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GPIES Campaign

Gemini Planet Imager Extra Solar Survey 

The GPIES Campaign is the winning proposal in the CfP for Campaign observations with GPI. It was awarded 890h over six semesters starting in 2014B

GPIES Campaign Executive summary

Program Time usage of the GPIES Campaign

GPIES Observations in GEA

GPIES Campaign Executive summary

The Gemini Planet Imager (GPI) was built as a survey instrument to directly detect planets and image debris disks. Our survey will use GPI to produce the first-ever robust census of giant planet populations in the 5-50 AU range, allowing us to


  1. illuminate the formation pathways of Jovian planets
  2. reconstruct the early dynamical evolution of systems, including migration mechanisms and the interaction with disks and belts of debris
  3. bridge the gap between Jupiter and the brown dwarfs with the first examples of cool lowgravity planetary atmospheres.


The only way to achieve robust and reliable statistical results is with a single coherent survey, with uniform and well-articulated selection criteria. We will observe 600 stars spanning spectral types A-M. We will use published young association catalogs and a proprietary list – the result of thousands of hours of telescope observations in preparation for GPI—that adds several hundred new young (<100 Myr, <75 pc) and adolescent (<300 Myr, <35 pc) stars. The latter, older but closer than the known young associations, allow our survey to probe in to the 5 AU ice line. Monte Carlo simulations of planet populations around these stars allow us to optimize the survey strategy for maximum statistical yield. The range of separations studied by GPI is completely inaccessible to Doppler and transit techniques (even with Kepler)—a new window into planet formation.

Simulations predict this survey will discover approximately 50 exoplanets, increasing the number of exoplanet images by an order of magnitude, enough for statistical investigation. The survey will deliver:

  1. A catalog of detected exoplanets—the principal legacy of this campaign—released for follow-up to the Gemini community within 18 months of observation
  2. For a subset of 10 planets, a library of high-SNR GPI spectra at all 5 bands to calibrate temperature and gravity indicators
  3. For each planet, estimated effective temperatures and luminosities from GPI spectrophotometry, and semi-major axis estimates from orbital motion
  4. Empirical measurements of the number of young planets as a function of mass, semi-major axis, and stellar mass with the same precision as Doppler giant-planet surveys
  5. An estimated eccentricity distribution of a subset of planets sufficient to distinguish different dynamical evolutionary states at the 3-5 sigma level
  6. 6. Snapshot polarimetry images of those stars in the survey predicted to have detectable debris disks
  7. High-SNR polarimetry images of all debris disks showing planet-induced structure
  8. An automated data pipeline to process images and recover calibrated astrometry and photometry
  9. A public catalog containing all reduced images, recovered planetary properties, and detection limits

The large sample will for the first time match the statistical power of extant studies of older planets using indirect techniques. GPI spectroscopy will reveal atmospheric conditions and thermal history, thereby calibrating atmosphere and accretion models. The statistical properties of the distributions will arbitrate between various formation and migration scenarios. 

Program Time usage of the GPIES Campaign

Total allocation is 890 hours over 6 semesters, starting semester 2014B




Night Hours 


























Continued use of 15B program





Continued use of 15B program




















Updated:September 16

43% progress on allocated time*

34% Effectiveness (IQ70 CC50 constraints expected 35%) **

*Progress is the percentage of the progress in completing the allocated 890h

**Percentage is the ratio of "Charged Time" to "Allocated Night hours"  

GPIES Observations in GEA

The Gemini Archive contains the GPIES observations, a link to the observations can be found here: 



GS-2015B-Q-500 data from August 1st, 2015 to January 31st 2016

GS-2015B-Q-500 data from February 1st, 2016 to July 31st 2016

GS-2015B-Q-500 data from August 1st, 2016 to January 31st, 2017

It should be noted that observations have the same proprietary period as regular queue.