GPI 2.0: pre-integrated pyramid wavefront sensor results

Saavidra Perera; Jérôme Maire; Clarissa R. Do Ó; Jayke S. Nguyen; Vincent Chambouleyron; Quinn M. Konopacky; Jeffrey Chilcote; Brian Sands; Randall Hamper; Matthew Engstrom; Joeleff Fitzsimmons; Dan Kerley; Bruce Macintosh; Christian Marois; Fredrik Rantakyrö; Dmitry Savransky; Jean-Pierre Veran; Guido Agapito; S. Mark Ammons; Marco Bonaglia; Marc-Andre Boucher; Joel Burke; Daren Dillon; Jennifer Dunn; Simone Esposito; Guillaume Filion; Oyku Galvan; Jean Thomas Landry; Olivier Lardiere; Duan Li; Alex Madurowicz; Teo Mocnik; Dillon Peng; Lisa Poyneer; Carlos Quiroz; Garima Singh; Eckhart Spalding

doi:10.1117/12.3020360

27 August 2024 GPI 2.0: pre-integrated pyramid wavefront sensor results

Saavidra Perera, Jérôme Maire, Clarissa R. Do Ó, Jayke S. Nguyen, Vincent Chambouleyron, Quinn M. Konopacky, Jeffrey Chilcote, Brian Sands, Randall Hamper, Matthew Engstrom, Joeleff Fitzsimmons, Dan Kerley, Bruce Macintosh, Christian Marois, Fredrik Rantakyrö, Dmitry Savransky, Jean-Pierre Veran, Guido Agapito, S. Mark Ammons, Marco Bonaglia, Marc-Andre Boucher, Joel Burke, Daren Dillon, Jennifer Dunn, Simone Esposito, Guillaume Filion, Oyku Galvan, Jean Thomas Landry, Olivier Lardiere, Duan Li, Alex Madurowicz, Teo Mocnik, Dillon Peng, Lisa Poyneer, Carlos Quiroz, Garima Singh, Eckhart Spalding

Author Affiliations +

Proceedings Volume 13097, Adaptive Optics Systems IX; 130971S (2024) https://doi.org/10.1117/12.3020360
Event: SPIE Astronomical Telescopes + Instrumentation, 2024, Yokohama, Japan

Abstract

The Gemini Planet Imager (GPI) is a high-contrast imaging instrument designed to directly detect and characterise young, Jupiter-mass exoplanets. After six years of operation at the Gemini South Telescope in Chile, the instrument is being upgraded and moved to the Gemini North Telescope in Hawaii as GPI 2.0. Several improvements have been made to the adaptive optics (AO) system as part of this upgrade. This includes replacing the current Shack-Hartmann wavefront sensor with a pyramid wavefront sensor (PWFS) and a custom EMCCD. These changes will increase GPI’s sky coverage by accessing fainter targets, improving corrections on fainter stars and allowing faster and ultra-low latency operations on brighter targets. The PWFS subsystem was independently built and tested to verify its performance before being integrated into the GPI 2.0 instrument. This paper will present the pre-integration performance test results, including pupil image quality, throughput and linearity without modulation.

Conference Presentation

(2024) Published by SPIE. Downloading of the abstract is permitted for personal use only.

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Saavidra Perera, Jérôme Maire, Clarissa R. Do Ó, Jayke S. Nguyen, Vincent Chambouleyron, Quinn M. Konopacky, Jeffrey Chilcote, Brian Sands, Randall Hamper, Matthew Engstrom, Joeleff Fitzsimmons, Dan Kerley, Bruce Macintosh, Christian Marois, Fredrik Rantakyrö, Dmitry Savransky, Jean-Pierre Veran, Guido Agapito, S. Mark Ammons, Marco Bonaglia, Marc-Andre Boucher, Joel Burke, Daren Dillon, Jennifer Dunn, Simone Esposito, Guillaume Filion, Oyku Galvan, Jean Thomas Landry, Olivier Lardiere, Duan Li, Alex Madurowicz, Teo Mocnik, Dillon Peng, Lisa Poyneer, Carlos Quiroz, Garima Singh, and Eckhart Spalding "GPI 2.0: pre-integrated pyramid wavefront sensor results", Proc. SPIE 13097, Adaptive Optics Systems IX, 130971S (27 August 2024); https://doi.org/10.1117/12.3020360

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