TMT High-Contrast Exoplanet Science. Michael Fitzgerald University of California, Los Angeles (UCLA)

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1 TMT High-Contrast Exoplanet Science Michael Fitzgerald University of California, Los Angeles (UCLA)

2 The Next Decade+ Demographics Kepler has provided rich census of radius/semimajoraxis 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

3 The Next Decade+ Atmospheric Characterization Transmittance, reflectance, and thermal emission HR 8799c 1100 K young giant planet CO + trace? CH 4 Low-res IR absorption spectroscopy gives some window to H2O, CH4, CO, CO2, equilibrium chemistry status (though degeneracies exist) Mg-silicates CO Low-res visible absorption spectroscopy gives Na, K, TiO, clouds/hazes Iron metal liquid high-resolution spectroscopy allows for more detailed characterization, C/O ratio, rotation, doppler imaging Perovskite CO Corundum Mixing Marley (2013)

4 The Next Decade+ Atmospheric Characterization Transmittance, reflectance, and thermal emission H 2 O CH 4 CO 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 F λ (scaled) high-resolution spectroscopy allows for more detailed characterization, C/O ratio, rotation, doppler imaging 0.0 HR 8799c Uncertainties Model Spectrum (Teff = 1100 K, log(g) = 4.0) Konopacky et al. (2013) Wavelength (µm)

5 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 Crossfield+14

6 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 Snellen+14

7 M. Liu More Characterization Direct imaging results Thermal emission spectroscopy of young giants Comparisons with brown dwarfs RXJ#1609# HR#8799# β#pic# AB#Pic# GSC#06214# WD#0806# 51#Eri# Jupiter# AU RV & transits direct imaging

8 The Next Decade+ Formation Pathways C. Mordasini

9 The Next Decade+ Formation Pathways Orbital dynamics Chemistry gradients Mordasini, Alibert, Benz (2009)

10 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+11

11 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. ~500 accurate orbits (assuming η Jup ~3% from RV) Some detectable with 10-8 contrast Astrometric trends from 1-70 M Jup companions. BDs detectable with current ExAO 0.8M at 300 pc 0.2M at 30 pc 0.05M at 2 pc Sozzetti et al 2015, 2015arXiv S GAIA 2.5 and 5 yr limits

12 TESS >2017 All-sky transit mission More exoplanet demographics Will detect a few super-earths in 100-day orbits around nearby stars Ricker et al.

13 JWST transit spectroscopy of shortperiod planets high-contrast imaging of selfluminous planets at larger separations limited low-resolution spectroscopy JWST%Transits% JWST%Imaging%% &%Spectroscopy%!!

14 WFIRST-AFTA >2024 Visible light R~70 spectroscopy Inner working angle 0.2 Discovery and characterization of nearby giant planets, several Neptunes W. Traub

15 Completing the Exoplanet Census. WFIRST-AFTA Together, Kepler and WFIRST complete the statistical census of planetary systems in the Galaxy. Microlensing survey ~2600 detections. Some sensitivity to outer Galactic bulge monitoring habitable zone planets. Sensitive to analogs of all Detection and the solar systems planets demographics except Mercury. Hundreds of free-floating Characterize planets.mass function the majority for >1 MECharacterize at a>1 AU to of host systems. better than 10%/dex Galactic distribution of planets. Expected Sensitive lunar-mass 2,800todetections satellites. With 300 ~1 ME planets But no spectroscopy (Penny et al. in prep)

16 Long-Term Complementarity e.g. HabEx, LUVOIR Deeper contrast, reflected-light terrestrial exoplanets at visible wavelengths (Perhaps) longer term than first wave of TMT 2ndgeneration instrumentation Smaller aperture than TMT (larger inner-working angle)

17 Early ELT Instruments For TMT/NFIRAOS/IRIS NFIRAOS control radius Moderate contrast, moderate spectral resolution, µm 3x10-6 contrast at 400 mas, R=4,000-8,000 (no coronagraph) Comparable to GPI, but higher spectral resolution IRIS On-axis FOV IRIS 1min HR 8799e Beta Pic b 51 Eri b GPI methane HR 8799d HD95086 b Keck 30s IRIS 1min ADI HR 8799c Keck 1h IRIS 2h ADI GPI 1h R~40 C. Marois GPI simulated exoplanet sample by D. Savransky

18 Early ELT Instruments For E-ELT/METIS Also a first-light instrument 3-19 µm coronagraphy 3-5 µm IFS characterizing luminosity, equilibrium temperature complementary to scattered-light imaging Quanz+14

19 Where can TMT make an impact?

20 Reflected Light 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 10-6 Planets within 30 pc Giant planets Rocky planets Water/ice planets Known Doppler planets 10-7 Contrast Macintosh & Savransky Separation (arcsec) Kepler-consistent RF; 1.9 pl/star Main sequence non binary stars

