Welcome to PACMAN’s documentation!
Welcome to the documentation for PACMAN
PACMAN is a pipeline to reduce and analyze Hubble/Wide Field Camera 3 (WFC3) observations of transiting exoplanets. The pipeline runs end-to-end, beginning with a time series of 2D images and ending with a spectrum for the planet.
PACMAN can easily fit multiple observations simultaneously.
The main steps in the pipeline are:
optimally extract spectra from the ‘ima’ data products provided by STScI
bin the spectra into user-specified wavelength bins and output the light curve(s)
fit the light curves with a variety of astrophysical models (transit, eclipse, phase curve) and instrument systematic models (visit-long quadratic trends, orbit-long exponential trends)
estimate uncertainties on the planet parameters with least-squares, MCMC, or nested sampling
For a more detailed roadmap, see Stages.
PACMAN is being developed on GitHub. If you find a bug or want a new feature, please raise an issue!