Direct detection of extrasolar planets: HR8799 + GPI Bruce Macintosh (LLNL / Stanford) HR8799: Christian Marois (LLNL/HIA), Travis Barman (Lowell), Quinn.
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Direct detection of extrasolar planets: HR8799 + GPI
Bruce Macintosh (LLNL / Stanford)HR8799: Christian Marois (LLNL/HIA), Travis Barman (Lowell), Quinn
Konopacky (LLNL/Toronto), Ben Zuckerman (UCLA)Gemini Planet Imager (I&T phase):
LLNL: Dave Palmer, Lisa Poyneer, Brian Bauman, Dmitry Savransky UC Berkeley: James Graham Toronto: Quinn Konopacky, Jerome Marie, Max Millar-Blanchaer
UC Santa Cruz: Don Gavel, Daren Dillon, Jim Ward, Sloane Wiktorowicz, Naru SadakuniJPL: Kent Wallace Other: Sandrine Thomas, Patrick Ingraham
UCLA: James Larkin, Jeff Chilcote Gemini: Stephen Goodsell, Markus Hartung, Kayla Harding, Brian Wolf, Carlos Quiroz, Fredrik Rantakyro, Pascale Hibon
HIA: Les Saddlmyer, Jennifer Dunn, Dan Kerley, Kris Kaputa, Andre AnthonyAMNH/STScI: Ben Oppenheimer, Remi Soummer, Anand Sivaramakrishnan, Lauret Puyeo,
Marshall Perrin, Schuyler Wolfe Science team leads: Paul Kalas, Rene Doyon, Inseok Song, Dan Fabrycky, Travis Barman, Mark Marley, Quinn Konopacky, Jennifer Patience, Franck Marchis
National Aeronautics and Space AdministrationJet Propulsion LaboratoryCalifornia Institute of Technology
HR 8799 bcde Beta Pic b
GJ 504 b HD 95086 b
Directly imaged planetary systems
Fomalhaut b
GPI installed on the telescope October 31 2013
“First Light” November 11-17 2013
GPI operated smoothly right out of the box – “best Gemini 1st light ever”
Science verification concentrated on known exoplanets
AO first light: November 11 2013
Integral Field Spectrograph (UCLA) produces a spectrum of every pixel
GPI spectral cube of Neptune
GPI image of Beta Pictoris b
Massive planet orbiting Beta Pictoris b
Gemini Planet Imager
3952 seconds60 seconds
Calibration spots
1980 seconds
Gemini NICI (previous generation)
Reaction to first planet images
Beta Pictoris b spectrum
Model T=1600K log(g)=5Massive planet
Beta Pic (VLT) aligned with disk
Beta Pictoris orbit
Beta Pic b orbit
Polarimetry: Massive dust ring around the young star HR4796A
GPI image of HR4696A dust disk
HR4796A
Total light intensity Polarized light
HR4796A: GPI vs Hubble
Hubble Space TelescopeGPI
Light becomes polarized as it scatters off the ring
End of first light
Gemini Planet Imager Exoplanet Survey
Gemini has allocated 890 hours for a 3 year exoplanet survey campaign
GPIES kickoff meeting October 2011
Teams and team leaders
Team Leaders
Target ID: Inseok Song, Jenny Patience
Exoplanet survey: James Graham
Debris disks: Paul Kalas, Mike Fitzgerald
Observing: Bruce Macintosh, Ben Oppenheimer
Data analysis and archiving: Christian Marois, Marshall Perrin
Astrometry and dynamics; Quinn Konopacky, Dan Fabrycky
Theory: Travis Barman, Mark Marley
EPO: Franck Marchis, Ben Oppenheimer
Co-Investigators: Etienne Artigau, Steve Beckwith, Mike Bessel, Doug Brenner, Adrian Brunini, Adam Burrows, Carolina A. Chavero, Christine Chen, Eugene Chiang, Jeffrey Chilcote, Gaspard Duchêne, Jonathan Fortney, Raphaël Galicher, Sasha Hinkley, Robert King, David Lafrenière, James Larkin, Jérôme Maire, Geoff Marcy, Brenda Matthews, James McBride, Ian McLean, Stanimir Metchev, Katie Morzinski, Ruth Murray-Clay, David Palmer, Erik Petigura, Lisa Poyneer, Laurent Pueyo, Roman Rafikov, Ramiro de la Reza, Emily Rice, Patricio Rojo, Robert de Rosa, Maria Teresa Ruiz, Dmitry Savransky, Didier Saumon, Gene Serabyn, Adam Schneider, Mike Shao, Remi Soummer, Anand Sivaramakrishnan, Sandrine Thomas, Carlos A. Torres, Gautam Vasisht, Jean-Pierre Veran, Arthur Vigan, Kent Wallace, Sloane Wiktorowicz, & Ben Zuckerman
Target identification
Model planet discoveries (McBride et al 2011)
Planet detections for hot-start and cold-start scenarios
Dmitry Savransky
Example: recovery of mass function
Dmitry Savransky
Orbital eccentricity measurements
Quinn Konopacky
Distinguishing high and low-eccentricity populations
Spectral characterization T=400-800 K
The future
• GPI currently ~8 times more sensitive than existing AO
• Servicing January-Feb. 2014– Mechanisms– Vibration
• Public data release Feb. 2014• Extended commissioning
March-May 2014– Public science verification April 2014
• Large-scale exoplanet survey begins second half of 2014
Small-particle phase functions (Graham et al 2007)
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