Discovery of a quadruply lensed quasar: the 'clover leaf H1413 + 117

Magain, Pierre; Surdej, Jean; Swings, Jean-Pierre; Borgeest, U.; Kayser, R.

doi:10.1038/334325a0

Cited by 135 publications

(95 citation statements)

References 6 publications

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“…15 (Wisotzki et al 1999;Anguita et al 2008), similar to the well-known Cloverleaf quasar (Magain et al 1988). It is lensed by two galaxies at almost identical redshift (z G1 = 0.523 ± 0.001, z G2 = 0.526 ± 0.002; Eigenbrod et al 2006).…”

Section: Previous Resultsmentioning

confidence: 91%

MOLECULAR GAS IN LENSEDz>2 QUASAR HOST GALAXIES AND THE STAR FORMATION LAW FOR GALAXIES WITH LUMINOUS ACTIVE GALACTIC NUCLEI

Riechers¹

2011

ApJ

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We report the detection of luminous CO(J = 2→1), CO(J = 3→2), and CO(J = 4→3) emission in the strongly lensed high-redshift quasars B1938+666 (z = 2.059), HE 0230−2130 (z = 2.166), HE 1104−1805 (z = 2.322), and B1359+154 (z = 3.240), using the Combined Array for Research in Millimeter-wave Astronomy. B1938+666 was identified in a "blind" CO redshift search, demonstrating the feasibility of such investigations with millimeter interferometers. These galaxies are lensing-amplified by factors of μ L 11-170, and thus allow us to probe the molecular gas in intrinsically fainter galaxies than currently possible without the aid of gravitational lensing. We report lensing-corrected intrinsic CO line luminosities of L CO = 0.65-21×10 9 K km s −1 pc 2 , translating to H 2 masses of M(H 2 ) = 0.52-17 × 10 9 (α CO /0.8) M . To investigate whether or not the active galactic nucleus (AGN) in luminous quasars substantially contributes to L FIR , we study the L CO -L FIR relation for quasars relative to galaxies without a luminous AGN as a function of redshift. We find no substantial differences between submillimeter galaxies and high-z quasars, but marginal evidence for an excess in L FIR in nearby low-L FIR AGN galaxies. This may suggest that an AGN contribution to L FIR is significant in systems with relatively low gas and dust content, but only minor in the most far-infrared-luminous galaxies (in which L FIR is dominated by star formation).

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Section: Previous Resultsmentioning

confidence: 91%

MOLECULAR GAS IN LENSEDz>2 QUASAR HOST GALAXIES AND THE STAR FORMATION LAW FOR GALAXIES WITH LUMINOUS ACTIVE GALACTIC NUCLEI

Riechers¹

2011

ApJ

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“…the line-ofsight-dependent extinction. In addition to three metal-line systems of absorption lines at z abs = 1.66, 1.44 and 2.07 (Hazard et al 1984;Magain et al 1988), numerous absorption lines were found at z abs = 0.61÷2.1 Monier et al 1998). The lensing galaxy had not been detected, but its redshift was expected to be z l > 1.…”

Section: Introductionmentioning

confidence: 97%

“…One example of such a long-term investigation of a gravitationally lensed E-mail: talat77@rambler.ru (TAA); jsurdej@ulg.ac.be (OW); owertz@ alumni.ulg.ac.be (AE) quasar is H1413+117, also known as the Clover Leaf, whose spectrum was first observed by Hazard et al (1984) and Drew & Boksenberg (1984). Later it became evident that this object is a lensed quasar displaying four images (Magain et al 1988). This source is relatively distant (z ≈ 2.55) and its brightness classifies it as a highly luminous quasar (M V < −29 and m V ≈ 17), while its spectrum revealed it to be a broad absorption line quasar (Hazard et al 1984).…”

Section: Introductionmentioning

confidence: 99%

Adaptive PSF fitting – a highly performing photometric method and light curves of the GLS H1413+117: time delays and micro-lensing effects

Akhunov

Wertz

Elyiv

et al. 2016

Mon. Not. R. Astron. Soc.

