DIRECT PLANET DETECTION

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1 DIRECT PLANET DETECTION James R. Graham (UCB) Bruce Macintosh (LLNL) & Mitchell Troy (JPL) 1

2 High Contrast Imaging? Broad new frontier enabled by large telescopes & AO Exoplanet detection Direct methods explore beyond 5 AU Direct detection is fast compared to Fourier-based methods Photometry & spectroscopy Indirect methods give only a, M sin i, & e Luminosity, temperature, gravity, & chemical composition Circumstellar disks Structure of proto-planetary & debris disks Fundamental stellar astrophysics Large mass range main sequence binaries Brown dwarf & white dwarf companions Mass transfer, mass loss, & stellar evolution Cataclysmic variables, symbiotic stars & supergiants Solar system: Jovian/Saturnian moons, asteroids 2

3 Direct Detection of Planets Voyager family portrait illustrates the impact of imaging Even in in situ observations of scattered sunlight presents a challenge to planet imaging Our solar system data remains central in testing planet formation theory 3

4 Why High Contrast on GSMT? Contrast Contours Better angular resolution λ/d = 11 H band 1.5 AU at Taurus! Improved astrometry Better contrast For a given wavefront error budget (fixed spatial bandwidth) contrast improves as D 2 GSMT can t lock on fainter guide stars without sacrificing contrast More collecting area Increase spectral resolution by x10 at fixed SNR RMS wavefront error (nm) HST Gemini GPI TPF-C? D tel [m] TMT PFI Jovian reflected light θ 2 = 1.0 arc sec θ 1 = 0.1 arc sec 4

5 Doppler Exoplanets Doppler surveys have cataloged 271 planets Indirect searches are limited by Kepler s third law: a = P 2/3 P Jupiter = 11 years P Neptune = 165 years Exo-Jupiter analogs at 5 AU remain undetected A survey beyond 10 AU (P > 31.6 yr) is impractical using indirect methods 5

6 Doppler Exoplanets Only 5% of stars have known Doppler planets Why isn t it 15 50%? A diversity of exoplanets 20% of the Solar System s orbital phase space explored Is the Solar System typical? Do A & early F stars have planets? What about M dwarfs? How do planets form? Core accretion vs. gravitational collapse New questions What is the origin of dynamical diversity? 6

7 Planetary System Architecture Fast alternative to Doppler Improved statistics for flat dn/dlog(a) 4 40 AU vs AU Search for exoplanets at large semimajor axis Is the solar system is unique? Sample beyond the snow line Measure planet forming efficiency vs. stellar mass Reveal if gravitational instability forms planets ( AU) Uncover traces of planetary migration Resolve M sin i ambiguity Q min = yr 350 yr Q min =1.4? 20 AU Mayer et al M1207b 7

8 Detection of Doppler Planets? Median contrast & angular separation for current catalog of Doppler planets Q = 2 x 10-8 Δθ = 30 mas 3λ/D = 33 H GSMT with highperformance diffraction suppression can detect Doppler planets Known Doppler Planets 30-m 3λ/D Median Gemini 3λ/D 8

9 Exoplanet Atmospheres Exoplanets occupy a unique location in (log g, T eff ) phase space T dwarfs Over 5 Gyr a Jovian-mass exoplanet traverses the H 2 O & NH 3 condensation tracks Last frontier of classical stellar atmospheres NH 3 log 10 (g) [cm s-2 ] Jupiter Graham et al. arxiv: Galileo T eff [K] 9

10 Planetary Composition Composition is destiny The zero-temperature equilibrium radius is determined by composition Composition is a primary window on planet formation Order of magnitude range in solar system abundances, e.g., C ranges from x 3 in Jupiter to x 30 in Uranus & Neptune Jovian abundances rule out formation by gravitational collapse Jupiter results agree with gravity/eos 10 Zapolsky & Salpeter 1965

11 Planetary Spectroscopy Doppler searches only give P, K, & e, hence a and M sini Direct detection gives access to the planetary atmosphere First order information regarding luminosity, T eff, and log(g) Major trace species (CNO) are revealed via the near-ir opacity of H 2 O, CH 4 & NH 3 In reflected light the depth of a molecular absorption band also depends on the column of absorbers above any scattering (cloud) layer 1 M J Fortney & Marley

12 Detection of Cooling Planets Contrast required detect a exo-jupiter in a 5 AU orbit is about 2 x 10-9 in the visible Near-IR contrast is 2-3 orders of magnitude more favorable Radiation escapes in gaps in the CH 4 and H 2 O opacity at Y, J, H, & K J H K Burrows Sudarsky & Hubeny 2004 ApJ

13 PFI/TMT Phase Space T dwarfs PFI Jupiter GPI 13

14 Young Planets Young, nearby stars with forming planetary systems are rare Need GSMT to to reach ρ Oph, Taurus, or Upper Sco d = 150 pc 5 AU/150 pc = 33 mas Name Age (Myr) TW Hya 8 β Pic 8 Tuc/Hor 30 Local Assoc. 60 AB Dor 70 Debris Disks Stars Total Dist. Approx. (pc) No < Gould s belt

15 Planets as Cooling Polytropes log (L/L ) Planets 50% Li burned 50% D burned L ~ t -2/3 Brown dwarfs Stars Burrows et al ApJ log (age/gyr) 15

16 Early Thermal History Early formation events (1), (2), & (3) have distinctive radiative fingerprints Potentially observable Significant early discrepancies with polytropic solution Memory of formation events persists longer for more massive planets Convergence with cooling tracks only at late time (>100 Myr) ) Accretion of solids 2 M J 2) Hydrodynamic (gas) accretion 3) Runaway gas accretion Fortney et al. 2008, arxiv

17 Thermal Evolution Reveals History The luminosity history of exoplanets may be punctuated by giant impacts Ejection of Mercury's mantle, the formation of the Earth- Moon system, Pluto-Charon system, the obliquities of Uranus & Saturn A giant impact by an earthmass projectile deposits (M/1 M )(v/50 km s -1 ) 2 erg in the target Radiated away over a KH timescale Anic et al. (2007). 17

18 Targets in Star Forming Clouds Star forming regions like Taurus, ρ Ophiuchus or Upper Sco have large numbers of young stars All at d ~ 150 pc Only GSMT can reach these NICI 18

19 Debris Disks Gravitationally sculpted disks provide key evidence for exoplanets Morphology of dust trapped in libration points provides key to masses an eccentricities of exoplanets Surface brightness,color, phase function, and polarization indicates quantity composition and grain size distribution Synergy with JWST, Herschel, & ALMA Probe disjoint dust grain populations and constraints the particle size distribution 19 HD µm Gemini/Michelle 1.6 µm Keck AO 1 mm CARMA Maness, Kalas & Graham 2008

20 Planets in Dusty Disks T Tauri star (150 pc) with a ΔH = 10 mag. companion in an optically thick disk (i = 66 o ) M = 3 M J, t = 10 Myr 20

21 Science Highlights GSMT enables a broad range of planet detection & characterization Young planets in circumstellar disks Self-luminous planets at large semimajor axis separations Old, cold Doppler planets (< 5 AU) which shine by reflected light Reveal the earliest steps in planet formation Detect accretion events as planets emerging from circumstellar disks Deliver a uniform census of planetary populations Sample self-luminous and reflected light Jupiters Develop and refine spectroscopic techniques for characterizing atmospheric conditions & composition 21

22 22

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