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IAU Symp. 276, Torino, october 2010 R. Gratton 1, M. Kasper 2, C. Verinaud 3, M. Bonavita 1,4 + EPICS Science team Science with EPICS The E-ELT Planet.

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Presentation on theme: "IAU Symp. 276, Torino, october 2010 R. Gratton 1, M. Kasper 2, C. Verinaud 3, M. Bonavita 1,4 + EPICS Science team Science with EPICS The E-ELT Planet."— Presentation transcript:

1 IAU Symp. 276, Torino, october 2010 R. Gratton 1, M. Kasper 2, C. Verinaud 3, M. Bonavita 1,4 + EPICS Science team Science with EPICS The E-ELT Planet Finder 1 INAF-Osservatorio Astronomico di Padova 2 ESO 3 LAOG 4 Un. of Toronto

2 IAU Symp. 276, Torino, october 2010 EPICS Phase-A study 2 ESO: Markus Kasper, Emmanuel Aller-Carpentier, Norbert Hubin, Florian Kerber, Natalia Yaitskova, Patrice Martinez, Enrico Fedrigo LAOG: Jean-Luc Beuzit, Christophe Verinaud, Visa Korkiaskoski, Patrick Rabou, Jacopo Antichi, Olivier Preis Padova Observatory: Raffaele G. Gratton, Mariangela Bonavita, Dino Mesa ASTRON: Lars Venema, Ronald Roelfsema, Rieks Jager, Hiddo Hanenburg 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

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

4 IAU Symp. 276, Torino, october 2010 Concept 4 1.E-ELT: 42 m telescope  λ/D=4.9 mas at 1 μm 2.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 2.Excellent temporal stability All moving or rotating optics are in the common path. Cover providing thermal inertia and dust protection. 3.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

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

6 IAU Symp. 276, Torino, october 2010 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

7 IAU Symp. 276, Torino, october 2010 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

8 IAU Symp. 276, Torino, october 2010 Limiting detectable mass of planets as a function of physical separation around a 10 Myr old G2V star at a distance 120 pc UranusNeptune

9 IAU Symp. 276, Torino, october 2010 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

10 IAU Symp. 276, Torino, october 2010 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.

11 IAU Symp. 276, Torino, october 2010 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 (O 2 -dominated) atmospheres.

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

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

14 IAU Symp. 276, Torino, october 2010 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.

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

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

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

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

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

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

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

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

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

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

25 IAU Symp. 276, Torino, october 2010 PLATO: ESA Cosmic Vison proposed mission for the search of transiting planets Planets down to about 10 M Earth 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 Synergy with PLATO (Simu’s made using MESS By MBo)


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