Gemini Planet Imager from presentations provided by James Graham and Marshall Perrin
Outline Ojectives The instrument Three examples of observations The GPI Exoplanet Survey 2
Objectives Radial velocity Transits Micro-lensing Timing Direct imaging 3
Objectives 1/ Statistics for planet frequency at large separations accretion vs gravitational instability 2/ Atmosphere characterization from spectra Radial velocity Transits Micro-lensing Timing Direct imaging 4
GPI main characteristics Near-IR: 1.2 to 4 μm Cassegrain instrument at Gemini South High order MEMS-based AO system - 64x64 BMC DM - spatially filtered SH WFS Achromatic apodized pupil Lyot coronagraph Integral field imaging/polarimeter Available pipeline for easy data reduction 5
GPI timeline 2006 Official GPI project kickoff 2007-2012 Tech development + subsystem assembly 2012-2013 Integration&Test at UC Santa Cruz 2013 Aug. South Transport to Gemini South 2013 Nov. First light 2014 Jan. AAS GPI first light press release 2013 Dec. - 2014 Sept. Verification&Commissioning 2014 Nov. Start of full science operations 6
GPI verification & commissioning All science modes commissioned Instrument offered for early science and queue 18% of Gemini South for 2015A: 350h (GPIES=200h) Pipeline generates science-quality data see website 8 peer-reviewed science papers in 2014 βpic spectra & orbit, HR 8799 spectra, HR 4796 disk and companions of HR 95086, HD 162142, HD 43527 7
GPI at Gemini South 8
Raw data Spectra R=30-80 9
Spectral data cube Numerical simulation Planets 10
Outline The instrument Three examples of observations The GPI Exoplanet Survey 11
HD 95086 during GPI SVT Star residuals Planet HD 95086 b 5+/-2MJup at 56 AU Rameau et al 2013 Direct image at L' GPI SVT observations K1 and H ~40min of integration Planets 12
HD 95086 1st detections at H and K bands high content of photospheric dust / reduced surface gravity Galicher et al 2014 13
HR 8799 b (outside the field of view) K1/K2 bands 2013 Nov 17/18 Non optimal conditions 14
HR 8799 Different spectral shapes and slopes seen from 1.9-2.2 µm, despite similar overall brightness and broadband colors. Deeper water absorption bands near 1.4 and 1.9 µm for planet c Confirms tentative earlier result at lower S/N from Palomar Project 1640 (Oppenheimer et al. 2013) Possibly sign of uniform cloud cover on planet d vs patchy on c Improved atmosphere modeling needed 15
HR 4796 Perrin et al. 2015 Schneider et al. 2009 N HST E GPI GPI Young (10 Myr) 2 solar mass A star, with well-known dust ring at 75 AU radius (1 arcsec) Observed during commissioning & SVT 2014 March 16
HR 4796 Polarization + total intensity insight into disk composition Silicate dust with relatively large particle size (> 5 µm) total and polarized light => disk must be slightly opaque (optically thick) Implies very narrow and thin geometry 17
Outline The instrument Three examples of observations The GPI Exoplanet Survey 18
GPI Exoplanet Survey (GPIES) 890 hours in total 600 young nearby stars (PI: Macintosh) median target: 45pc, 125Myr Survey initiated Nov. 2014 integrated target database, selection/prioritization algorithms, data access, automated reduction & PSF subtraction (KLIP) and survey coordination Reduced data in real-time 19
GPIES Progress at the end of 2014 ~50 science targets were observed 48h charged in 2014B and 31.4h of open shutter => 65% efficient typical contrast 3e-6 at 0.5 (5σ) GPIES Target s Observed 20
Model discrimination Number of detected planets is a strong function of planet formation pathway Prediction for GPIES: 25 vs 35 21
Conclusions GPI All science modes commissioned Instrument offered for early science and queue 18% of Gemini South for 2015A: 350h (GPIES=200h) 1st results from Com and SVT HD 95086 b 1st detection at H and K, HR 8799 c and d spectra, HR 4796 disk, Beta Pic b, etc GPIES 890 hours in total, 600 young nearby stars (PI: Macintosh) initiated in Nov. 2014 new science to discover from GPI and SPHERE! 22
HD 95086 HR 4796 HR 4796 N HR 8799 E Thank you Beta Pictoris 23