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!

Indices and tables