Microlensing Planets

Gould, Andrew

doi:10.1007/978-3-319-27458-4_3

Cited by 6 publications

(2 citation statements)

References 80 publications

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“…This means that the dimensions of galaxies are close to the mean distance between galaxies in clusters. Moreover the power spectrum of the matter in the universe can be explored: for weak lensing of large-scale structure (cosmic shear) see Bacon et al (2000) for weak lensing of faint galaxies (gravitational shear) see Wilson et al (2001) 44 For reviews see Roulet & Mollerach (1997), Gould (2001a), Gould (2001b) (Alcock et al, 1993) and EROS (Aubourg et al, 1993) collaborations reported the first microlensing candidates toward the LMC. In the same year the OGLE collaboration (Udalski et al, 1993) found the first candidates in the direction of the Galactic center (see also DUO (Alard et al, 1995)).…”

Section: Microlensingmentioning

confidence: 99%

List of Figures. List of Tables

David¹,

Chacón²

2015

Descriptive Grammar of Bangla

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Section: Microlensingmentioning

confidence: 99%

List of Figures. List of Tables

David¹,

Chacón²

2015

Descriptive Grammar of Bangla

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“…Gravitational microlensing has opened a unique window for probing extrasolar planets beyond the snowline (the minimum radius from a star at which water ice could have condensed) (Mao & Paczynski 1991;Gould & Loeb 1992;Gaudi 2012;Mao 2012;Gould 2016). Among the 132 confirmed microlens planets, 12 were detected in a triple lens event 1 .…”

Section: Introductionmentioning

confidence: 99%

Light Curve Calculations for Triple Microlensing Systems

Kuang,

Mao,

Wang

et al. 2021

Preprint

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We present a method to compute the magnification of a finite source star lensed by a triple lens system based on the image boundary (contour integration) method. We describe a new procedure to obtain continuous image boundaries from solutions of the tenth-order polynomial obtained from the lens equation. Contour integration is then applied to calculate the image areas within the image boundaries, which yields the magnification of a source with uniform brightness. We extend the magnification calculation to limb-darkened stars approximated with a linear profile. In principle, this method works for all multiple lens systems, not just triple lenses. We also include an adaptive sampling and interpolation method for calculating densely covered light curves. The C++ source code and a corresponding Python interface are publicly available.

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Exoplanet Occurrence Rates from Microlensing Surveys

Mróz,

Poleski

2024

Handbook of Exoplanets

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Microlensing Planets

Cited by 6 publications

References 80 publications

List of Figures. List of Tables

List of Figures. List of Tables

Light Curve Calculations for Triple Microlensing Systems

Exoplanet Occurrence Rates from Microlensing Surveys

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