21 Reflected Light Detection and Characterization Known RV planets 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 Fig. 2. Known RV planets potentially accessible to highcontrast observations in reflected light. Data Crossfield are taken (2016) from the NASA Exoplanet Archive. The only assumptions are an albedo of 0.1, R p /R =(M p /M ) 0.485,andtheradiiofallplanetswith R P /R J > 1.8 andm p /M J > 1.8 setto1.2r J.Thesolidlineisthe approximate NIR contrast performance predicted for ELT instruments, and the color scale indicates T e. The accessible systems

22 Reflected Light Detection and Characterization Hypothetical rocky HZ planets 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 Fig. 3. Accessibility of hypothetical temperate, rocky planets to NIR-contrast observations in reflected light. Crossfield Each point (2016) represents a 1.25 R planet receiving Earth-like irradiation, with one such planet for each star within 20 pc. The solid line is the approximate NIR contrast performance predicted for ELT instruments. The color scale indicates T e,andpointsizescalesinverselywith distance from Earth. The most accessible temperate planets will

23 Reflected Light 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 Mass of star relative to Sun Star type 0 Radial velocity Transit Microlensing Earth Dry terrestrial planet Radius of orbit relative to Earth s Earth-like planet Hydrogenatmosphere planet INTERNAL HEAT REQUIRED Seager Fig. 2. The habitable zone. The light blue region depicts the conventional habitable zone for planets with N 2 -CO 2 -H 2 Oatmospheres(9, 10). The yellow region shows the habitable zone as extended inward for dry planets (36, 37), as dry as 1% relative humidity (37). The outer darker blue region shows the outer extension of the habitable zone for hydrogen-rich atmospheres (34) andcanextendevenout to free-floating planets with no host star (35). The solar system planets are shown with images. Known exoplanets are shown with symbols [here, planets with a mass or minimum mass less than 10 Earth

24 High Spectral Resolution Detection and detailed characterization With improved R and raw contrast more ability to detect molecular species via cross-correlation down to Earth-size planets O2 and H2O can only be detected with R > 10,000 with the crosscorrelation method at very high levels of raw contrast can detect of CO2 and CH4 at more modest raw contrast of 10-5 characterize variability (rotation, cloud patchiness, moons) courtesy of Ji Wang, Renyu Hu, Dimitri Mawet

25 High Spectral Resolution Detection and detailed characterization With improved R and raw contrast more ability to detect molecular species via cross-correlation down to Earth-size planets O2 and H2O can only be detected with R > 10,000 with the crosscorrelation method at very high levels of raw contrast can detect of CO2 and CH4 at more modest raw contrast of 10-5 characterize variability (rotation, cloud patchiness, moons) courtesy of Ji Wang, Renyu Hu, Dimitri Mawet

26 Technical Challenges 10-8 detection contrast at ~2 λ/d Extremely low wavefront error High-order wavefront corrector Fast sensing Low-noise high-frame-rate sensors Elimination of non-common-path error Sensing in science focal-plane Crossfield (2016)

27 Technical Challenges 10-8 detection contrast at ~2 λ/d Extremely low wavefront error High-order wavefront corrector Fast sensing Low-noise high-frame-rate sensors Elimination of non-common-path error Sensing in science focal-plane Crossfield (2016) Significant challenges, but instruments can address these in the near term

28 ExAO TMT Why consider deploying a precursor? High impact science at first light: habitable planets reflected light spectroscopy around the nearest stars Focusing on a single goal, small number of targets to meet schedule Risk mitigation for 2 nd generation instrument Learn what works what needs fixing (instrument/algorithms AND telescope) Opens up opportunities for a more incremental approach: Test subsystems / components on precursor Develop and validate ON SKY : hardware, algorithms TMT precursor starts NOW on 8m telescope(s) see for example SCExAO approach Extensive testing on 8m telescope(s) + modeling for jump to larger aperture will mitigate risks and avoid lengthy engineering/learning on TMT. Fully characterized instruments + algorithms (& yrs of experience) would be deployed on TMT courtesy of Olivier Guyon

29 Science Along the Way Demographics will be largely characterized, e.g. WFIRST Will also have samples of planets around nearby stars (e.g. GAIA, TESS) Characterization JWST transit spectroscopy of short-period planets (relatively low spectral resolution) Thermal emission spectroscopy of longer-period planets still unique from the ground Post-JWST direct detection of planets around nearby stars in space is done in visible light

30 Science Along the Way Clear advantage is in spectral resolution Atmospheric characterization, rotation vs. age for census of self-luminous giant planets Thermal emission of giant planets will continue to be interesting from now through TMT era Technology continues to press on inner working angle Discovery space in context of condensation profiles

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