Recurrence of the Blue Wing Enhancements in the High-Ionization Lines of SDSS 1004+4112A

Gómez-Álvarez, P.; Mediavilla, E.; Muñoz, J. A.; Arribas, S.; Sanchez, S. F.; Oscoz, A.; Prada, Francisco; Serra-Ricart, M.

doi:10.1086/506147

Cited by 24 publications

(36 citation statements)

References 22 publications

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“…The second season shows no obvious features that can be used to measure the delay. The second important point to note is that the A / B flux ratio has changed significantly between the first and third seasons, indicating that microlensing is occurring in this system as has been previously suggested by variations in the C iv emission-line profile (Richards et al 2004;Lamer et al 2006;Gómez-Á lvarez et al 2006 within each season of the light curves. Of the many techniques for calculating time delays from light curves (e.g., Gil-Merino et al 2002;Pelt et al 1994;Press et al 1992;Kochanek et al 2006a), we apply three.…”

Section: Datamentioning

confidence: 54%

“…This result provides strong evidence that the differential changes in the A/ B emission line profiles are also due to microlensing ( Richards et al 2004;Lamer et al 2006;Gómez-Á lvarez et al 2006) rather than variable absorption in the source (Green 2006). The microlensing timescales in SDSS J1004+4112 should be relatively shorter than in most single galaxy lenses because the internal velocities of the cluster are about 3 times higher than those of a galaxy.…”

Section: Discussionmentioning

confidence: 77%

“…Because the cluster has a higher velocity dispersion (700 km s À1 ) than a typical galaxy lens ($200 km s À1 ), the microlensing timescales in this system may also be shorter than for a typical lens by about a factor of 3. There is already evidence for microlensing from the time variability of the C iv k1549 line in image A that is not observed in image B ( Richards et al 2004;Lamer et al 2006;Gómez-Á lvarez et al 2006), although recently Green (2006) has suggested that this could also be due to time variable absorption in the source quasar.…”

Section: Introductionmentioning

confidence: 99%

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A Time Delay for the Cluster‐lensed Quasar SDSS J1004+4112

Fohlmeister

Kochanek

Falco

et al. 2007

ApJ

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We present 426 epochs of optical monitoring data spanning 1000 days from 2003 December to 2006 June for the gravitationally lensed quasar SDSS J1004+4112. The time delay between the A and B images is Át BA ¼ 38:4 AE 2:0 days (Á 2 ¼ 4) in the expected sense that B leads A and the overall time ordering is C-B-A-D-E. The measured delay invalidates all published models. The models probably failed because they neglected the perturbations from cluster member galaxies. Models including the galaxies can fit the data well, but conclusions about the cluster mass distribution should await the measurement of the longer, and less substructure sensitive, delays of the C and D images. For these images, a delay of Át CB ' 681 AE 15 days is plausible but requires confirmation, while delays of Át CB > 560 days and Át AD > 800 days are required. We clearly detect microlensing of the A / B images, with the delay-corrected flux ratios changing from m B À m A ¼ 0:44 AE 0:01 mag in the first season to 0:29 AE 0:01 mag in the second season and 0:32 AE 0:01 mag in the third season.

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Section: Datamentioning

confidence: 54%

Section: Discussionmentioning

confidence: 77%

Section: Introductionmentioning

confidence: 99%

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A Time Delay for the Cluster‐lensed Quasar SDSS J1004+4112

Fohlmeister

Kochanek

Falco

et al. 2007

ApJ

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“…Abajas et al (2002) have estimated which gravitational lens systems are more likely to show BLR changes due to microlensing. Some examples of these variations in the BLR have been presented by Filippenko (1989), Chartas et al (2002), Chartas et al (2004), Richards et al (2004), Gómez-Álvarez et al (2006), and Sluse et al (2011) in the cases of MG0414+0534, H1413+117, SDSS1004+4112, and Q2237+0305.…”

