GPI Data Pipeline Documentation

The Gemini Planet Imager Data Pipeline allows transformation of raw data from GPI into calibrated spectral and polarimetric data cubes. It also provides some basic capabilities for PSF suppression through differential imaging, and for astrometry and spectrophotometry of detected sources.

Software and documentation by: Marshall Perrin (STScI), Jérôme Maire (University of Toronto), Patrick Ingraham (Stanford), Dmitry Savransky (Cornell), Jeff Chilcote (Toronto), Zack Draper (U Victoria), Michael Fitzgerald (UCLA), Kate Follette (Stanford), Alex Greenbaum (JHU), Pascale Hibon (Gemini), Li-Wei Hung (UCLA), Quinn Konopacky (UCSD), Doug Long (STScI), Franck Marchis (SETI), Christian Marois (NRC), Max Millar-Blanchaer (Toronto), Eric Nielsen (Stanford/SETI), Laurent Pueyo (STScI), Abhi Rajan (ASU), Jean-Baptiste Ruffio (Stanford), Naru Sadakuni (UCSC and Gemini), Jason Wang (Berkeley), Schuyler Wolff (JHU), Sloane Wiktorowicz (UCSC), Joe Zalesky (Berkeley) and other members of the GPI Data Analysis Team. Please see the development credits for a complete list of contributors, and the release notes for further details.

Acknowledging the GPI Pipeline in Publications: Users of the GPI data pipeline should cite one of the following. Please also cite appropriate references for GPI overall, the AO system and IFS, and other aspects of the instrument as relevant.

You may wish to see what’s new in the latest version or jump to the quick start tutorial.

New Users Start Here

If you are new to working with GPI data, the following parts of this documentation are good places to start.

Getting Help: The best approach is to email your Gemini contact scientist. Another channel for support of this software is the Gemini Data Reduction Forum. Please post questions there and mark them with the tag gpi. Gemini staff and members of the GPI data analysis team monitor that forum to help support the Gemini community in using GPI. You may also wish to consult the FAQ. Contributions of improvements to the software or this documentation are very much welcomed.


This software comes with no warranty nor guarantee of correctness. It represents the GPI instrument team’s best effort at calibrating and reducing GPI data, but is necessarily a work in progress and incomplete. Integral field spectroscopy, polarimetry, and high contrast PSF subtraction are complicated, and GPI is a new instrument we are still getting to know on sky. Use your own scientific judgement when analyzing and publishing data from GPI.

Indices and tables

Documentation last updated on Dec 05, 2017