6533b7defe1ef96bd12768f2
RESEARCH PRODUCT
Flux and color variations of the quadruply imaged quasar HE 0435-1223
D. RicciJ. PoelsA. ElyivF. FinetP. G. SprimontT. AnguitaV. BozzaP. BrowneM. BurgdorfS. Calchi NovatiM. DominikS. DreizlerM. GlitrupF. GrundahlK. HarpsøeF. HessmanT. C. HinseA. HornstrupM. HundertmarkU. G. JørgensenC. LiebigG. MaierL. ManciniG. MasiM. MathiasenS. RahvarG. ScarpettaJ. SkottfeltC. SnodgrassJ. SouthworthJ. TeuberC. C. ThöneJ. WambsganßF. ZimmerM. ZubJ. Surdejsubject
Point spread functionCosmology and Nongalactic Astrophysics (astro-ph.CO)FluxFOS: Physical sciencesAstrophysicsAstrophysics::Cosmology and Extragalactic AstrophysicsGravitational microlensing01 natural scienceslaw.inventionTelescopeSettore FIS/05 - Astronomia e AstrofisicaObservatorylaw0103 physical sciencesAstrophysics::Solar and Stellar Astrophysics010303 astronomy & astrophysicsgeneral – gravitational lensing; weak – techniques: photometric [quasars]Astrophysics::Galaxy AstrophysicsPhysics010308 nuclear & particles physicsphotometric [Techniques]Astrophysics::Instrumentation and Methods for AstrophysicsAstronomy and AstrophysicsQuasargeneral [Quasars]Spectral bandsSpace and Planetary Scienceastro-ph.COAstrophysics::Earth and Planetary Astrophysicsweak [Gravitational lensing]Astrophysics - Cosmology and Nongalactic Astrophysicsdescription
aims: We present VRi photometric observations of the quadruply imaged quasar HE 0435-1223, carried out with the Danish 1.54m telescope at the La Silla Observatory. Our aim was to monitor and study the magnitudes and colors of each lensed component as a function of time. methods: We monitored the object during two seasons (2008 and 2009) in the VRi spectral bands, and reduced the data with two independent techniques: difference imaging and PSF (Point Spread Function) fitting.results: Between these two seasons, our results show an evident decrease in flux by ~0.2-0.4 magnitudes of the four lensed components in the three filters. We also found a significant increase (~0.05-0.015) in their V-R and R-i color indices. conclusions: These flux and color variations are very likely caused by intrinsic variations of the quasar between the observed epochs. Microlensing effects probably also affect the brightest "A" lensed component.
| year | journal | country | edition | language |
|---|---|---|---|---|
| 2011-01-19 |