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Proceedings Article

The Gemini Planet Imager

[+] Author Affiliations
Bruce Macintosh, David Palmer, Brian Bauman, Julia Evans, Lisa Poyneer

NSF Ctr. for Adaptive Optics and Lawrence Livermore National Lab.

James Graham

NSF Ctr. for Adaptive Optics and Univ. of California at Berkeley

Rene Doyon

Univ. de Montreal (Canada)

Don Gavel, Katie Morzinski

NSF Ctr. for Adaptive Optics and Univ. of California, Santa Cruz

James Larkin

NSF Ctr. for Adaptive Optics and Univ. of California, Los Angeles

Ben Oppenheimer, Anand Sivaramakrishnan, Remi Soummer

NSF Ctr. for Adaptive Optics and American Museum of Natural History

Leslie Saddlemyer, Darren Erikson, Jean-Pierre Veran

Herzberg Institute of Astrophysics (Canada)

J. Kent Wallace

NSF Ctr. for Adaptive Optics and Jet Propulsion Lab.

Donald Phillion

Lawrence Livermore National Lab.

Simon Thibault

Immervision (Canada)

Proc. SPIE 6272, Advances in Adaptive Optics II, 62720L (June 27, 2006); doi:10.1117/12.672430
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From Conference Volume 6272

  • Advances in Adaptive Optics II
  • Orlando, Florida , USA | May 24, 2006

abstract

The next major frontier in the study of extrasolar planets is direct imaging detection of the planets themselves. With high-order adaptive optics, careful system design, and advanced coronagraphy, it is possible for an AO system on a 8-m class telescope to achieve contrast levels of 10-7 to 10-8, sufficient to detect warm self-luminous Jovian planets in the solar neighborhood. Such direct detection is sensitive to planets inaccessible to current radial-velocity surveys and allows spectral characterization of the planets, shedding light on planet formation and the structure of other solar systems. We have begun the construction of such a system for the Gemini Observatory. Dubbed the Gemini Planet Imager (GPI), this instrument should be deployed in 2010 on the Gemini South telescope. It combines a 2000-actuator MEMS-based AO system, an apodized-pupil Lyot coronagraph, a precision infrared interferometer for real-time wavefront calibration at the nanometer level, and a infrared integral field spectrograph for detection and characterization of the target planets. GPI will be able to achieve Strehl ratios > 0.9 at 1.65 microns and to observe a broad sample of science targets with I band magnitudes less than 8. In addition to planet detection, GPI will also be capable of polarimetric imaging of circumstellar dust disks, studies of evolved stars, and high-Strehl imaging spectroscopy of bright targets. We present here an overview of the GPI instrument design, an error budget highlighting key technological challenges, and models of the system performance.

© (2006) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.
Citation

Bruce Macintosh ; James Graham ; David Palmer ; Rene Doyon ; Don Gavel, et al.
"The Gemini Planet Imager", Proc. SPIE 6272, Advances in Adaptive Optics II, 62720L (June 27, 2006); doi:10.1117/12.672430; http://dx.doi.org/10.1117/12.672430


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