High-Resolution Optical and Near-Infrared Imaging of the Quadruple Quasar RX J0911.4+0551

Burud, I.; Courbin, F.; Lidman, C.; Jaunsen, A. O.; Hjorth, J.; Østensen, R. H.; Andersen, M. I.; Clasen, J. W.; Wucknitz, O.; Meylan, G.; Magain, Pierre; Stabell, R.; Refsdal, S.

doi:10.1086/311450

Cited by 58 publications

(91 citation statements)

References 9 publications

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“…Although the MCS deconvolution enables one to retrieve accurate photometry, the results are affected by systematic errors (Burud et al 1998) mainly associated with the regularization term λ. The latter works like a local smoothing term by reducing the high frequencies of the background.…”

Section: The Methodsmentioning

confidence: 99%

Multi-wavelength study of the gravitational lens system RXS J113155.4-123155

Sluse

Claeskens²,

Altiéri

et al. 2006

A&A

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Aims. RXS J113155.4-123155 (z = 0.66) is a quadruply imaged lensed quasar with a resolved Einstein Ring. The goal of this paper is to provide a full characterization of this system, and more particularly accurate astrometry and photometry. These observational constraints constitute a mandatory ingredient for the precise determination of the lens mass profile, the derivation of the Hubble constant H 0 from time delay measurements and investigations on the presence of massive substructures in the lensing galaxy. Methods. Visible and near-infrared imaging observations of RXS J113155.4-123155 were carried out at various epochs using several ground based telescopes and the HST. The frames have been deconvolved using the MCS algorithm. A Singular Isothermal Ellipsoid (SIE) + external shear has been used to model the lensing galaxy potential. Results. MCS deconvolution enables us to separate the flux of the QSO (point-like images) from that of its host galaxy and to accurately track the flux variations of the point-like images in various filters. The deconvolved frames unveil several multiply imaged structures in the Einstein ring and an unidentified object in the vicinity of the lensing galaxy. We discuss the lightcurves and the chromatic flux ratio variations and deduce that both intrinsic variability and microlensing took place during a span longer than one year. We demonstrate that microlensing may easily account for the so called anomalous flux ratios presented in the discovery paper. However, the observed flux ratios are still poorly reproduced when modeling the lens potential with a SIE+shear. We argue that this disagreement can hardly be explained by milli-lensing caused by substructures in the lensing galaxy. A solution proposed in Paper II consists in a more complex lens model including an octupole term to the lens gravitational potential.

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Section: The Methodsmentioning

confidence: 99%

Multi-wavelength study of the gravitational lens system RXS J113155.4-123155

Sluse

Claeskens²,

Altiéri

et al. 2006

A&A

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“…RX J0911+0551 is partially resolved into its four images (e.g., Burud et al 1998): with a peak S/N = 11.8 detection of the eastern three closely spaced images and a s 5.64 peak detection of the fourth western image. We measure a total flux from the combined images of ( ) .…”

Section: Rx J0911+0551mentioning

confidence: 99%

A Total Molecular Gas Mass Census in Z ∼ 2–3 Star-Forming Galaxies: Low-J Co Excitation Probes of Galaxies’ Evolutionary States

Sharon

Riechers

Hodge

et al. 2016

ApJ

133

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We present CO(1-0) observations obtained at the Karl G. Jansky Very Large Array for 14z 2 galaxies with existing CO(3-2) measurements, including 11 galaxies thatcontain active galactic nuclei (AGNs) and three submillimeter galaxies (SMGs). We combine this sample with an additional 15z 2 galaxies from the literature that have both CO(1-0) and CO(3-2) measurements in order to evaluate differences in CO excitation between SMGs and AGN host galaxies, tomeasure the effects of CO excitation on the derived molecular gas properties of these populations, and to look for correlations between the molecular gas excitation and other physical parameters. With our expanded sample of CO(3-2)/CO(1-0) line ratio measurements, we do not find a statistically significant difference in the mean line ratio between SMGs and AGN host galaxies as can be found in the literature; we instead find =  r 1.03 0. for both populations combined). We also do not measure a statistically significant difference between the distributions of the line ratios for these populations at the p=0.05 level, although this result is less robust. We find no excitation dependence on the index or offset of the integrated Schmidt-Kennicutt relation for the two CO lines, and weobtain indices consistent with N=1 for the various subpopulations. However, including low-z "normal" galaxies increases our best-fit Schmidt-Kennicutt index toÑ 1.2. While we do not reproduce correlations between the CO line width and luminosity, we do reproduce correlations between CO excitation and star-formation efficiency.

