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SCIENTIFIC OUTPUT OF SINGLE APERTURE IMAGING OF EXOPLANETS

SCIENTIFIC OUTPUT OF SINGLE APERTURE IMAGING OF EXOPLANETS. Raffaele Gratton, INAF-OAPD, I Anthony Boccaletti, LESIA-OAPM, F Mariangela Bonavita, INAF-OAPD, I Silvano Desidera, INAF-OAPD, I Markus Kasper, ESO, D Florian Kerber, ESO, D . Outline.

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SCIENTIFIC OUTPUT OF SINGLE APERTURE IMAGING OF EXOPLANETS

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  1. SCIENTIFIC OUTPUT OF SINGLE APERTURE IMAGING OF EXOPLANETS Raffaele Gratton, INAF-OAPD, I Anthony Boccaletti, LESIA-OAPM, F Mariangela Bonavita, INAF-OAPD, I Silvano Desidera, INAF-OAPD, I Markus Kasper, ESO, D Florian Kerber, ESO, D Barcelona, September 14, 2009

  2. Outline • Introduction: direct imaging of planets, no longer a dream! • What planets can be observed in the near-mid term • Statistics: • Mass distribution • Orbits and system parameters • Spectroscopy and atmosphere composition • Synergies with other techniques  dynamical masses • Radial velocities • Astrometry • Transits Barcelona, September 14, 2009

  3. No longer a dream ! Detection was made possible because : - smallmass ratios(contrast is lower) - young ages (planet is brighter) - large physical / angular separations Barcelona, September 14, 2009 3

  4. Barcelona, September 14, 2009

  5. Problematic Planets are faint and close …. 109 = 1 milliard 106 = 1 million Reflected light Thermal emission Barcelona, September 14, 2009

  6. Single aperture planet imagers of the next future • Ground based 8m telescopes (2011-) • Hi-Ciao (Subaru) • SPHERE (VLT) • GPI (Gemini) (http://gpi.berkeley.edu/) • JWST (2014-) • <5 μm: NIRCAM/TFI (http://ircamera.as.arizona.edu/nircam/) • >5 μm: MIRI (http://www.roe.ac.uk/ukatc/consortium/miri/index.html) • 1.5 m class space coronagraphs (??) • PECO: Guyon et al. 2008, SPIE, 7010, 70101Y • EPIC: Clampin et al. 2006, SPIE, 6265, 62651B; Lyon et al. 2008, SPIE, 7010, 101045 • ACCESS: Trauger et al. 2008, SPIE, 7010, 701029 • SEE-COAST: http://luth7.obspm.fr/SEE-COAST/SEE-COAST.html • ELT Instruments (>2018-) • NIR: EPICS (E-ELT), PFI (TMT), HRCAM (GMT) • MIR: METIS (E-ELT: Brandl et al. 2008, SPIE ), MIRES (TMT), MIISE (GMT) Barcelona, September 14, 2009

  7. Niches: Contrast, Wavelength, IWA Barcelona, September 14, 2009

  8. Observable planets: methodology - inputs • STELLAR PARAMETERS (MStar (Msun), d (pc), Age (Myr), etc.) from two samples of real stars: • Young sample (Age < 500 Myrs, d<100 pc), ~1200 stars • Nearby sample (d < 20 pc) ~600 stars • PLANET PARAMETERS: • Mpsini (MJ) and P (days) randomly generated using the distributions from Cumming et al. 2008, extrapolated up to periods corresponding to a = 40 AU (for MStar = 1 Msun) and scaled with the stellar mass • 0.0 < e < 0.6 generated following the observed RV distribution • All the orbital elements (including inclination), randomly generated using uniform distributions • MONTE-CARLO SIMULATION TOOL: • MESS (Multi-purpose Exo-planet Simulation System) see Bonavita et al.(2009) in prep. • DETECTION LIMIT CURVES: • Direct Imaging (SPHERE, GPI, EPICS, METIS, JWST, Space Coronagraphs) • Radial velocity (HARPS, EXPRESSO, CODEX)‏ • Astrometry (GAIA)

