Extrasolar Moons as Gravitational Microlenses Christine Liebig
Extrasolar Moons as Gravitational Microlenses Christine Liebig
Extrasolar Moons as Gravitational Microlenses Christine Liebig
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Contents<br />
1 Introduction 3<br />
2 <strong>Gravitational</strong> Lensing 7<br />
2.1 Historical Development . . . . . . . . . . . . . . . . . . . . . . . . . . 7<br />
2.2 B<strong>as</strong>ic Equations . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 8<br />
2.2.1 Triple-Lens Equation . . . . . . . . . . . . . . . . . . . . . . . 11<br />
2.3 Search for Planets via Galactic Microlensing . . . . . . . . . . . . . . 13<br />
3 Method 15<br />
3.1 Magnification Patterns . . . . . . . . . . . . . . . . . . . . . . . . . . 16<br />
3.1.1 The microlens code . . . . . . . . . . . . . . . . . . . . . . . 16<br />
3.1.2 The moonlens code . . . . . . . . . . . . . . . . . . . . . . . . 17<br />
3.2 Light Curves . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 17<br />
3.2.1 Light curve extraction . . . . . . . . . . . . . . . . . . . . . . 18<br />
3.2.2 Light curve fitting . . . . . . . . . . . . . . . . . . . . . . . . 20<br />
3.3 Statistical Analysis . . . . . . . . . . . . . . . . . . . . . . . . . . . . 22<br />
3.3.1 Comparing data and a theoretical model . . . . . . . . . . . . 24<br />
3.3.2 Comparing two theoretical models . . . . . . . . . . . . . . . . 25<br />
4 Choice of Scenarios 31<br />
4.1 Parameters Relevant for Magnification Patterns . . . . . . . . . . . . 31<br />
4.1.1 M<strong>as</strong>s ratio of planet and star . . . . . . . . . . . . . . . . . . 32<br />
4.1.2 M<strong>as</strong>s ratio of moon and planet . . . . . . . . . . . . . . . . . . 32<br />
4.1.3 Angular separation of planet and star . . . . . . . . . . . . . . 33<br />
4.1.4 Angular separation of moon and planet . . . . . . . . . . . . . 35<br />
4.1.5 Position angle of moon with respect to planet-star axis . . . . 37<br />
4.2 Parameters Relevant for Light Curve Analysis . . . . . . . . . . . . . 37<br />
4.2.1 Distance to source plane . . . . . . . . . . . . . . . . . . . . . 38<br />
4.2.2 Distance to lens plane . . . . . . . . . . . . . . . . . . . . . . 38<br />
4.2.3 M<strong>as</strong>s of lensing star . . . . . . . . . . . . . . . . . . . . . . . . 38<br />
4.2.4 Source size . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 39<br />
4.2.5 Sampling rate . . . . . . . . . . . . . . . . . . . . . . . . . . . 41<br />
4.2.6 Photometric uncertainty of observed data . . . . . . . . . . . 42<br />
4.3 The Standard Scenario . . . . . . . . . . . . . . . . . . . . . . . . . . 42<br />
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