Michael Fitzgerald University of California, Los Angeles (UCLA), Lecture notes of Chemistry

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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