Integral field spectroscopy of four lensed quasars: analysis of their neighborhood and evidence for microlensing

Anguita, T.; Fauré, C.; Yonehara, A.; Wambsganß, J.; Kneib, Jean-Paul; Covone, G.; Alloin, D.

doi:10.1051/0004-6361:20077306

Cited by 27 publications

(32 citation statements)

References 51 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…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: 96%

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

Riechers¹

2011

ApJ

View full text Add to dashboard Cite

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).

show abstract

Section: Previous Resultsmentioning

confidence: 96%

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

Riechers¹

2011

ApJ

View full text Add to dashboard Cite

show abstract

“…This is not a complete list of known microlensed quasars (see e.g. Richards et al 2004;Anguita et al 2008a), but these systems were among the first quasars lensed by a single lensing galaxy where significant microlensing of the BLR has been unveiled and discussed, with the advantage that the fully processed shows the extracted spectra of the lensed QSO images and of the lensing galaxy derived from the deconvolution. The last three panels f-h) show the calibrated spectra of these components following the procedure explained in Sect.…”

Section: The Extended Samplementioning

confidence: 99%

Microlensing of the broad line region in 17 lensed quasars

Sluse

Hutsemékers

Courbin

et al. 2012

A&A

Self Cite

133

184

View full text Add to dashboard Cite

When an image of a strongly lensed quasar is microlensed, the different components of its spectrum are expected to be differentially magnified owing to the different sizes of the corresponding emitting region. Chromatic changes are expected to be observed in the continuum while the emission lines should be deformed as a function of the size, geometry and kinematics of the regions from which they originate. Microlensing of the emission lines has been reported only in a handful of systems so far. In this paper we search for microlensing deformations of the optical spectra of pairs of images in 17 lensed quasars with bolometric luminosities between 10 44.7−47.4 erg/s and black hole masses 10 7.6−9.8 M . This sample is composed of 13 pairs of previously unpublished spectra and four pairs of spectra from literature. Our analysis is based on a simple spectral decomposition technique which allows us to isolate the microlensed fraction of the flux independently of a detailed modeling of the quasar emission lines. Using this technique, we detect microlensing of the continuum in 85% of the systems. Among them, 80% show microlensing of the broad emission lines. Focusing on the most common emission lines in our spectra (C iii] and Mg ii) we detect microlensing of either the blue or the red wing, or of both wings with the same amplitude. This observation implies that the broad line region is not in general spherically symmetric. In addition, the frequent detection of microlensing of the blue and red wings independently but not simultaneously with a different amplitude, does not support existing microlensing simulations of a biconical outflow. Our analysis also provides the intrinsic flux ratio between the lensed images and the magnitude of the microlensing affecting the continuum. These two quantities are particularly relevant for the determination of the fraction of matter in clumpy form in galaxies and for the detection of dark matter substructures via the identification of flux ratio anomalies.

show abstract

“…2 FWHM). Details on the observations and reductions are given in Anguita et al (2008a). For this data set, it was not possible to separate the spectra of images A and B of H1413+117.…”

Section: Data Collectionmentioning

confidence: 99%

“…In particular, Angonin et al (1990) found that the equivalent width of the emission lines is systematically smaller in component D than observed in the other components, a result which can be interpreted by microlensing of the continuum source, the larger region at the origin of the emission lines being unaffected. This effect, which appeared to last at least a decade (Chae et al 2001;Anguita et al 2008a), offers the possibility to separate the microlensed attenuated continuum (i.e. the absorption profile) from the true emission line profile, thus providing new clues to the formation of BAL profiles (Hutsemékers 1993;Hutsemékers et al 1994).…”

Section: Introductionmentioning

confidence: 99%

Microlensing in H1413+117: disentangling line profile emission and absorption in a broad absorption line quasar

Hutsemékers

Borguet

Sluse

et al. 2010

A&A

Self Cite

View full text Add to dashboard Cite

On the basis of 16 years of spectroscopic observations of the four components of the gravitationally lensed broad absorption line (BAL) quasar H1413+117, covering the ultraviolet to visible rest-frame spectral range, we analyze the spectral differences observed in the P Cygni-type line profiles and have used the microlensing effect to derive new clues to the BAL profile formation. We first find that the absorption gradually decreases with time in all components and that this intrinsic variation is accompanied by a decrease in the intensity of the emission. We confirm that the spectral differences observed in component D can be attributed to a microlensing effect lasting at least a decade. We show that microlensing magnifies the continuum source in image D, leaving the emission line region essentially unaffected. We interpret the differences seen in the absorption profiles of component D as the result of an emission line superimposed onto a nearly black absorption profile. We also find that the continuum source and a part of the broad emission line region are likely de-magnified in component C, while components A and B are not affected by microlensing. Differential dust extinction is measured between the A and B lines of sight. We show that microlensing of the continuum source in component D has a chromatic dependence compatible with the thermal continuum emission of a standard Shakura-Sunyaev accretion disk. Using a simple decomposition method to separate the part of the line profiles affected by microlensing and coming from a compact region from the part unaffected by this effect and coming from a larger region, we disentangle the true absorption line profiles from the true emission line profiles. The extracted emission line profiles appear double-peaked, suggesting that the emission is occulted by a strong absorber, narrower in velocity than the full absorption profile, and emitting little by itself. We propose that the outflow around H1413+117 is constituted by a high-velocity polar flow and a denser, lower velocity disk seen nearly edge-on. Finally, we report on the first ground-based polarimetric measurements of the four components of H1413+117.

show abstract

Integral field spectroscopy of four lensed quasars: analysis of their neighborhood and evidence for microlensing

Cited by 27 publications

References 51 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

Microlensing of the broad line region in 17 lensed quasars

Microlensing in H1413+117: disentangling line profile emission and absorption in a broad absorption line quasar

Contact Info

Product

Resources

About