A Fast and Very Accurate Approach to the Computation of Microlensing Magnification Patterns Based on Inverse Polygon Mapping

Mediavilla, E.; Muñoz, J. A.; López, Pablo López; Mediavilla, T.; Abajas, C.; González-Morcillo, Carlos; Gil-Merino, R.

doi:10.1086/508796

Cited by 73 publications

(71 citation statements)

References 12 publications

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“…The magnification maps were calculated using the Inverse Polygon Mapping algorithm (Mediavilla et al 2006(Mediavilla et al , 2011b. We have used canonical values for κ and γ for the four images from Schmidt et al (1998) and put all the mass into equal mass stars.…”

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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“…To compare microlensing magnification estimates for different models to observations, we follow the procedures of Jiménez-Vicente et al (2012). We compute magnification maps for each of the four images in the 10 systems using the Inverse Polygon Mapping technique (Mediavilla et al 2006(Mediavilla et al , 2011a. We take the values for κ and γ provided by Schechter et al (2014), and put 20% of the surface mass density in the form of stars, as derived from microlensing in the optical by Jiménez-Vicente et al (2015).…”

Section: The Dependence Of X-ray Sizes On Black Hole Massmentioning

confidence: 99%

Probing the Dark Matter Radial Profile in Lens Galaxies and the Size of X-Ray Emitting Region in Quasars With Microlensing

Jiménez-Vicente

Mediavilla

Kochanek

et al. 2015

ApJ

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We use X-ray and optical microlensing measurements to study the shape of the dark matter density profile in the lens galaxies and the size of the (soft) X-ray emission region. We show that single epoch X-ray microlensing is sensitive to the source size. Our results, in good agreement with previous estimates, show that the size of the X-ray emission region scales roughly linearly with the black hole mass, with a half-light radius of R r ( 24 14 = ☉ . We simultaneously estimated the fraction of the local surface mass density in stars, finding that the stellar mass fraction is α = 0.20 ± 0.05 at an average radius of R 1.9 e ∼ , where R e is the effective radius of the lens. This stellar mass fraction is insensitive to the X-ray source size and in excellent agreement with our earlier results based on optical data. By combining X-ray and optical microlensing data, we can divide this larger sample into two radial bins. We find that the surface mass density in the form of stars is α = 0.31 ± 0.15 and α = 0.13 ± 0.05 at R (1.3 0.3) e ± and R (2.3 0.3) e ± , respectively, in good agreement with expectations and some previous results.

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A Fast and Very Accurate Approach to the Computation of Microlensing Magnification Patterns Based on Inverse Polygon Mapping

Cited by 73 publications

References 12 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 Dark Matter Radial Profile in Lens Galaxies and the Size of X-Ray Emitting Region in Quasars With Microlensing

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