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!


If you use PACMAN in your research, please cite Zieba & Kreidberg (2022). The BibTeX entry for the paper is:

       author = {{Zieba}, Sebastian and {Kreidberg}, Laura},
        title = "{PACMAN: A pipeline to reduce and analyze Hubble Wide Field Camera 3 IR Grism data}",
      journal = {The Journal of Open Source Software},
     keywords = {astronomy, exoplanets, python, Python, spectroscopy, HST, photometry, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics},
         year = 2022,
        month = dec,
       volume = {7},
       number = {80},
          eid = {4838},
        pages = {4838},
          doi = {10.21105/joss.04838},
archivePrefix = {arXiv},
       eprint = {2212.11421},
 primaryClass = {astro-ph.IM},
       adsurl = {https://ui.adsabs.harvard.edu/abs/2022JOSS....7.4838Z},
      adsnote = {Provided by the SAO/NASA Astrophysics Data System}

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