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TMT High-Contrast
Exoplanet Science
Michael Fitzgerald
University of California, Los Angeles (UCLA)
The Next Decade+
- (^) Demographics
- (^) Kepler has provided rich
census of radius/semimajor-
axis space down to terrestrial
planets
- (^) But at lower mass and larger
separations picture is much
less clear
- (^) Important for formation
(condensation profiles)
- (^) Masses, densities, occurrence
rates
The Next Decade+
- (^) Atmospheric Characterization
- (^) Transmittance, reflectance, and thermal emission
- (^) Low-res IR absorption spectroscopy gives some window to H2O, CH4, CO, CO2, equilibrium chemistry status (though degeneracies exist)
- (^) Low-res visible absorption spectroscopy gives Na, K, TiO, clouds/hazes
- (^) high-resolution spectroscopy allows for more detailed characterization, C/O ratio, rotation, doppler imaging 2.0 2.1 2.2 2. Wavelength (μm)
F λ^ (scaled) H 2 O CH 4 CO HR 8799c Uncertainties Model Spectrum (Teff = 1100 K, log(g) = 4.0) Konopacky et al. (2013)
The Next Decade+
Crossfield+
- (^) Atmospheric Characterization
- (^) Transmittance, reflectance, and thermal emission
- (^) Low-res IR absorption spectroscopy gives some window to H2O, CH4, CO, CO2, equilibrium chemistry status (though degeneracies exist)
- (^) Low-res visible absorption spectroscopy gives Na, K, TiO, clouds/hazes
- (^) high-resolution spectroscopy allows for more detailed characterization, C/O ratio, rotation, doppler imaging
More Characterization
- (^) Direct imaging results
- (^) Thermal emission spectroscopy of young giants
- (^) Comparisons with brown dwarfs 3 10 30 100 300 1000 3000 AU HR#8799# β#Pic# GSC#06214# RXJ#1609# AB#Pic#^ WD#0806# Jupiter# 51#Eri# RV & transits direct imaging M. Liu
The Next Decade+
- (^) Formation Pathways C. Mordasini
The Next Decade+
- (^) Formation Pathways
- (^) Orbital dynamics
- (^) Chemistry gradients H 2 O! snowline! (~140 K) CO 2! snowline! (~50 K) CO! snowline (~20 K) Oberg+
Astrometry with GAIA
- (^) GAIA expects to find >>10,000 Jupiters orbiting
FGKM and WDs <100 pc, many with orbits
- (^) ~2,600 detections of Jupiter mass planets incl. ~
accurate orbits (assuming η
Jup
~3% from RV)
(^) Some detectable with ELTs @ 10
contrast
- Astrometric trends from 1-70 M Jup
companions. BDs
detectable with current ExAO
Sozzetti et al 2015, 2015arXiv150203575S
0.8M⊙ at 300 pc 0.2M⊙ at 30 pc 0.05M⊙ at 2 pc GAIA 2.5 and 5 yr limits
JWST
- (^) transit spectroscopy of short- period planets
- (^) high-contrast imaging of self- luminous planets at larger separations
- (^) limited low-resolution spectroscopy ! !
JWST%Transits% JWST%Imaging%%
&%Spectroscopy%
WFIRST-AFTA
- (^) >
- (^) Visible light
- (^) R~70 spectroscopy
- (^) Inner working angle 0.2”
- (^) Discovery and characterization of nearby giant planets, several Neptunes W. Traub
Long-Term Complementarity
- (^) e.g. HabEx, LUVOIR
- (^) Deeper contrast, reflected-light terrestrial exoplanets at visible wavelengths
- (^) (Perhaps) longer term than first wave of TMT 2nd- generation instrumentation
- (^) Smaller aperture than TMT (larger inner-working angle)
Early ELT Instruments
- (^) For TMT/NFIRAOS/IRIS
- (^) Moderate contrast, moderate spectral resolution, 0.8-2.5 μm
- (^) 3x10-6^ contrast at 400 mas, R=4,000-8,000 (no coronagraph)
- (^) Comparable to GPI, but higher spectral resolution Keck 30s Keck 1h IRIS 1min IRIS 1min ADI IRIS 2h ADI GPI 1h R~ Beta Pic b HR 8799d HR 8799c HR 8799e IRIS vs a GPI simulated survey (600 stars, 5 GPI simulated exoplanet sample by D. Savransky R s NFIRAOS control radius 51 Eri b HD95086 b
- All currently known DI exoplanets are outside IRIS well samp
- And outside NFIRAOS’ control radius (no dark hole to bette IRIS On-axis FOV GPI methane C. Marois
Where can TMT make
an impact?
Reflected Light
Planets within 30 pc
0.001 0.010 0.100 1.000 10. Separation (arcsec) 10
10
10
10
10
10
Contrast Giant planets Rocky planets Water/ice planets Known Doppler planets Macintosh & Savransky Kepler-consistent RF; 1.9 pl/star Main sequence non binary stars
- (^) Detection and Characterization
- (^) Enabled by angular resolution and inner-working angle
- (^) Opportunity for first reflectance spectroscopy of Super-Earths in NIR
- (^) Opportunity for first reflectance spectroscopy of cooler Earth-size planets