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!

Contents:

• Installation
• Stages
• Repository Structure
• PACMAN Control File (.pcf)
• Fitting the Light Curves
• The Code (API)
• PACMAN FAQ
• Contact

Quickstart

• Introduction
• Before Running
• Download data
• Stage 00
• Stage 01
• Stage 02
• Stage 03
• Stage 10
• Stage 20
• Stage 21
• Stage 30
• Outputs

Others

• Download data (alternatives)

Indices and tables

• Index

• Module Index

• Search Page