  9. Observable planets: methodology - outputs • DERIVED PLANET PARAMETERS: • Semi-major axis (AU) and projected separation (arcsec) evaluated assuming Distance and Mass of each star • Radius (RJ) estimated following the approach of Fortney et al. (2007)‏ • Teff (K) estimated using the models by Sudarsky et al. (2001) • Intrinsic luminosity obtained using the models by Baraffe et al. (2003)‏ • Reflected luminosity in visible and NEAR-IR (V, H, K, L Band) obtained scaling the Jupiter luminosity with planet semi-major axis and radius • Reflected luminosity in MID-IR (λC = 11.4 μm) obtained assuming a black body emission at T = Teff and λ= λC • Radial Velocity Semi-amplitude (m/s)‏ • Astrometric Signature (mas)

  10. SYNTHETIC PLANET POPULATION: • 5 planets per star (mass>0.7 MEarth), randomly extracted from a set of 10.000 combinations of planet parameters • CHARACTERISTICS OF DETECTABLE PLANETS • Contrast vs projected separation • Mass vs Semi-major Axis • Radial velocity signal (K(RV)) vs Period • Astrometric Signature vs Period

  11. Planets observable with Sphere and GPI (2011-) Young stars (<5 108 yrs) Nearby stars (<20 pc) • Tens of young giant planets at rather large separations Barcelona, September 14, 2009

  12. Planets observable with JWST-MIRI (2014-) Young stars (<5 108 yrs) Nearby stars (<20 pc) • Tens of young giant planets at large separations • But care of disks! Barcelona, September 14, 2009

  13. Planets observable with E-ELT+EPICS (2020-) Young stars (<5 108 yrs) Nearby stars (<20 pc) • Many giant planets (both young and old) • Tens of Neptune-like planets • A few rocky planets Barcelona, September 14, 2009

  14. Planets observable with ~1.5 m dedicated space telescopes (?-) Young stars (<5 108 yrs) Nearby stars (<20 pc) • Many giant planets (both young and old) • Tens of Neptune-like planets • A few rocky planets Barcelona, September 14, 2009

  15. Planets observable with E-ELT+METIS (2020-) Young stars (<5 108 yrs) Nearby stars (<20 pc) • Many young and a few old giant planets at rather large separations Barcelona, September 14, 2009

  16. CURRENT STATUS Nearby stars (<20 pc) Mass/semimajor axis distribution of detectable planets: Present Barcelona, September 14, 2009

  17. Mass/semimajor axis distribution of detectable planets: 2011- Young stars (<5 108 yrs) Nearby stars (<20 pc) Barcelona, September 14, 2009

  18. Mass/semimajor axis distribution of detectable planets: 2014- Young stars (<108 yrs) Nearby stars (<20 pc) Barcelona, September 14, 2009

  19. Mass/semimajor axis distribution of detectable planets: >2018- Young stars (<5 108 yrs) Nearby stars (<20 pc) Barcelona, September 14, 2009

  20. Mass/semimajor axis distribution of detectable planets: ?? Young stars (<5 108 yrs) Nearby stars (<20 pc) Barcelona, September 14, 2009

  21. Mass/semimajor axis distribution of detectable planets: >2018 Young stars (<5 108 yrs) Nearby stars (<20 pc) Barcelona, September 14, 2009

  22. Planets in the habitable zone: 2011-2018 Barcelona, September 14, 2009

  23. Planets in the habitable zone: >2018 Barcelona, September 14, 2009

  24. Planets in the habitable zone: >2018 Barcelona, September 14, 2009

  25. Summary Barcelona, September 14, 2009

  26. Atmospheric composition Barcelona, September 14, 2009

  27. Visible: Space Coronagraphs H3+ C2H2 PH3 H2S C0 02 03 NH3 C02 CH4 H20 Wavelength (μm) Barcelona, September 14, 2009

  28. NIR: Sphere, GPI, NIRCAM, EPICS H3+ C2H2 PH3 H2S C0 02 03 NH3 C02 CH4 H20 Wavelength (μm) Barcelona, September 14, 2009

