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Science with EPICS The E-ELT Planet Finder

Science with EPICS The E-ELT Planet Finder. R. Gratton 1 , M. Kasper 2 , C. Verinaud 3 , M. Bonavita 1,4 + EPICS Science team. 1 INAF-Osservatorio Astronomico di Padova 2 ESO 3 LAOG 4 Un. of Toronto. EPICS Phase-A study.

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Science with EPICS The E-ELT Planet Finder

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  1. Science with EPICSThe E-ELT Planet Finder R. Gratton1, M. Kasper2, C. Verinaud3, M. Bonavita1,4 + EPICS Science team 1INAF-Osservatorio Astronomico di Padova 2ESO 3LAOG 4Un. of Toronto IAU Symp. 276, Torino, october 2010

  2. EPICS Phase-A study ESO: Markus Kasper, Emmanuel Aller-Carpentier, Norbert Hubin, FlorianKerber, Natalia Yaitskova, Patrice Martinez, EnricoFedrigo LAOG: Jean-Luc Beuzit, Christophe Verinaud, Visa Korkiaskoski, Patrick Rabou, Jacopo Antichi, Olivier Preis Padova Observatory: Raffaele G. Gratton, MariangelaBonavita, Dino Mesa ASTRON: Lars Venema, Ronald Roelfsema, RieksJager, HiddoHanenburg University of Oxford: Niranjan Thatte, Mattias Tecza, Graeme Salter LESIA: Pierre Baudoz, Anthony Boccaletti NOVA: Christoph Keller ETH Zürich: Hans Martin Schmid FIZEAU: Lyu Abe LAM: Kjetil Dohlen 2 IAU Symp. 276, Torino, october 2010

  3. Concept Top view Nasmyth implementation 3 IAU Symp. 276, Torino, october 2010

  4. Concept • E-ELT: 42 m telescope  λ/D=4.9 mas at 1 μm • Superb XAO and wavefront control • Turbulence residual halo ~10-5 at 30 mas <10-6 close to the AO correction radius • Quasi-static speckles at a similar level than AO residuals through phase-diversity • Excellent temporal stability • All moving or rotating optics are in the common path. • Cover providing thermal inertia and dust protection. • Efficient calibration of PSF residuals • Well behaved and known chromaticity for spectral deconvolution • Small instrumental polarization and efficient calibration for differential polarimetry • => EPICS is photon noise limited 4 IAU Symp. 276, Torino, october 2010

  5. EXPECTED PERFORMANCES Y (arcsec) Y (arcsec) Separation (arcsec) IAU Symp. 276, Torino, october 2010 X (arcsec)

  6. Three Driving Science Cases • Young self-luminous gas planets in star forming regions and young associations • Mature planets in the solar neighbourhood • Giant planets • Neptune-like & Rocky Planets • Planets discovered by RV, astrometry and transit searches IAU Symp. 276, Torino, october 2010

  7. Young self-luminous gas planets in star forming regions and young associations • Determine the initial frequency and distribution with mass and separation of giant planets • This will allow extensive comparisons with models of planetary system formation and evolution IAU Symp. 276, Torino, october 2010

  8. Limiting detectable mass of planets as a function of physical separation around a 10 Myr oldG2V star at a distance 120 pc Uranus Neptune IAU Symp. 276, Torino, october 2010

  9. Mature planets in the solar neighbourhood • Frequency and mass distribution of giant planets at old ages, once dynamic evolution have cleaned systems from planets in unstable orbits, can be compared with the results obtained in star forming regions and young associations • Systems may be studied in regions much closer to the central star with respect to the snow line, allowing exploring the HZ and even inner regions • These observations are important forerunner for spatial missions for spectroscopy of Earth-like planets, clarifying which systems are most likely to host rocky planets in the HZ IAU Symp. 276, Torino, october 2010

  10. The expected frequency of low-mass planets at various separations from the central star is a basic parameter for models of planet formation. Model by Mordasini et al. IAU Symp. 276, Torino, october 2010

  11. Even low resolution and low S/N spectra of such objects would allow a first characterization of their atmosphere. This is extremely important because little is known about the range of possible variations for the atmospheres of low-mass planets, and moreover about the incidence of Earth-like (O2-dominated) atmospheres. IAU Symp. 276, Torino, october 2010

  12. IFS & Pol. Analyzer 1.5m space coronagraphs SPHERE @VLT/GPI@Gemini EPICS-EPOL @E-ELT EPICS-IFS @E-ELT Monte Carlo simulations using MESS by M. Bonavita IAU Symp. 276, Torino, october 2010

  13. IFS E-POL (Simu’s made using MESS By MBo) IAU Symp. 276, Torino, october 2010

  14. Planets discovered by RV, astrometry and transit searches • Breakthrough: • planet masses and even radii (transits) • stellar ages are (isochrones, magnetic activity and rotation, kinematics, etc.). • ideal benchmarks for the calibration of models for sub-stellar objects. IAU Symp. 276, Torino, october 2010

  15. RV Planets in the separation-contrast plane (J-band) Gl581d IAU Symp. 276, Torino, october 2010

  16. RV signal of detectable planets ~2012 (Simu’s made using MESS By MBo) IAU Symp. 276, Torino, october 2010

  17. RV signal of detectable planets ~2014 (Simu’s made using MESS By MBo) IAU Symp. 276, Torino, october 2010

  18. RV signal of detectable planets ~2020 (Simu’s made using MESS By MBo) IAU Symp. 276, Torino, october 2010

  19. RV signal of detectable planets ~2022 (Simu’s made using MESS By MBo) IAU Symp. 276, Torino, october 2010

  20. SIM Astrometric signal of detectable planets ~2012 (Beichman et al. 2008) (Simu’s made using MESS By MBo) IAU Symp. 276, Torino, october 2010

  21. SIM Astrometric signal of detectable planets ~2014 (Beichman et al. 2008) (Simu’s made using MESS By MBo) IAU Symp. 276, Torino, october 2010

  22. SIM-LITE Astrometric signal of detectable planets ~2020 (Beichman et al. 2008) (Simu’s made using MESS By MBo) IAU Symp. 276, Torino, october 2010

  23. SIM-LITE Astrometric signal of detectable planets ~2022 (Beichman et al. 2008) (Simu’s made using MESS By MBo) IAU Symp. 276, Torino, october 2010

  24. SIM-LITE Astrometric signal of detectable planets ~2020 (Beichman et al. 2008) (Simu’s made using MESS By MBo) IAU Symp. 276, Torino, october 2010

  25. Synergy 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 HZ 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 (Simu’s made using MESS By MBo) IAU Symp. 276, Torino, october 2010

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