under the assumption of differential magnification of a quasar accretion disk.

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A catalog of secondary photometric standard stars around gravitational lenses

Cited by 9 publications

References 5 publications

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

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

Flux and color variations of the doubly imaged quasar UM673

Photometric monitoring of the doubly imaged quasar UM 673: possible evidence for chromatic microlensing

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