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

Fohlmeister, Janine; Kochanek, C. S.; Falco, E.; Wambsganß, J.; Morgan, N. D.; Morgan, Christopher W.; Ofek, E. O.; Maoz, Dan; Keeton, Charles R.; Barentine, John C.; Dalton, Gavin; Dembicky, J.; Ketzeback, William; McMillan, R.; Peters, C. S.

doi:10.1086/518018

Cited by 70 publications

(78 citation statements)

References 27 publications

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“…Lovell et al 1998), SDSS J1004+4112 (Fohlmeister et al 2007(Fohlmeister et al , 2008, QSO 0957+561 (e.g. Oscoz et al 2001;Shalyapin et al 2008;Fadely et al 2010).…”

Section: -Class B1600+434 (I)mentioning

confidence: 99%

COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses

Sluse

Chantry

Magain

et al. 2012

A&A

121

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Gravitationally lensed quasars can be used as powerful cosmological and astrophysical probes. We can (i) infer the Hubble constant H 0 based on the so-called time-delay technique, (ii) unveil substructures along the line-of-sight toward distant galaxies, and (iii) compare the shape and the slope of baryons and dark matter distributions in the inner regions of galaxies. To reach these goals, we need highaccuracy astrometry of the quasar images relative to the lensing galaxy and morphology measurements of the lens. In this work, we first present new astrometry for 11 lenses with measured time delays, namely, JVAS B0218+357, SBS 0909+532, RX J0911.4+0551, FBQS J0951+2635, HE 1104-1805, PG 1115+080, JVAS B1422+231, SBS 1520+530, CLASS B1600+434, CLASS B1608+656, and HE 2149-2745. These measurements proceed from the use of the Magain-Courbin-Sohy (MCS) deconvolution algorithm applied in an iterative way (ISMCS) to near-IR HST images. We obtain a typical astrometric accuracy of about 1-2.5 mas and an accurate shape measurement of the lens galaxy. Second, we combined these measurements with those of 14 other lensing systems, mostly from the COSMOGRAIL set of targets, to present new mass models of these lenses. The modeling of these 25 gravitational lenses led to the following results: 1) in four double-image quasars (HE0047-1746, J1226-006, SBS 1520+530, and HE 2149-2745), we show that the influence of the lens environment on the time delay can easily be quantified and modeled, hence putting these lenses with high priority for time-delay determination; 2) for quadruple-image quasars, the difficulty often encountered in reproducing the image positions to milli-arcsec accuracy (astrometric anomaly problem) is overcome by explicitly including the nearest visible galaxy/satellite in the lens model. However, one anomalous system (RXS J1131-1231) does not show any luminous perturber in its vicinity, and three others (WFI 2026-4536, WFI 2033, and B2045+265) have problematic modeling. These four systems are the best candidates for a pertubation by a dark matter substructure along the line-of-sight; 3) we revisit the correlation between the position angle (PA) and ellipticity of the light and of the mass distribution in lensing galaxies. As in previous studies, we find a significant correlation between the PA of the light and of the mass distributions. However, in contrast with these same studies, we find that the ellipticity of the light and of the mass also correlate well, suggesting that the overall spatial distribution of matter is not very different from the baryon distribution in the inner ∼5 kpc of lensing galaxies. This offers a new test for high-resolution hydrodynamical simulations.

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“…Lovell et al 1998), SDSS J1004+4112 (Fohlmeister et al 2007(Fohlmeister et al , 2008, QSO 0957+561 (e.g. Oscoz et al 2001;Shalyapin et al 2008;Fadely et al 2010).…”

Section: -Class B1600+434 (I)mentioning

confidence: 99%

COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses

Sluse

Chantry

Magain

et al. 2012

A&A

121

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“…2. Although slow microlensing was detected in light curves of several lensed quasars (e.g., Gaynullina et al 2005;Fohlmeister et al 2007;Shalyapin et al 2009;Eulaers & Magain 2011), typical gradients are too small to play a role in brightness records over relatively short time segments. For example, Hainline et al (2012) used LQLM I data and more recent measurements from the United States Naval Observatory (USNO) to study the r-band flux ratio of Q0957+561.…”

Section: Time Delays From the Lrt Main Fluctuationsmentioning

confidence: 99%

A 5.5-year robotic optical monitoring of Q0957+561: substructure in a non-local cD galaxy