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We present new photometric observations of H1413+117 acquired during seasons between 2001 and 2008 in order to estimate the time delays between the lensed quasar images and to characterize at best the on-going micro-lensing events. We propose a highly performing photometric method called the adaptive point spread function fitting and have successfully tested this method on a large number of simulated frames. This has enabled us to estimate the photometric error bars affecting our observational results. We analysed the V-and R-band light curves and V-R colour variations of the A-D components which show short-and long-term brightness variations correlated with colour variations. Using the χ 2 and dispersion methods, we estimated the time delays on the basis of the R-band light curves over the seasons between 2003 and 2006. We have derived the new values: t AB = −17.4 ± 2.1, t AC = −18.9 ± 2.8 and t AD = 28.8 ± 0.7 d using the χ 2 method (B and C are leading, D is trailing) with 1σ confidence intervals. We also used available observational constraints (resp. the lensed image positions, the flux ratios in mid-IR and two sets of time delays derived in the present work) to update the lens redshift estimation. We obtained z l = 1.95 +0.06 −0.10 which is in good agreement with previous estimations. We propose to characterize two kinds of micro-lensing events: micro-lensing for the A,

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“…H1413+1143 (the Cloverleaf) consists of 4 images of a z = 2.55 quasar with angular separations of 0.77 to 1.36 arcsec (Magain et al 1988;Turnshek et al 1997). …”

Section: H1413+1143mentioning

confidence: 99%

“…The lensing galaxy has only recently been identified (Kneib, Alloin, & Pello 1998;Chantry & Magain 2007), with Magain et al (1988) and Angonin et al (1990) identifying two prominent absorption systems at z = 1.438 and 1.661; for the purposes of this study, and for consistency with Lewis & Belle (1998), we adopt 1 Despite being first proposed by Chwolson (1924) the mean of these two values, z = 1.55, to represent the redshift of the lensing galaxy. One of the images, D, (see Chartas et al (2004)), has been seen to exhibit variability consistent with microlensing (Angonin et al 1990;Kayser et al 1990;Østensen 1997), with Hutsemékers (1993) suggesting that prominent differences in the absorption profiles of the images might be due to selective microlensing of absorbing clouds, with the scale size of these clouds being smaller than the continuum-forming region.…”

Section: H1413+1143mentioning

confidence: 99%

Resolving the Structure at the Heart of BAL Quasars Through Microlensing Induced Polarisation Variability

Hales¹,

Lewis²

2007

Publ. Astron. Soc. Aust

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While amongst the most luminous objects in the universe, many details regarding the inner structure of quasars remain unknown. One such area is the mechanism promoting increased polarisation in the broad absorption line troughs of certain quasars. This study shows how microlensing can be used to differentiate between two popular models that explain such polarisation through a realistic computational analysis. By examining a statistical ensemble of correlation data between two observables (namely image brightness and polarisation of the flux coming from the quasar), it was found that through spectropolarimetric monitoring it would be possible to discern between a model with an external scattering region and a model without one.

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Discovery of a quadruply lensed quasar: the 'clover leaf H1413 + 117

Cited by 135 publications

References 6 publications

MOLECULAR GAS IN LENSEDz>2 QUASAR HOST GALAXIES AND THE STAR FORMATION LAW FOR GALAXIES WITH LUMINOUS ACTIVE GALACTIC NUCLEI

MOLECULAR GAS IN LENSEDz>2 QUASAR HOST GALAXIES AND THE STAR FORMATION LAW FOR GALAXIES WITH LUMINOUS ACTIVE GALACTIC NUCLEI

Adaptive PSF fitting – a highly performing photometric method and light curves of the GLS H1413+117: time delays and micro-lensing effects

Resolving the Structure at the Heart of BAL Quasars Through Microlensing Induced Polarisation Variability

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