New observations and gravitational lens models of the Cloverleaf quasar H1413 + 117

Kayser, R.; Surdej, Jean; Condon, J. J.; Kellermann, K. I.; Magain, Pierre; Rémy, M.; Smette, A.

doi:10.1086/169382

Cited by 62 publications

(56 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…These changes are observed in all components, indicating that the time scale of the intrinsic line profile variation is longer than the time delays between the four images. In fact, the longest time delay is not larger than one month according to the observations of Goicoecha & Shalyapin (2010) and in agreement with models 1 (Kayser et al 1990;Chae & Turnshek 1999).…”

Section: Evidence For Microlensingsupporting

confidence: 80%

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

Hutsemékers

Borguet

Sluse

et al. 2010

A&A

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

Section: Evidence For Microlensingsupporting

confidence: 80%

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

Hutsemékers

Borguet

Sluse

et al. 2010

A&A

View full text Add to dashboard Cite

show abstract

“…Theoretical estimations of the time delays have led to values of about several weeks (Kayser et al 1990). The first light curves of the individual lensed images of H1413+117 in the Bessel V filter have been reported by Arnould et al (1993).…”

Section: Introductionmentioning

confidence: 99%

“…Finally, we should note that the only work dedicated to the observational determination of the time delays between the components Kayser et al (1990), respectively. of the Clover Leaf has been performed by Goicoechea & Shalyapin (2010).…”

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.

Self Cite

View full text Add to dashboard Cite

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,

show abstract

“…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. It was conceded, however, that this would require a very precise lensing configuration.…”

Section: H1413+1143mentioning

confidence: 86%

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

Hales¹,

Lewis²

2007

Publ. Astron. Soc. Aust

View full text Add to dashboard Cite

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.

show abstract

New observations and gravitational lens models of the Cloverleaf quasar H1413 + 117

Cited by 62 publications

References 0 publications

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

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

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

Contact Info

Product

Resources

About