This listing of credits is incomplete. Suggestions and improvements welcome. Consult the svn repository history or the Release Notes for the full details of who did what when.
Pipeline architecture design, initial algorithms development, core structure, GUI frameworks, and many primitives by Jerome Maire and Marshall Perrin.
Patrick Ingraham developed many of the primitives, led major aspects of IFS calibration and testing, and extensively contributed to analyses and documentation. Dmitry Savransky made major contributions to pipeline primitives, infrastructure, and GPItv. Jean-Baptiste “JB” Ruffio vanquished many bugs, enhanced the destriping and microphonics removal primitives, and wrote portions of the documentation. Max Millar-Blanchaer contributed to polarization mode primitives and GPItv polarization support, and with Sloane Wiktorowicz calibrated the instrumental polarization. Schuyler Wolff developed and tested the PSF-fitting wavelength calibration algorithm, improved the Data Parser, made other pipeline improvements, and contributed significantly to this documentation. Naru Sarakuni extensively supported integration and test, and contributed improvements to GPItv. Christian Marois contributed to improving PSF subtraction algorithms and contrast measurement code. Zack Draper developed improved datacube extraction routines and tools for fitting flexure. Jason Wang contributed to satellite spot fitting, improved the installation system, and contributed improvements to GPItv.
Jeff Chilcote provided guidance on detector operations and calibrations. Alexandra Greenbaum is leading development of nonredundant aperture masking interferometry algorithms applied to GPI, and also contributed to this documentation. Tyler Barker implemented the KLIP algorithm, under guidance from Dmitry. Steven Beckwith analyzed detector testing data to assess optimal readout modes. Quinn Konopacky developed the distortion correction primitive along with Jerome. Franck Marchis oversees the computer infrastructure at the SETI Institute hosting software repositories and documentation, and supervised visiting student JB Ruffio. Laurent Pueyo contributed to data analyses and algorithms development. Some utility functions used in the pipeline are by Mathilde Bealieau, David Lafreniere, Jean-Francois Lavigne, and Lisa Poyneer.
Rene Doyon was subsystem PI for the GPI DRP as part of the GPI project, and provided top-level guidance in overall pipeline design. James Graham developed core algorithm concepts for the polarization reduction, which were subsequently implemented by Marshall and enhanced by Max. Bruce Macintosh maintained overall coherence of the GPI project wavefront.
From Gemini, Stephen Goodsell kept the project on track. Carlos Quiroz and Fredrik Rantakyro supported the Gemini Data System, including establishment of interfaces and extensive implementation and testing. Kathleen Labrie provided valuable input from Gemini’s perspective during software reviews.
The GPI pipeline software architecture was inspired by, and portions of the backbone code re-used from, the Keck OSIRIS pipeline. The OSIRIS pipeline was developed by James Larkin, Shelley Wright, Jason Weiss, Mike McElwain, Marshall Perrin, Christof Iserlohe, Alfred Krabbe, Tom Gasaway, and Tommer Wizanski.
The Recipe Editor was inspired by the OSIRIS ODRFGUI, orginally written in Java by Jason Weiss. Jerome Maire and Marshall Perrin reimplemented it in a modified form in IDL, with improvements contributed by several team members.
GPItv is based on atv by Aaron Barth et al. The Header Viewer dialog in gpitv is taken from the OSIRIS Quicklook tool ql2, itself derived from the NIRC2/NIRspec quicklook. The “Browse Files” dialog is based upon code derived from David Fanning’s tool selectimage.pro.
The GPI data pipeline is built upon an extensive foundation of other open source software from the astronomical community, including but not limited to the Goddard IDL Astronomy Pipeline, the JHUAPL library, Craig Markwardt’s MPFIT library, Liam Gumley’s IMDISP.PRO, and many other individual tools.