Welcome to PACMAN’s documentation!
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 transmission spectra, emission spectra, or phase curves of the planet. PACMAN supports simultaneous fitting of multiple visits and spectroscopic wavelength bins.
The main steps in the pipeline are:
optimally extract spectra from the
IMAdata products provided by STScIbin the spectra into user-defined wavelength bins and generate spectroscopic light curves
fit the light curves using astrophysical models (transits, eclipses, phase curves) together with instrument systematic models (visit-long quadratic trends, orbit-long exponential trends)
estimate parameters and their uncertainties using least-squares optimization, 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