Flux and color variations of the quadruply imaged quasar HE 0435-1223

Ricci, Davide; Poels, J.; Elyiv, A.; Finet, F.; Sprimont, Pierre-Guillaume; Anguita, T.; Bozza, V.; Browne, P.; Burgdorf, M.; Novati, S. Calchi; Dominik, M.; Glitrup, M.; Grundahl, F.; Harpsøe, K.; Hessman, F. V.; Hinse, T. C.; Hornstrup, A.; Hundertmark, M.; Jørgensen, U. G.; Liebig, C.; Maier, G.; Mancini, L.; Mathiasen, M.; Rahvar, S.; Scarpetta, G.; Skottfelt, J.; Snodgrass, C.; Southworth, J.; Teuber, J.; Thöne, C. C.; Wambsganß, J.; Zimmer, F.; Zub, M.; Surdej, Jean

doi:10.1051/0004-6361/201016188

Cited by 16 publications

(14 citation statements)

References 20 publications

(42 reference statements)

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“…Since microlensing in the optical bands has been extensively studied in these systems (e.g., Morgan et al 2006;Kochanek et al 2006;Lamer et al 2006;Fohlmeister et al 2007Fohlmeister et al , 2008Eigenbrod et al 2008;Faure et al 2009;Poindexter & Kochanek 2010a, 2010bRicci et al 2011;Blackburne et al 2011), our X-ray microlensing light curves provide complementary data to constrain non-thermal emission processes in accretion disks. For example, a simple comparison of the microlensing variability between the soft and hard X-ray bands in Q 2237+0305 has already led us to conclude that the hard X-ray continuum emission region is smaller than that of the soft in this quasar, suggesting a temperature gradient in the X-ray emitting corona (Chen et al 2011).…”

Section: Notesmentioning

confidence: 97%

X-RAY MONITORING OF GRAVITATIONAL LENSES WITHCHANDRA

Chen

Dai

Kochanek

et al. 2012

ApJ

100

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We present Chandra monitoring data for six gravitationally lensed quasars: QJ 0158−4325, HE 0435−1223, SDSS 0924+0219, SDSS 1004+4112, HE 1104−1805, and Q 2237+0305. X-ray microlensing variability is detected in all six lenses with high confidence. We furthermore detect energy-dependent microlensing in HE 0435−1223, SDSS 0924+0219, SDSS 1004+4112, and Q 2237+0305. Through a detailed spectral analysis for each lens we find that simple power-law models plus Gaussian emission lines give good fits to the spectra. We detect intrinsic spectral variability in two epochs of Q 2237+0305, and differential absorption between images in QJ 0158−4325 and Q2237+0305. We also detect the Fe Kα emission line in all six lenses, and the Ni xxvii Kα line in two images of Q 2237+0305. The rest-frame equivalent widths of the Fe Kα lines are measured to be 0.4-1.2 keV, significantly higher than those measured in typical active galactic nuclei of similar X-ray luminosities. This suggests that the Fe Kα emission region is more compact or centrally concentrated than the continuum emission region.

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Section: Notesmentioning

confidence: 97%

X-RAY MONITORING OF GRAVITATIONAL LENSES WITHCHANDRA

Chen

Dai

Kochanek

et al. 2012

ApJ

100

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“…That there is microlensing in image A has been suggested based on photometric monitoring (Ricci et al 2011;Courbin et al 2011). Using narrow-band photometric data obtained in 2007, Mosquera et al (2011) have detected chromatic microlensing in the continuum of image A.…”

Section: Detected Microlensing Of the Ciii] And Mgii Lines In The Spementioning

confidence: 99%

Microlensing of the broad-line region in the quadruply imaged quasar HE0435-1223

Braibant

Hutsemékers

Sluse

et al. 2014

A&A

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Using infrared spectra of the z = 1.693 quadruply lensed quasar HE0435-1223 acquired in 2009 with the spectrograph SINFONI at the ESO Very Large Telescope, we have detected a clear microlensing effect in images A and D. While microlensing affects the blue and red wings of the Hα line profile in image D very differently, it de-magnifies the line core in image A. The combination of these different effects sets constraints on the line-emitting region; these constraints suggest that a rotating ring is at the origin of the Hα line. Visible spectra obtained in 2004 and 2012 indicate that the MgII line profile is microlensed in the same way as the Hα line. Our results therefore favour flattened geometries for the low-ionization line-emitting region, for example, a Keplerian disk. Biconical models cannot be ruled out but require more fine-tuning. Flux ratios between the different images are also derived and confirm flux anomalies with respect to estimates from lens models with smooth mass distributions.

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“…We treated the images following the same procedure as those relative to HE 0435-1223 described in a previous paper (Ricci et al 2011b), with the exception that we used the images already de-biased and flat-fielded in loco by the Interactive Data Language (IDL) automatic pipeline used at the Danish Telescope for the daily monitoring of the bulge microlenses.…”

Section: Observations and Pre-processingmentioning

confidence: 99%

“…We applied the PSF fitting technique while accounting for the magnitude of the lens on the best frames previously chosen, by refining the robust method already used in our previous work (Ricci et al 2011b). …”

Section: Starmentioning

confidence: 99%

“…In previous papers (Ricci et al 2011b,a), we have studied such variations for the quadruply imaged quasar HE 0435-1223, observed in the framework of a VRi multiepoch monitoring of five lensed quasars 1 , a parallel project of the Microlensing Network for the Detection of Small Terrestrial Exoplanets (MiNDSTEp) campaign (Dominik et al 2010). …”

Section: Introductionmentioning

confidence: 99%

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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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Flux and color variations of the quadruply imaged quasar HE 0435-1223

Cited by 16 publications

References 20 publications

X-RAY MONITORING OF GRAVITATIONAL LENSES WITHCHANDRA

X-RAY MONITORING OF GRAVITATIONAL LENSES WITHCHANDRA

Microlensing of the broad-line region in the quadruply imaged quasar HE0435-1223

Flux and color variations of the doubly imaged quasar UM673

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