Direct detection of extrasolar planets HR 8799 GPI

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Direct detection of extrasolar planets: HR 8799 + GPI Bruce Macintosh (LLNL / Stanford)

Direct detection of extrasolar planets: HR 8799 + GPI Bruce Macintosh (LLNL / Stanford) HR 8799: 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 Sadakuni JPL: 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 Anthony AMNH/STSc. I: 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 Administration Jet Propulsion Laboratory California Institute of Technology

Directly imaged planetary systems HR 8799 bcde GJ 504 b Beta Pic b HD

Directly imaged planetary systems HR 8799 bcde GJ 504 b Beta Pic b HD 95086 b Fomalhaut b

GPI installed on the telescope October 31 2013

GPI installed on the telescope October 31 2013

“First Light” November 11 -17 2013 GPI operated smoothly right out of the box

“First Light” November 11 -17 2013 GPI operated smoothly right out of the box – “best Gemini 1 st light ever” Science verification concentrated on known exoplanets

AO first light: November 11 2013

AO first light: November 11 2013

Integral Field Spectrograph (UCLA) produces a spectrum of every pixel GPI spectral cube of

Integral Field Spectrograph (UCLA) produces a spectrum of every pixel GPI spectral cube of Neptune

GPI image of Beta Pictoris b

GPI image of Beta Pictoris b

Massive planet orbiting Beta Pictoris b Calibration spots Gemini Planet Imager 1980 seconds 60

Massive planet orbiting Beta Pictoris b Calibration spots Gemini Planet Imager 1980 seconds 60 seconds Gemini NICI (previous generation) 3952 seconds

Reaction to first planet images

Reaction to first planet images

Beta Pictoris b spectrum Model T=1600 K log(g)=5 Massive planet

Beta Pictoris b spectrum Model T=1600 K log(g)=5 Massive planet

Beta Pic (VLT) aligned with disk

Beta Pic (VLT) aligned with disk

Beta Pictoris orbit Beta Pic b orbit

Beta Pictoris orbit Beta Pic b orbit

Polarimetry: Massive dust ring around the young star HR 4796 A GPI image of

Polarimetry: Massive dust ring around the young star HR 4796 A GPI image of HR 4696 A dust disk

HR 4796 A Total light intensity Polarized light

HR 4796 A Total light intensity Polarized light

HR 4796 A: GPI vs Hubble Space Telescope GPI

HR 4796 A: GPI vs Hubble Space Telescope GPI

Light becomes polarized as it scatters off the ring

Light becomes polarized as it scatters off the ring

End of first light

End of first light

Gemini Planet Imager Exoplanet Survey Gemini has allocated 890 hours for a 3 year

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:

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 Mc. Bride, Ian Mc. Lean, 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, &

Target identification

Target identification

Model planet discoveries (Mc. Bride et al 2011)

Model planet discoveries (Mc. Bride et al 2011)

Planet detections for hot-start and cold-start scenarios Dmitry Savransky

Planet detections for hot-start and cold-start scenarios Dmitry Savransky

Example: recovery of mass function Dmitry Savransky

Example: recovery of mass function Dmitry Savransky

Orbital eccentricity measurements Quinn Konopacky

Orbital eccentricity measurements Quinn Konopacky

Distinguishing high and low-eccentricity populations

Distinguishing high and low-eccentricity populations

Spectral characterization T=400 -800 K

Spectral characterization T=400 -800 K

The future • GPI currently ~8 times more sensitive than existing AO • Servicing

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)

Small-particle phase functions (Graham et al 2007)