NOAO >   Observing Info >   Approved Programs >   2017A-0275

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Program Information for 2017A-0275


PI: Adam Kraus, U. of Texas, Austin, alk@astro.as.utexas.edu
Address: 2515 Speedway Ave, Stop C1400, Austin, TX, USA 78701 USA

CoI: David Lafreniere, University of Montreal
CoI: Michael Ireland, Australian National U.
CoI: Lucas Cieza, Universidad Diego Portales
CoI: Anand Sivramakrishnan, STScI
CoI: Marshall Perrin, STScI
CoI: Alexandra Greenbaum, Johns Hopkins U.
CoI: Peter Tuthill, U. of Sydney
CoI: James Lloyd, Cornell U.
CoI: Sylvestre Lacour, Observatoire de Paris
CoI: Jennifer Patience, Arizona State U.
CoI: Anthony Cheetham, U. of Sydney
CoI: Aaron C Rizzuto, U. of Texas, Austin
CoI: John Carpenter, California Institute of Technology
CoI: Laurent Pueyo, STScI
CoI: David Principe, MIT
CoI: Simon Casassus, Universidad de Chile
CoI: Alice Zurlo, Universidad Diego Portales
CoI: Sasha Hinkley, University of Exeter

Title: The Planetary Systems of Young Massive Stars

Abstract: We propose to use the Gemini Planet Imager with nonredundant mask interferometry (NRM) to study planet formation around 38 massive stars in the Upper Scorpius subgroup of the 10-20 Myr old Scorpius-Centaurus OB association. Sco-Cen is the nearest large population of young massive stars (d=140 pc). Analogs of our own gas giants (5-20 AU) should be quite bright (contrast of ~1000:1 in K-band) but they have projected separations of only ~40-150 mas. This parameter space is inaccessible with the GPI coronagraph (IWA=200 mas), but as our team has demonstrated with precursor science at Keck and VLT, these separations and contrasts are readily probed with NRM. GPI-NRM will reach a contrast (>8 magnitudes, >2000:1 at 5-sigma) which is sufficient to detect massive gas giants in Sco-Cen down to the diffraction limit (~50 mas), and even slightly below. GPI-NRM provides the only means of probing the same region of orbital space for more massive stars as will be probed for closer, less massive stars with coronagraphic imaging. Through this unique approach, our survey will fill a major hole in our understanding of extrasolar planets by measuring the frequency of planetary companions around 2-5 Msun stars, determining the primordial state of planetary systems and testing interior and evolution models of giant planets.

Program Type: Standard/Galactic

Scheduled Nights:
Run 1 (2017A):  GEM-SQ/GPI -- 23.4hrs band 1 (GS-2017A-Q-16)


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