Microlensing Constraints on Broad Absorption and Emission Line Flows in the Quasar H1413+117

O’Dowd, Matthew; Bate, N. F.; Webster, R. L.; Labrie, Kathleen; Rogers, Joshua

doi:10.1088/0004-637x/813/1/62

Cited by 17 publications

(17 citation statements)

References 74 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…2, the C IV 1550 Å line in the fiducial model is typically formed between 100 and 1000 r G (∼10 17 -10 18 cm). This is in rough agreement with the reverberation mapping results of Kaspi et al (2007) for the 2.6 × 10 9 M quasar S5 0836+71, and also compares favourably with microlensing measurements of the size of the C IV 1550 Å emission line region in the BALQSO H1413+117 (O'Dowd et al 2015). Fig.…”

Section: Physical Conditions and Ionization Statesupporting

confidence: 89%

Testing Quasar Unification: Radiative Transfer in Clumpy Winds

Matthews¹

2017

Disc Winds Matter

View full text Add to dashboard Cite

Section: Physical Conditions and Ionization Statesupporting

confidence: 89%

Testing Quasar Unification: Radiative Transfer in Clumpy Winds

Matthews¹

2017

Disc Winds Matter

View full text Add to dashboard Cite

“…It is common in spectroscopic observations of microlensed quasars to find that only one image is strongly affected (see e.g. O'Dowd et al 2015;MacLeod et al 2015;Motta et al 2017), and saddle point images in close image pairs are known to be more strongly effected by microlensing (Schechter & Wambsganss 2002;Vernardos et al 2014). Nevertheless, by restricting the microlensing to a single image we do exclude some chromatic signatures from our sample of mock observations.…”

Section: Additional Simulation Caveatsmentioning

confidence: 99%

HST imaging of four gravitationally lensed quasars

Bate

Vernardos

O’Dowd

et al. 2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present new HST WFPC3 imaging of four gravitationally lensed quasars: MG 0414+0534; RXJ 0911+0551; B 1422+231; WFI J2026-4536. In three of these systems we detect wavelength-dependent microlensing, which we use to place constraints on the sizes and temperature profiles of the accretion discs in each quasar. Accretion disc radius is assumed to vary with wavelength according to the power-law relationship r ∝ λ p , equivalent to a radial temperature profile of T ∝ r −1/p . The goal of this work is to search for deviations from standard thin disc theory, which predicts that radius goes as wavelength to the power p = 4/3. We find a wide range of power-law indices, from p = 1.4 +0.5 −0.4 in B 1422+231 to p = 2.3 +0.5 −0.4 in WFI J2026-4536. The measured value of p appears to correlate with the strength of the wavelength-dependent microlensing. We explore this issue with mock simulations using a fixed accretion disc with p = 1.5, and find that cases where wavelength-dependent microlensing is small tend to under-estimate the value of p. This casts doubt on previous ensemble singleepoch measurements which have favoured low values using samples of lensed quasars that display only moderate chromatic effects. Using only our systems with strong chromatic microlensing we prefer p > 4/3, corresponding to shallower temperature profiles than expected from standard thin disc theory.

show abstract

“…A detailed study of microlensing in the lensed BAL quasar H1413+117 provided interesting constraints on the outflow. In particular, the C iv λ1550 BAL profile was found to consist of a completely black absorption which starts at an onset velocity of ∼2000 km s −1 and is partially filled in by the broad emission line, thus suggesting diskwind or disk-wind and polar outflows (Hutsemékers et al 2010;O'Dowd et al 2015). An extended source of continuum was uncovered in addition to the compact, microlensed one .…”

Section: Introductionmentioning

confidence: 99%

Spatially separated continuum sources revealed by microlensing in the gravitationally lensed broad absorption line quasar SDSS J081830.46+060138.0

Hutsemékers

Sluse

Kumar

2020

A&A

View full text Add to dashboard Cite

Gravitational microlensing is a powerful tool for probing the inner structure of distant quasars. In this context, we have obtained spectropolarimetric observations of the two images of the broad absorption line (BAL) quasar SDSS J081830.46+060138.0 (J0818+0601) at redshift z ≃ 2.35. We first show that J0818+0601 is actually gravitationally lensed, and not a binary quasar. A strong absorption system detected at z = 1.0065±0.0002 is possibly due to the lensing galaxy. Microlensing is observed in one image and it magnifies the emission lines, the continuum, and the BALs differently. By disentangling the part of the spectrum that is microlensed from the part that is not microlensed, we unveil two sources of continuum that must be spatially separated: a compact one, which is microlensed, and an extended one, which is not microlensed and contributes to two thirds of the total continuum emission. J0818+0601 is the second BAL quasar in which an extended source of rest-frame ultraviolet continuum is found. We also find that the images are differently polarized, suggesting that the two continua might be differently polarized. Our analysis provides constraints on the BAL flow. In particular, we find that the outflow is seen with a nonzero onset velocity, and stratified according to ionization. ⋆ Based on observations made with ESO Very Large Telescope at the Paranal Observatory under program ID 100.B-0590. The reduced spectra are available at the CDS via anonymous ftp to

show abstract

Microlensing Constraints on Broad Absorption and Emission Line Flows in the Quasar H1413+117

Cited by 17 publications

References 74 publications

Testing Quasar Unification: Radiative Transfer in Clumpy Winds

Testing Quasar Unification: Radiative Transfer in Clumpy Winds

HST imaging of four gravitationally lensed quasars

Spatially separated continuum sources revealed by microlensing in the gravitationally lensed broad absorption line quasar SDSS J081830.46+060138.0

Contact Info

Product

Resources

About