New Developments on Inverse Polygon Mapping to Calculate Gravitational Lensing Magnification Maps: Optimized Computations

Mediavilla, E.; Mediavilla, T.; Muñoz, J. A.; Ariza, O.; López, Pablo López; González-Morcillo, Carlos; Jiménez-Vicente, J.

doi:10.1088/0004-637x/741/1/42

Cited by 56 publications

(65 citation statements)

References 32 publications

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“…The statistical procedure used to estimate the size of the accretion disk and the strength of the chromaticity is a variant of that described in Mediavilla et al (2011a), Muñoz et al (2011) andJiménez-Vicente et al (2012). The main difference is that the observed magnitudes for the four quasar images in the five different bands are used simultaneously to calculate the probability distributions.…”

Section: Resultsmentioning

confidence: 99%

Structure of the Accretion Disk in the Lensed Quasar Q2237+0305 From Multi-Epoch and Multi-Wavelength Narrowband Photometry

Muñoz

Vives-Arias

Mosquera

et al. 2016

ApJ

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We present estimates for the size and the logarithmic slope of the disk temperature profile of the lensed quasar Q2237+0305, independent of the component velocities. These estimates are based on six epochs of multiwavelength narrowband images from the Nordic Optical Telescope. For each pair of lensed images and each photometric band, we determine the microlensing amplitude and chromaticity using pre-existing mid-IR photometry to define the baseline for no microlensing magnification. A statistical comparison of the combined microlensing data (6 epochs×5 narrow bands×6 image pairs) with simulations based on microlensing magnification maps gives Bayesian estimates for the half-light radius oflt-day, and p=0.95±0.33 for the exponent of the logarithmic temperature profile µ -T R p 1 . This size estimate is in good agreement with most recent studies. Other works based on the study of single microlensing events predict smaller sizes, but could be statistically biased by focusing on high-magnification events.

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Section: Resultsmentioning

confidence: 99%

Structure of the Accretion Disk in the Lensed Quasar Q2237+0305 From Multi-Epoch and Multi-Wavelength Narrowband Photometry

Muñoz

Vives-Arias

Mosquera

et al. 2016

ApJ

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“…, 10. The 517 magnification maps were created using the Inverse Polygon Mapping algorithm described by Mediavilla et al (2006Mediavilla et al ( , 2011a. We used equal mass microlenses of 1 M .…”

Section: Statistical Analysis and Resultsmentioning

confidence: 99%

Dark Matter Mass Fraction in Lens Galaxies: New Estimates From Microlensing

Jiménez-Vicente

Mediavilla

Kochanek

et al. 2015

ApJ

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We present a joint estimate of the stellar/dark matter mass fraction in lens galaxies and the average size of the accretion disk of lensed quasars based on microlensing measurements of 27 quasar image pairs seen through 19 lens galaxies. The Bayesian estimate for the fraction of the surface mass density in the form of stars is α = 0.21 ± 0.14 near the Einstein radius of the lenses (∼1-2 effective radii). The estimate for the average accretion disk size is R 1/2 = 7.9 +3.8 −2.6 √ M/0.3 M light days. The fraction of mass in stars at these radii is significantly larger than previous estimates from microlensing studies assuming quasars were point-like. The corresponding local dark matter fraction of 79% is in good agreement with other estimates based on strong lensing or kinematics. The size of the accretion disk inferred in the present study is slightly larger than previous estimates.

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“…The procedure we use to separate microlensing and extinction consist of measuring the displacement between the continuum and the core of the emission line flux ratios (e.g., see Mediavilla et al 2009Mediavilla et al , 2011Motta et al 2012;Guerras et al 2013;Rojas et al 2014). Thus, the baseline for no-microlensing is established by using the line core fluxes.…”

Section: Methodsmentioning

confidence: 99%

Probing the Broad-Line Region and the Accretion Disk in the Lensed Quasars HE 0435-1223, WFI 2033-4723, and HE 2149-2745 Using Gravitational Microlensing

Motta

Mediavilla

Rojas

et al. 2017

ApJ

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-2 -We use single-epoch spectroscopy of three gravitationally lensed quasars, HE0435-1223, WFI2033-4723, and HE2149-2745, to study their inner structure (BLR and continuum source). We detect microlensing-induced magnification in the wings of the broad emission lines of two of the systems (HE0435-1223 and WFI2033-4723). In the case of WFI2033-4723, microlensing affects two "bumps" in the spectra which are almost symmetrically arranged on the blue (coincident with an Al III emission line) and red wings of C III]. These match the typical double-peaked profile that follows from disk kinematics. The presence of microlensing in the wings of the emission lines indicates the existence of two different regions in the BLR: a relatively small one with kinematics possibly related to an accretion disk, and another one that is substantially more extended and insensitive to microlensing. There is good agreement between the estimated size of the region affected by microlensing in the emission lines, r s = 10 M/M ⊙ light-days. The estimates of p, the exponent of the size vs. wavelength (r s ∝ λ p ), are 1.2 ± 0.6, 0.8 ± 0.2, and 0.4 ± 0.3 for HE0435-1223, WFI2033-4723, and HE2149-2745, respectively. In conclusion, the continuum microlensing amplitude in the three quasars and chromaticity in WFI2033-4723 and HE2149-2745 are below expectations for the thin disk model. The disks are larger and their temperature gradients are flatter than predicted by this model.

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New Developments on Inverse Polygon Mapping to Calculate Gravitational Lensing Magnification Maps: Optimized Computations

Cited by 56 publications

References 32 publications

Structure of the Accretion Disk in the Lensed Quasar Q2237+0305 From Multi-Epoch and Multi-Wavelength Narrowband Photometry

Structure of the Accretion Disk in the Lensed Quasar Q2237+0305 From Multi-Epoch and Multi-Wavelength Narrowband Photometry

Dark Matter Mass Fraction in Lens Galaxies: New Estimates From Microlensing

Probing the Broad-Line Region and the Accretion Disk in the Lensed Quasars HE 0435-1223, WFI 2033-4723, and HE 2149-2745 Using Gravitational Microlensing

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