1. SEARCHING FOR PLANETS IN THE HABITABLE ZONE. FROM COROT TO PLATO Ennio Poretti – INAF OAB

2. 51 Pegasi : Discovered by Mayor & Queloz (1995, Nature 378, 355) The first extrasolar planet Wolszczan & Frail, 1992, Nature 355, 145

3. RADIAL VELOCITY 635 detections

4. TIMING METHOD: periodic deviations from a given ephemeris. The case of the pulsar PSR1257+12 (10 detections)

5. MICROLENSING (12 detections)

6. ASTROMETRY (waiting for GAIA, used in KEPLER data)

7. Fomalhaut b : Hubble images taken 2 years apart (Kalas et al.2008) DIRECT IMAGING (15 detections)

8. THE TRANSIT METHOD Planetary mass Density Inclination Orbital distance Planetary radius Using Doppler data too: Angle between orbital plane and equatorial plane(Rossiter effect) INFRARED: Ellipticity Photons from planet Spectroscopy during the transit:

10. 0 E2 CCD A1CCD E1 CCD E2 CCD A2 0 E1 0 A1 0 A2 3.05° 2.70° Asteroseismology Bright stars 5.5 < V < 9.5 2x5  in each field Exoplanetary search Faint stars 11.0 < V < 16.5 2x6000  in each field Mission life extended to 2012 5 long runs (150 d each or 2x80d) 10 short runs (20 - 30 d) V = 6 --> ~2.5 10 4 photons cm -2 s –1 outside atmosphere, T ~ 6000°K mv = 16 --> ~2.5 photons cm -2 s -1 CoRoT

11. COROT, 30 cm mirror V> 12, raw data CoRoT 1b HUBBLE, 2.5m mirror, V=7.8, published curve HD 209458

12. RESULTS Mandel & Agol formalism Limb-darkening quadratic law(Claret) Using R S = 1.11±0.05 R  R P /R S = 0.1350±0.0018R P = 1.46±0.07 R G R P = 1.45±0.07 R G R P = 1.44±0.07 R G R P /R S = 0.1349±0.0015 R P /R S = 0.1332±0.0008 R P /R S = 0.1334±0.0016 a/R S = 4.89±0.06 sin i = 0.996±0.001 t c = 2593.3263±0.0008 White light curve Coloured light curves COROT 1b Laurea Thesis Francesco Borsa

13. CoRoT 3b: the link between stars and planets Different depths of the transit R S = 1.56±0.09 R  R P = 0.78±0.07 R G R P = 0.98±0.06 R G Stellar object !! R P /R S = 0.0608±0.0006 a/R S = 7.90±0.18 sin i= 0.998±0.001 t c = 2695.5700±0.0012 P = 4.25695±0.00009d M = 21.7±1 M J Deuterium burning Laurea Thesis Francesco Borsa

14. LINE PROFILE VARIATIONS BY USING HARPS The fingerprint of the nonradial pulsations

15. V1127 Aql: the full Blazhko effect

16. Line profile variations allow us : -To separate radial modes from nonradial modes -To broke the degeneracy in m due to the rotational splitting Mean line profile (top) and standard deviation across the line profile (in red after removing 20 frequencies) HD 50870

17. MODE IDENTIFICATION HD 50844 ( l, m couples) Inclination angle: 82°

19. 19 Power spectrum of light curve gives frequencies Asteroseismology Inversions + model fitting +  consistent , M, , J, age : Large separations    M/R 3  density Small separations d 02  probe the core  age Uncertainty in Age ~ 10% Uncertainty in Mass ~ 2% Asteroseismic age of the Sun: 4.68 +/- 0.02 Gys (Houdek & Gough, 2007)

20. N. Batalha et al. [2011 Jan 10]

21. N. Batalha, et al. [2010 Jan 11]

24. Jupiter, Saturn, Uranus, Neptune and icy-rocky trans-neptunian bodies Interaction between giant planets and external bodies. Increase of the angular moments of the giant planets. INSTABILITY: Jupiter and Saturn in 2:1 resonance. Giant planets shifted outward

25. 25Insert footer25 PLATO PLAnetary Transits and Oscillations of Stars The exoplanetary system explorer

26. Main objective: - detect and characterize exoplanets of all kinds around stars of all types and all ages  full statistical study of formation and evolution of exoplanetary systems - including telluric planets in the habitable zone of their host stars Three complementary techniques: - photometric transits : R p /R s (R s known thanks to Gaia) - groundbased follow-up in radial velocity : M p /M s - seismic analysis of host-stars (stellar oscillations) : R s, M s, age > measurement of radius and mass, hence of planet mean density > measurement of age of host stars, hence of planetary systems Tool: - ultra-high precision, long, uninterrupted, CCD photometric monitoring of very large samples of bright stars: CoRoT - Kepler heritage - bright stars: efficient groundbased follow-up and capability of seismic analysis PLATO Science Objectives

27. Instrumental Concept - 32 « normal » cameras : cadence 25 sec - 2 « fast » cameras : cadence 2.5 sec, 2 colours - pupil 120 mm - dynamical range: 4 ≤ m V ≤ 16 optical field 37° 4 CCDs: 4510 2 18  m « normal » « fast » focal planes fully dioptric, 6 lenses + 1 window Very wide field + large collecting area : multi-instrument approach optical design On board data treatment: 1 DPU /2 cameras + 1 ICU Science ground segment Orbit around L2 Lagrangian point, 6+2 year lifetime

28. Concept of overlapping line of sight 4 groups of 8 cameras with offset lines of sight offset = 0.35 x field diameter 8 8 8 8 16 24 32 Optimization of number of stars at given noise level AND of number of stars at given magnitude 37° 50°

29. CoRoT Kepler PLATO Basic observation strategy very wide field + 2 successive long monitoring phases:

30. Kepler PLATO 25% of the whole sky ! CoRoT step and stare phase (1 year) : N fields for 3-5 months each - increase sky coverage - potential to re-visit interesting targets - explore various stellar environments Basic observation strategy

31. PLATO Kepler CoRoT step and stare phase (2 years) : N fields for 3-5 months each - increase sky coverage - potential to re-visit interesting targets - explore various stellar environments 42% of the whole sky ! Basic observation strategy

32. 32 The Discovery Space Transit RV μlensing PLATO

33. 33 Planet population predictions Small planets expected to be very common and PLATO could monitor the 42% of the sky ! Observations Population Synthesis ?

34. monitor in ultra-high precision photometry a very large number of bright and very bright stars The PLATO challenge

35. CoRoT Plato (2018) Kepler THE FUTURE OF ASTEROSEISMOLOGY AND SEARCH OF “EARTHS” E-ELT (2017) Combination of different techniques, from ground and space Spectroscopy Photometry HARPS, HARPS-N ESPRESSO, CODEX