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Direct detection of extrasolar planets: HR8799 + GPI

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):

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Direct detection of extrasolar planets: HR8799 + GPI

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  1. 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, NaruSadakuni JPL: Kent Wallace Other: Sandrine Thomas, Patrick Ingraham UCLA: James Larkin, Jeff ChilcoteGemini: 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/STScI: Ben Oppenheimer, RemiSoummer, AnandSivaramakrishnan, LauretPuyeo, 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

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

  3. GPI installed on the telescope October 31 2013

  4. “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

  5. AO first light: November 11 2013

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

  7. GPI image of Beta Pictoris b

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

  9. Reaction to first planet images

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

  11. Beta Pic (VLT) aligned with disk

  12. Beta Pictoris orbit Beta Pic b orbit

  13. Polarimetry: Massive dust ring around the young star HR4796A GPI image of HR4696A dust disk

  14. HR4796A Total light intensity Polarized light

  15. HR4796A: GPI vs Hubble Hubble Space Telescope GPI

  16. Light becomes polarized as it scatters off the ring

  17. End of first light

  18. Gemini Planet Imager Exoplanet Survey Gemini has allocated 890 hours for a 3 year exoplanet survey campaign GPIES kickoff meeting October 2011

  19. 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, RaphaëlGalicher, Sasha Hinkley, Robert King, David Lafrenière, James Larkin, JérômeMaire, Geoff Marcy, Brenda Matthews, James McBride, Ian McLean, StanimirMetchev, 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, RemiSoummer, AnandSivaramakrishnan, Sandrine Thomas, Carlos A. Torres, GautamVasisht, Jean-Pierre Veran, Arthur Vigan, Kent Wallace, Sloane Wiktorowicz, & Ben Zuckerman

  20. Target identification

  21. Model planet discoveries (McBride et al 2011)

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

  23. Example: recovery of mass function Dmitry Savransky

  24. Orbital eccentricity measurements Quinn Konopacky

  25. Distinguishing high and low-eccentricity populations

  26. Spectral characterization T=400-800 K

  27. 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

  28. Small-particle phase functions (Graham et al 2007)

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