Direct detection of extrasolar planets: HR8799 + GPI Bruce Macintosh (LLNL / Stanford) HR8799: Christian Marois (LLNL/HIA), Travis Barman (Lowell), Quinn.

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)