Shalyapin

Goicoechea

Gil-Merino

2012

A&A

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New light curves of the gravitationally lensed double quasar Q0957+561 in the gr bands during 2008-2010 include densely sampled, sharp intrinsic fluctuations with unprecedentedly high signal-to-noise ratio. These relatively violent flux variations allow us to very accurately measure the g-band and r-band time delays between the two quasar images A and B. Using correlation functions, we obtain that the two time delays are inconsistent with each other at the 2σ level, with the r-band delay exceeding the 417-day delay in the g band by about 3 days. We also studied the long-term evolution of the delay-corrected flux ratio B/A from our homogeneous two-band monitoring with the Liverpool Robotic Telescope between 2005 and 2010. This ratio B/A slightly increases in periods of violent activity, which seems to be correlated with the flux level in these periods. The presence of the previously reported dense cloud within the cD lensing galaxy, along the line of sight to the A image, could account for the observed time delay and flux ratio anomalies.

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“…Of the 14 remaining systems, we did not model the mass distribution for four of them for the following reasons. 8 GHz, 15 GHz ∆t AB 10.1 +1.5 −1.6 (95% CI) 10.7 ± 0.8 HE 0435−1223 (Courbin et al 2011; R ∆t AB 8.4 ± 2.1 9.8 ± 1.1 Blackburne et al 2014) ∆t AC 0.6 ± 2.3 3.1 ± 2.2 ∆t AD 14.9 ± 2.1 13.7 ± 1.0 ∆t BC −7.8 ± 0.8 −8.0 ± 1.0 ∆t BD 6.5 ± 0.7 6.2 ± 1.5 ∆t CD 14.3 ± 0.8 13.6 ± 0.8 SBS 0909+532 (Goicoechea et al 2008; r ∆t AB −50 +2 R ∆t AB 16 ± 2 7.8 ± 14.0 Q0957+561 (Shalyapin et al 2012) r, g ∆t AB 417.4 ± 0.9 420.0 ± 1.4 SDSS J1001+5027 (Rathna Kumar et al 2013) R ∆t AB 119.3 ± 3.3 119.7 ± 1.8 SDSS J1004+4112 (Fohlmeister et al 2007; R, r ∆t AB −40.6 ± 1.8 −37.2 ± 3.1 Fohlmeister et al 2008) ∆t AC −821.6 ± 2.1 −822.5 ± 7.4 ∆t BC −777.1 ± 9.2 SDSS J1029+2623 (Fohlmeister et al 2013) r ∆t A(B+C) 744 ± 10 (90% CI) 734.3 ± 3.8 HE 1104−1805 (Poindexter et al 2007) R, V ∆t AB −152.2 +2.8 …”

Section: H 0 From Pixellated Modeling Of Ten Gravitational Lensesmentioning

confidence: 99%

H₀from ten well-measured time delay lenses

Kumar

Stalin

Prabhu

2015

A&A

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In this work, we present a homogeneous curve-shifting analysis using the difference-smoothing technique of the publicly available light curves of 24 gravitationally lensed quasars, for which time delays have been reported in the literature. The uncertainty of each measured time delay was estimated using realistic simulated light curves. The recipe for generating such simulated light curves with known time delays in a plausible range around the measured time delay is introduced here. We identified 14 gravitationally lensed quasars that have light curves of sufficiently good quality to enable the measurement of at least one time delay between the images, adjacent to each other in terms of arrival-time order, to a precision of better than 20% (including systematic errors). We modeled the mass distribution of ten of those systems that have known lens redshifts, accurate astrometric data, and sufficiently simple mass distribution, using the publicly available PixeLens code to infer a value of H 0 of 68.1 ± 5.9 km s −1 Mpc −1 (1σ uncertainty, 8.7% precision) for a spatially flat universe having Ω m = 0.3 and Ω Λ = 0.7. We note here that the lens modeling approach followed in this work is a relatively simple one and does not account for subtle systematics such as those resulting from line-of-sight effects and hence our H 0 estimate should be considered as indicative.

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

Cited by 70 publications

References 27 publications

COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses

COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses

A 5.5-year robotic optical monitoring of Q0957+561: substructure in a non-local cD galaxy

H₀from ten well-measured time delay lenses

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

Cited by 70 publications

References 27 publications

COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses

COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses

A 5.5-year robotic optical monitoring of Q0957+561: substructure in a non-local cD galaxy

H0from ten well-measured time delay lenses

Contact Info

Product

Resources

About

H₀from ten well-measured time delay lenses