Outline
- Learn to interpret key light curve features
- Gain familiarity with some of the software tools available for modeling microlensing events
- Practice modeling different events
Shapes of Planetary Caustics in various regions of the parameter space
Shapes of Planetary Caustics as a function of projected separation
Gaudi 2021
Planetary anomalies in the light curve
Estimating Planetary Parameters
- Gaudi & Gould (1997) By-eye fitting
- Gould and Loeb (1992)
$$s = \frac{u \pm \sqrt{u^{2} + 4}}{2},$$
where
$$u = \sqrt{u_{0}^{2} + \left(\frac{t_{0}-t_{p}}{t_{E}}\right)^{2}}$$
$$t_{Ep} = \sqrt{(q + \rho^{2})} \times t_{E}, \rho = \frac{t_{*}}{t_{E}}$$
Estimating the Projected Separation
$$u = \sqrt{u_{0}^{2} + \left(\frac{t_{0}-t_{p}}{t_{E}}\right)^{2}}$$
$$s = \frac{u \pm \sqrt{u^{2} + 4}}{2}$$
Minor Image vs Major Image Perturbation
Minor Image vs Major Image Perturbation
When ρ > caustic
$$\rho = \frac{t_{*}}{t_{E}}$$
Image Gallery
The following images illustrate the light curve features (aka perturbations) corresponding with different source images and caustic structures.
Review these images, then work through the notebooks provided, using the gallery to interpret the light curves in the exercises.
Minor Image Perturbation
Major Image Perturbation
Minor Image, ρ < caustic
Major Image, ρ < caustic
Major Image, ρ > caustic
Notebook Exercises
In order to use them, please make sure you have these packages installed in your environment.