Flux and color variations of the doubly imaged quasar UM673

Ricci, Davide; Elyiv, A.; Finet, F.; Wertz, O.; Alsubai, K. A.; Anguita, T.; Bozza, V.; Browne, P.; Burgdorf, M.; Novati, S. Calchi; Dodds, P.; Dominik, M.; Gerner, T.; Glitrup, M.; Grundahl, F.; Hardis, S.; Harpsøe, K.; Hinse, T. C.; Hornstrup, A.; Hundertmark, M.; Jørgensen, U. G.; Kains, N.; Kerins, E.; Liebig, C.; Maier, G.; Mancini, L.; Mathiasen, M.; Penny, Matthew T.; Proft, S.; Rahvar, S.; Scarpetta, G.; Sahu, K. C.; Schäfer, Sebastian; Schönebeck, F.; Schmidt, R. W.; Skottfelt, J.; Snodgrass, C.; Southworth, J.; Thöne, C. C.; Wambsganß, J.; Zimmer, F.; Zub, M.; Surdej, Jean

doi:10.1051/0004-6361/201118755

Cited by 6 publications

(7 citation statements)

References 20 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Such a behaviour has already been observed for the double quasar SBS 1520+530 by Gaynullina et al (2005). 2004), Pereyra et al (2006), Ricci et al (2011), andRicci et al (2013). The yearly averages of the colour are shown in Table 6.…”

Section: Time Delay For He 0047-1756supporting

confidence: 69%

“…light curve as a function of the MJD, shown in the upper part of Fig. 15, reveals that the two components span the highest colour variation of ≈ 0.07 mag between seasons 2008 and 2009, with both images turning bluer in correspondence to the 2009 brightening, as already observed by Vanden Berk et al (2004), Pereyra et al (2006), Ricci et al (2011), and Ricci et al (2013). The yearly averages of the colour are shown in Table 6.…”

Section: The Light Curve Of the Brightest Component A Is Linearly In-supporting

confidence: 62%

“…The four light curves, obtained with two different telescopes and two different methods, show an average weighted root mean square deviation of rms = 1.36σ. A similar test has been carried out by computing with this method the light curves of quasar UM673 (MacAlpine & Feldman (1982), Surdej et al (1987), Surdej et al (1988)), Smette et al (1992), Eigenbrod et al (2007)), which was observed by MiNDSTEp and published by Ricci et al (2013), and comparing the results for the two components with the results obtained in filter V and R by Koptelova et al (2012). The average weighted root mean square deviation is rms = 1.6σ.…”

Section: Photometrymentioning

confidence: 99%

See 2 more Smart Citations

MiNDSTEp differential photometry of the gravitationally lensed quasars WFI 2033-4723 and HE 0047-1756: microlensing and a new time delay

Giannini

Schmidt

Wambsganß

et al. 2016

A&A

Self Cite

View full text Add to dashboard Cite

Aims. We present V and R photometry of the gravitationally lensed quasars WFI 2033-4723 and HE 0047-1756. The data were taken by the MiNDSTEp collaboration with the 1.54 m Danish telescope at the ESO La Silla observatory from 2008 to 2012. Methods. Differential photometry has been carried out using the image subtraction method as implemented in the HOTPAnTS package, additionally using GALFIT for quasar photometry. Results. The quasar WFI 2033-4723 showed brightness variations of order 0.5 mag in V and R during the campaign. The two lensed components of quasar HE 0047-1756 varied by 0.2-0.3 mag within five years. We provide, for the first time, an estimate of the time delay of component B with respect to A of ∆t = (7.6 ± 1.8) days for this object. We also find evidence for a secular evolution of the magnitude difference between components A and B in both filters, which we explain as due to a long-duration microlensing event. Finally we find that both quasars WFI 2033-4723 and HE 0047-1756 become bluer when brighter, which is consistent with previous studies.

show abstract

Section: Time Delay For He 0047-1756supporting

confidence: 69%

Section: The Light Curve Of the Brightest Component A Is Linearly In-supporting

confidence: 62%

Section: Photometrymentioning

confidence: 99%

See 1 more Smart Citation

MiNDSTEp differential photometry of the gravitationally lensed quasars WFI 2033-4723 and HE 0047-1756: microlensing and a new time delay

Giannini

Schmidt

Wambsganß

et al. 2016

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…The other possibility is to study the quasars in the strong lensing systems and remove any intrinsic variations in the light curve by shifting the light curves according to the time delay between the images [41]. This method in recent years is used for detecting microlensing signals in the geometric optics regime [46,62,63].…”

Section: Observational Prospect and Optical Depthmentioning

confidence: 99%

Primordial black hole detection through diffractive microlensing

2018

Self Cite

View full text Add to dashboard Cite

Recent observations of gravitational waves motivate investigations for the existence of Primordial Black Holes (PBHs). We propose the observation of gravitational microlensing of distant quasars for the range of infrared to the submillimeter wavelengths by sub-lunar PBHs as lenses. The advantage of observations in the longer wavelengths, comparable to the Schwarzschild radius of the lens (i.e. R sch λ) is the detection of the wave optics features of the gravitational microlensing. The observation of diffraction pattern in the microlensing light curve of a quasar can break the degeneracy between the lens parameters and determine directly the lens mass as well as the distance of the lens from the observer. We estimate the wave optics optical-depth, also calculate the rate of ∼ 0.1 to ∼ 0.3 event per year per a quasar, assuming that hundred percent of dark matter is made of sublunar PBHs. Also, we propose a long-term survey of quasars with the cadence of almost one hour to few days to resolve the wave optics features of the light curves to discover PBHs and determine the fraction of dark matter made of sub-lunar PBHs as well as their mass function.

show abstract

“…For the remaining more compact systems we performed a multiple PSF fitting analysis to precise their morphology (pointlike or extended source) and accurate magnitude measurement of each component. We adopted the same PSF fitting technique as that used for the analysis of the gravitational lens systems HE 0435-1223 described in Ricci et al (2011) and UM673 in Ricci et al (2013).…”

Section: The Sample Of Gravitational Lens Candidatesmentioning

confidence: 99%

Search for gravitational lens candidates in the XMM-LSS/CFHTLS common field

Elyiv¹,

Мelnyk²,

Finet³

et al. 2013

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

Our aim was to identify gravitational lens candidates among some 5500 optical counterparts of the X-ray point-like sources in the medium-deep ∼ 11 sq. deg. XMM-LSS survey. We have visually inspected the optical counterparts of each QSOs/AGN using CFHTLS T006 images. We have selected compact pairs and groups of sources which could be multiply imaged QSO/AGN. We have measured the colors and characterized the morphological types of the selected sources using the multiple PSF fitting technique.We found three good gravitational lens candidates: J021511.4-034306, J022234.3-031616 and J022607.0-040301 which consist of pairs of point-like sources having similar colors. On the basis of a color-color diagram and X-ray properties we could verify that all these sources are good QSO/AGN candidates rather than stars. Additional secondary gravitational lens candidates are also reported.

show abstract

Flux and color variations of the doubly imaged quasar UM673

Cited by 6 publications

References 20 publications

MiNDSTEp differential photometry of the gravitationally lensed quasars WFI 2033-4723 and HE 0047-1756: microlensing and a new time delay

MiNDSTEp differential photometry of the gravitationally lensed quasars WFI 2033-4723 and HE 0047-1756: microlensing and a new time delay

Primordial black hole detection through diffractive microlensing

Search for gravitational lens candidates in the XMM-LSS/CFHTLS common field

Contact Info

Product

Resources

About