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Proceedings Paper

The integral field spectrograph for the Gemini planet imager
Author(s): James E. Larkin; Jeffrey K. Chilcote; Theodore Aliado; Brian J. Bauman; George Brims; John M. Canfield; Andrew Cardwell; Daren Dillon; René Doyon; Jennifer Dunn; Michael P. Fitzgerald; James R. Graham; Stephen Goodsell; Markus Hartung; Pascale Hibon; Patrick Ingraham; Christopher A. Johnson; Evan Kress; Quinn M. Konopacky; Bruce A. Macintosh; Kenneth G. Magnone; Jerome Maire; Ian S. McLean; David Palmer; Marshall D. Perrin; Carlos Quiroz; Fredrik Rantakyrö; Naru Sadakuni; Leslie Saddlemyer; Andrew Serio; Simon Thibault; Sandrine J. Thomas; Philippe Vallee; Jason L. Weiss
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Paper Abstract

The Gemini Planet Imager (GPI) is a complex optical system designed to directly detect the self-emission of young planets within two arcseconds of their host stars. After suppressing the starlight with an advanced AO system and apodized coronagraph, the dominant residual contamination in the focal plane are speckles from the atmosphere and optical surfaces. Since speckles are diffractive in nature their positions in the field are strongly wavelength dependent, while an actual companion planet will remain at fixed separation. By comparing multiple images at different wavelengths taken simultaneously, we can freeze the speckle pattern and extract the planet light adding an order of magnitude of contrast. To achieve a bandpass of 20%, sufficient to perform speckle suppression, and to observe the entire two arcsecond field of view at diffraction limited sampling, we designed and built an integral field spectrograph with extremely low wavefront error and almost no chromatic aberration. The spectrograph is fully cryogenic and operates in the wavelength range 1 to 2.4 microns with five selectable filters. A prism is used to produce a spectral resolution of 45 in the primary detection band and maintain high throughput. Based on the OSIRIS spectrograph at Keck, we selected to use a lenslet-based spectrograph to achieve an rms wavefront error of approximately 25 nm. Over 36,000 spectra are taken simultaneously and reassembled into image cubes that have roughly 192x192 spatial elements and contain between 11 and 20 spectral channels. The primary dispersion prism can be replaced with a Wollaston prism for dual polarization measurements. The spectrograph also has a pupil-viewing mode for alignment and calibration.

Paper Details

Date Published: 8 July 2014
PDF: 13 pages
Proc. SPIE 9147, Ground-based and Airborne Instrumentation for Astronomy V, 91471K (8 July 2014); doi: 10.1117/12.2056504
Show Author Affiliations
James E. Larkin, Univ. of California, Los Angeles (United States)
Jeffrey K. Chilcote, Univ. of California, Los Angeles (United States)
Theodore Aliado, Univ. of California, Los Angeles (United States)
Brian J. Bauman, Lawrence Livermore National Lab. (United States)
George Brims, Univ. of California, Los Angeles (United States)
John M. Canfield, Univ. of California, Los Angeles (United States)
Andrew Cardwell, Gemini Observatory (Chile)
Daren Dillon, UARC, Univ. of California, Santa Cruz (United States)
René Doyon, Univ. de Montréal (Canada)
Jennifer Dunn, NRC - Herzberg Institute of Astrophysics (Canada)
Michael P. Fitzgerald, Univ. of California, Los Angeles (United States)
James R. Graham, Univ. of California, Berkeley (United States)
Stephen Goodsell, Gemini Observatory (Chile)
Markus Hartung, Gemini Observatory (Chile)
Pascale Hibon, Gemini Observatory (Chile)
Patrick Ingraham, Kavli Institute for Particle Astrophysics and Cosmology, Stanford Univ. (United States)
Univ. de Montréal (Canada)
Christopher A. Johnson, Univ. of California, Los Angeles (United States)
Evan Kress, Univ. of California, Los Angeles (United States)
Quinn M. Konopacky, Dunlap Institute for Astronomy and Astrophysics, Univ. of Toronto (Canada)
Bruce A. Macintosh, Lawrence Livermore National Lab. (United States)
Kavli Institute for Particle Astrophysics and Cosmology, Stanford Univ. (United States)
Kenneth G. Magnone, Univ. of California, Los Angeles (United States)
Jerome Maire, Dunlap Institute for Astronomy and Astrophysics, Univ. of Toronto (Canada)
Ian S. McLean, Univ. of California, Los Angeles (United States)
David Palmer, Lawrence Livermore National Lab. (United States)
Marshall D. Perrin, Space Telescope Science Institute (United States)
Carlos Quiroz, Gemini Observatory (Chile)
Fredrik Rantakyrö, Gemini Observatory (Chile)
Naru Sadakuni, Gemini Observatory (Chile)
Leslie Saddlemyer, NRC - Herzberg Institute of Astrophysics (Canada)
Andrew Serio, Gemini Observatory (Chile)
Simon Thibault, Univ. Laval (Canada)
Sandrine J. Thomas, NASA Ames Research Ctr. (United States)
UARC, Univ. of California, Santa Cruz (United States)
Philippe Vallee, Univ. de Montréal (Canada)
Jason L. Weiss, Univ. of California, Los Angeles (United States)


Published in SPIE Proceedings Vol. 9147:
Ground-based and Airborne Instrumentation for Astronomy V
Suzanne K. Ramsay; Ian S. McLean; Hideki Takami, Editor(s)

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