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“…This object was identified as a gravitationally lensed quasar by Bade et al (1997). The image configuration consists of four images in an ''animal paw'' pattern with mutual separations of up to 3B1 ( Burud et al 1998). The object appears to be lensed by a galaxy cluster at z ¼ 0:7689 ( Burud et al 1998;Kneib et al 2000).…”

Section: Rx J09114+0551mentioning

confidence: 99%

“…The image configuration consists of four images in an ''animal paw'' pattern with mutual separations of up to 3B1 ( Burud et al 1998). The object appears to be lensed by a galaxy cluster at z ¼ 0:7689 ( Burud et al 1998;Kneib et al 2000). The QSO itself is a mini-broad absorption line ( BAL) QSO ( Bade et al 1997); in the present data (see below) we detect triangular troughs at blueshifts of 18,700 km s À1 relative to the QSO's broad C iv emission peak ( Fig.…”

Section: Rx J09114+0551mentioning

confidence: 99%

“…Our results are based on a comparison between the spectra of a spatial average of images A1, A2, and A3 on one hand and image B on the other (in the nomenclature for the lensed images established by Burud et al 1998). The B image was always well separated from the others, but because of the small separation between the A images, it was not possible to resolve them separately and components A1, A2, and A3 were partly on the slit simultaneously.…”

Section: Rx J09114+0551mentioning

confidence: 99%

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Expansion and Collapse in the Cosmic Web

Rauch

Becker

Viel

et al. 2005

ApJ

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We study the kinematics of the gaseous cosmic web at high redshift using Ly forest absorption in multiple QSO sight lines. Observations of the projected velocity shifts between Ly absorbers common to the lines of sight to a gravitationally lensed QSO and three more widely separated QSO pairs are used to directly measure the expansion of the cosmic web in units of the Hubble velocity, as a function of redshift and spatial scale. The lines of sight used span a redshift range from about 2 to 4.5 and represent transverse scales from the subkiloparsec range to about 300 h À1 70 physical kpc. Using a simple analytic model and a cosmological hydrodynamic simulation, we constrain the underlying three-dimensional distribution of expansion velocities from the observed line-of-sight distribution of velocity shear across the plane of the sky. The shape of the shear distribution and its width (14.9 km s À1 rms for a physical transverse separation of 61 h À1 70 kpc at z ¼ 2, 30.0 km s À1 for 261 h À1 70 kpc at z ¼ 3:6) are found to be in good agreement with the IGM undergoing large-scale motions dominated by the Hubble flow, making this one of the most direct observations possible of the expansion of the universe. However, modeling the Ly clouds with a simple ''expanding pancake'' model, the average expansion velocity of the gaseous structures causing the Ly forest in the lower redshift (z $ 2) smaller separation (61 kpc) sample appears about 20% lower than the local Hubble expansion velocity.In order to understand the observed velocity distribution further we investigated the statistical distribution of expansion velocities in cosmological Ly forest simulations. The mean expansion velocity in the (z $ 2, separation $ 60 kpc) simulation is indeed somewhat smaller than the Hubble velocity, as found in the real data. We interpret this finding as tentative evidence for some Ly forest clouds breaking away from the Hubble flow and undergoing the early stages of gravitational collapse. However, the distribution of velocities is highly skewed, and the majority of Ly forest clouds at all redshifts from 2 to 3.8 expand with super-Hubble velocities, typically about 5%-20% faster than the Hubble flow. This behavior is explained if most Ly forest clouds in the column density range typically detectable are expanding filaments that stretch and drain into more massive nodes. The significant difference seen in the velocity distributions between the high-and low-redshift samples may conceivably reflect actual peculiar deceleration, the differences in spatial scale, or our selecting higher densities at lower redshift for a given detection threshold for Ly forest lines.We also investigate the alternative possibility that the velocity structure of the general Ly forest could have an entirely different, local origin, as expected if the Ly forest were produced or at least significantly modified by galactic feedback, e.g., winds from star-forming galaxies at high redshift. However, we find no evidence that the observed distribution of veloc...

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High-Resolution Optical and Near-Infrared Imaging of the Quadruple Quasar RX J0911.4+0551

Cited by 58 publications

References 9 publications

Multi-wavelength study of the gravitational lens system RXS J113155.4-123155

Multi-wavelength study of the gravitational lens system RXS J113155.4-123155

A Total Molecular Gas Mass Census in Z ∼ 2–3 Star-Forming Galaxies: Low-J Co Excitation Probes of Galaxies’ Evolutionary States

Expansion and Collapse in the Cosmic Web

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