Section: Continuum Microlensing Measurementmentioning

confidence: 99%

Measuring Microlensing Using Spectra of Multiply Lensed Quasars

Motta

Mediavilla

Falco

et al. 2012

ApJ

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We report on a program of spectroscopic observations of gravitationally lensed QSOs with multiple images. We seek to establish whether microlensing is occurring in each QSO image using only single-epoch observations. We calculate flux ratios for the cores of emission lines in image pairs to set a baseline for no microlensing. The offset of the continuum flux ratios relative to this baseline yields the microlensing magnification free from extinction, as extinction affects the continuum and the lines equally. When we find chromatic microlensing, we attempt to constrain the size of the QSO accretion disk. SDSSJ1004+4112 and HE1104-1805 show chromatic microlensing with amplitudes 0.2 < |Δm| < 0.6 and 0.2 < |Δm| < 0.4 mag, respectively. Modeling the accretion disk with a Gaussian source (I ∝ exp(−R 2 /2r 2 s )) of size r s ∝ λ p and using magnification maps to simulate microlensing, we find r s (λ3363) = 7 ± 3 lt-day(18.1 ± 7.8 × 10 15 cm) and p = 1.1 ± 0.4 for SDSS1004+4112, and r s (λ3363) = 6±2 lt-day(15.5±5.2×1015 cm) and p = 0.7±0.1 for HE1104-1805. For SDSSJ1029+2623, we find strong chromaticity of ∼0.4 mag in the continuum flux ratio, which probably arises from microlensing, although not all the available data fit within this explanation. For Q0957+561, we measure B − A magnitude differences of 0.4 mag, much greater than the ∼0.05 mag amplitude usually inferred from light-curve variability. It may substantially modify the current interpretations of microlensing in this system, likely favoring the hypothesis of smaller sources and/or larger microdeflectors. For HS0818+1227, our data yield possible evidence of microlensing.

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“…Richards et al (2004) found enhancement of the blue wings of some emission lines in SDSS J1004+4112 that were attributed to microlensing. The blue wing enhancement was also observed by Gómez‐Álvarez et al (2006), but the absence of other microlensing‐induced changes suggested that intrinsic variability may be the cause. The latter has been supported by Lamer et al (2006), who suggest it provides a better explanation than microlensing for differences in X‐ray and ultraviolet variability.…”

Section: Introductionmentioning

confidence: 84%

Gravitational microlensing of a reverberating quasar broad-line region - I. Method and qualitative results★

Garsden

Bate

Lewis

2011

Monthly Notices of the Royal Astronomical Society

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The kinematics and morphology of the broad emission‐line region (BELR) of quasars are the subject of significant debate. The two leading methods for constraining BELR properties are microlensing and reverberation mapping. Here we combine these two methods with a study of the microlensing behaviour of the BELR in Q2237+0305, as a change in continuum emission (a ‘flare’) passes through it. Beginning with some generic models of the BELR – sphere, bicones, disc – we slice in velocity and time to produce brightness profiles of the BELR over the duration of the flare. These are numerically microlensed to determine whether microlensing of reverberation mapping provides new information about the properties of BELRs. We describe our method and show images of the models as they are flaring, and the unlensed and lensed spectra that are produced. Qualitative results and a discussion of the spectra are given in this paper, highlighting some effects that could be observed. Our conclusion is that the influence of microlensing, while not strong, can produce significant observable effects that will help in differentiating the properties of BELRs.

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Recurrence of the Blue Wing Enhancements in the High-Ionization Lines of SDSS 1004+4112A

Cited by 24 publications

References 22 publications

A Time Delay for the Cluster‐lensed Quasar SDSS J1004+4112

A Time Delay for the Cluster‐lensed Quasar SDSS J1004+4112

Measuring Microlensing Using Spectra of Multiply Lensed Quasars

Gravitational microlensing of a reverberating quasar broad-line region - I. Method and qualitative results★

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