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!
Citing PACMAN
If you use PACMAN in your research, please cite Zieba & Kreidberg (2022). The BibTeX entry for the paper is:
@ARTICLE{2022JOSS....7.4838Z,
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}
}
Contents:
Quickstart
Others