  29. MIR: MIRI, METIS H3+ C2H2 PH3 H2S C0 02 03 NH3 C02 CH4 H20 Wavelength (μm) Barcelona, September 14, 2009

  30. 0.5-30 mm spectrum of an isolated 2 MJ planet (Burrows et al.2003, ApJ 596, 587) vs Visible (Space Coronagraphs)

  31. 0.5-30 mm spectrum of an isolated 2 MJ planet (Burrows et al.2003, ApJ 596, 587) vs NIR (Sphere, GPI, NIRCAM, EPICS)

  32. 0.5-30 mm spectrum of an isolated 2 MJ planet (Burrows et al.2003, ApJ 596, 587) vs MIR (MIRI, METIS)

  33. Spectroscopic characterization • Spectra at higher resolution than in standard set-up for planet detection will allow a more detailed characterization (for planets detected with high enough S/N) • Some science goals: identification of spectral features, determination of physical parameters (temperature, gravity, chemical composition), cloud process and their variation with time (e.g. for planets in eccentric orbits) • R=3000, R=20000 considered See Poster by Claudi et al. Barcelona, September 14, 2009

  34. Medium resolution Barcelona, September 14, 2009 McLean+2007

  35. High resolution (R=20000) R=20000 J band spectrum of a T4.5 BD (Mc Lean+2007), many spectral lines available Identified H2O lines marked Barcelona, September 14, 2009

  36. Planet radial velocity • Earth semi-amplitude: 30 km/s • Useful to constrain the planetary orbit if only visual measurements available, planet-star mass ratio even based on small time baseline • Detection of binary planets, if any • Several lines at high resolution, resolved sky lines to be used as wavelength reference. Barcelona, September 14, 2009

  37. Planet rotational velocity • Jupiter: Vrot:12.6 km/s, Saturn: 9.9 km/s, Neptune: 2.7 km/s • Field T dwarfs typically rotate faster (30-50 km/s: McLean et al., Zapaterio Osorio et al.) • R=20,000 corresponds to FWHM=15 km/s, R=3000 to 100 km/s • Possibility of measuring rotational velocity similar to that of Jupiter • Very interesting if coupled with photometric rotational modulation ( Planet radius independent of luminosity; inclination of rotational axis over orbital plane) Barcelona, September 14, 2009

  38. Number of targets for EPICS Estimate of the number and type of accessible targets using Monte Carlo simulation (R=3000, R=20000) R=3,000 hundreds R=20,000 tens Barcelona, September 14, 2009

  39. Synergies with radial velocitiesPlanets already discovered from RVs Very important: planet mass independent of model assumptions! Barcelona, September 14, 2009

  40. Synergies with radial velocitiesPlanets already discovered from RVs Very important: planet mass independent of model assumptions! Barcelona, September 14, 2009

  41. RV signal of detectable planets Barcelona, September 14, 2009

  42. RV signal of detectable planets Barcelona, September 14, 2009

  43. RV signal of detectable planets Barcelona, September 14, 2009

  44. RV signal of detectable planets Barcelona, September 14, 2009

  45. SIM Astrometric signal of detectable planets (Beichman et al. 2008) Barcelona, September 14, 2009

  46. SIM Astrometric signal of detectable planets (Beichman et al. 2008) Barcelona, September 14, 2009

  47. SIM Astrometric signal of detectable planets (Beichman et al. 2008) Barcelona, September 14, 2009

  48. SIM Astrometric signal of detectable planets (Beichman et al. 2008) Barcelona, September 14, 2009

  49. Potential overlap with PLATO • PLATO: ESA Cosmic Vison proposed mission for the search of transiting planets • Planets down to about 10 MEarth around K and M dwarfs with V=8.5-10 (bright end of PLATO) can be detected also with EPICS • For K dwarfs, planets in the habitable zone are detectable • Availability of planet spectrum from EPICS and planet radius from PLATO will be relevant for the physical study of the planets. • For G and F stars (and K and M dwarfs as well) planets at separation larger than that accessible to PLATO can be detected, allowing to study the outer planetary system of PLATO targets See talk by Claudi et al. Barcelona, September 14, 2009

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