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Title: First light of the Gemini Planet Imager

Journal Article · · Proceedings of the National Academy of Sciences of the United States of America
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  1. Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States); Stanford Univ., Stanford, CA (United States)
  2. Univ. of California, Berkeley, CA (United States)
  3. Stanford Univ., Stanford, CA (United States)
  4. Univ. of Toronto, ON (Canada)
  5. National Research Council of Canada, Ottawa, ON (Canada)
  6. Space Telescope Science Institute, Baltimore, MD (United States)
  7. Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
  8. Univ. of Arizona, Tucson, AZ (United States)
  9. Princeton Univ., Princeton, NJ (United States)
  10. Gemini Observatory, Hilo, HI (United States)
  11. Univ. of California, Los Angeles, CA (United States)
  12. Arizona State Univ., Tempe, AZ (United States)
  13. Univ. of California, Santa Cruz, CA (United States)
  14. Univ. de Montreal, Montreal, QC (Canada)
  15. National Research Council of Canada Herzberg, Victoria, BC (Canada)
  16. SETI Institute, Mountain View, CA (United States)
  17. NASA Ames Research Center, Mountain View, CA (United States)
  18. American Museum of Natural History, New York, NY (United States)
  19. Cornell Univ., Ithaca, NY (United States)
  20. Space Telescope Science Institute, Baltimore, MD (United States); American Museum of Natural History, New York, NY (United States)
  21. Univ. of Georgia, Athens, GA (United States)
  22. California Inst. of Technology (CalTech), Pasadena, CA (United States)
  23. The John Hopkins Univ., Baltimore, MD (United States)
+ Show Author Affiliations

The Gemini Planet Imager is a dedicated facility for directly imaging and spectroscopically characterizing extrasolar planets. It combines a very high-order adaptive optics system, a diffraction-suppressing coronagraph, and an integral field spectrograph with low spectral resolution but high spatial resolution. Every aspect of the Gemini Planet Imager has been tuned for maximum sensitivity to faint planets near bright stars. During first-light observations, we achieved an estimated H band Strehl ratio of 0.89 and a 5-σ contrast of 106 at 0.75 arcseconds and 105 at 0.35 arcseconds. Observations of Beta Pictoris clearly detect the planet, Beta Pictoris b, in a single 60-s exposure with minimal postprocessing. Beta Pictoris b is observed at a separation of 434 ± 6 milliarcseconds (mas) and position angle 211.8 ± 0.5°. Fitting the Keplerian orbit of Beta Pic b using the new position together with previous astrometry gives a factor of 3 improvement in most parameters over previous solutions. The planet orbits at a semimajor axis of 9.0+0.8–0.4 AU near the 3:2 resonance with the previously known 6-AU asteroidal belt and is aligned with the inner warped disk. In conclusion, the observations give a 4% probability of a transit of the planet in late 2017.

Research Organization:
Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States)
Sponsoring Organization:
USDOE
Grant/Contract Number:
AC52-07NA27344
OSTI ID:
1274052
Report Number(s):
LLNL-JRNL-678638
Journal Information:
Proceedings of the National Academy of Sciences of the United States of America, Vol. 111, Issue 35; ISSN 0027-8424
Publisher:
National Academy of Sciences, Washington, DC (United States)Copyright Statement
Country of Publication:
United States
Language:
English
Citation Metrics:
Cited by: 447 works
Citation information provided by
Web of Science

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Observing Exoplanets with High Dispersion Coronagraphy. I. The Scientific Potential of Current and Next-generation Large Ground and Space Telescopes journal March 2017
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Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
high-contrast imaging
extreme adaptive optics
debris disks