1. PlanetVision: Belgian-Spanish project for the characterization of planetary systems, stars and planets A. Moya and H. Deeg et al. (Spain) C. Aerts and J. De Ridder et al. (Belgium) N. Santos et al. (Portugal) H. Kjeldsen et al. (Denmark) L. Kiss et al. (Hungary)

2. General context 1)Understand the origin and structure of the diversity of planetary systems found 2)Is there life outside the Solar System? 3)Steps planned already: I.Search for exoplanets II.Accurate characterization of these systems, habitability studies III.Search for biomarkers “An European roadmap for exoplanets” (Exoplanet Roadmap Advisory Team, October 2010)

3. History of project 1) 2010/11: informal discussions in Spain to lead space project, topic exoplanet & astero science (Andy Moya & Hans Deeg + industrials) 2) Contact with C. Aerts in June 2011 to consider bilateral project: PlanetVision as answer to future S-mission call of ESA 3) First specs defined over summer (incl. Joris De Ridder, CoRoT and Kepler heritage) 4) Delegations + ESA meet in Madrid & Brussels, Oct. 2011, Jan. 2012 5) 2011/12: Discussions with Swiss-led consortium but mission concepts judged too ≠

4. Current situation ~ 700 exoplanets known First planets touching habitable zone found in 2010 and 2011

5. Current situation ~ 600 discovered from ground ~170 with transits: mass, size, etc. known: 1) ~ 50 from space (high accuracy) 2) ~ 120 from ground (low accuracy) The focus in exoplanets is changing from discovering to understanding. ~ 450 discovered with RV (poor information)

6. There is only one thoroughly studied case: The Solar System. a) Exoplanet’s nature: density, surface properties, atmospheric properties b) Planetary orbits: Historical evolution, effects due to other bodies c) Host stars: Evolution, chemical composition, accurate physical characteristics Current research issues

7. Current situation Transits Radial Velocity Direct imaging (age)

8. Homogeneous studies of transiting extrasolar planets. IV. Thirty systems with space-based light curves M*M* R*R* ρ*ρ* AgeMpMp RpRp 9,3%7%13.7%150%10.6%7.1% Mean errors Southworth, J., 2011, arXiv:1107.1235 Current situation Errors of M P and R P dominated by errors of M * and R *

9. Almost a 47% have m V <8, a 72% have m V <10 Current situation

10. PlanetVision: Scientific project

11. Scientific project Data acquisition technique: Observation of temporal series of high-precision multicolor photometry

12. Scientific project 1)Exoplanet science : Led by Spain 1)Asteroseismology : Led by Belgium Scientific methods: Goal: Bright stars with planets (Specs defined for m v <8)

13. Exoplanet’s photometry: Transits, eclipses, reflected light PlanetVision complements space observations (CoRoT, Kepler) and improves ground-based observations - Consistent high-precision photometry in 3 color bands for bright targets (cf. EChO preparation) - Long observations with high duty cycle - flexibility in targets to observe: · Large range of brightness admissible, · Entire sky accessible, · High temporal resolution possible

14. The more transits are observed, the greater the accuracy of the characterization Exoplanet’s photometry: Transits, eclipses, reflected light

15. Exoplanets science: Objectives 1) Characterization of planetary systems already known A. Improving planet and star system parameters B. Studies about the planet atmospheres C. Detection of further bodies in transiting systems D. Studies on planet host stars 2) Discovering of new planets A. Verification of candidates coming from other instruments B. Direct discovery of new transits

16. High precision photometry with at least three different photometric bands, pointing flexibility, very high duty cycle. 3) Study of planets WITHOUT known transits A. Detection of reflected planetary light B. Search for transits of RV planets Exoplanets science: Objectives

17. Asteroseismology Something similar happens in the stars

18. Asteroseismology Real cases

19. From Asteroseismology μ Arae Very accurate determination Y=0.30±0.01, Age=6.3±0.8 Gyr

20. From asteroseismology 1 planet (Transit) Kepler observations solar-like modes Work: Christensen-Dalsgaard et al., 2010 Age=2.14 ± 0.26 Gyr Mean density=0.2712 ± 0.0032 g cm -3 Uncertainty R p changes 3% → 0.5%

21. From asteroseismology Precision obtained with Kepler An uniform asteroseismic analysis of 22 solar-type stars observed with Kepler Mathur et al., 2012, A&A, in press Individual frequencies not resolved Individual frequencies resolved Mass5%1% Radius2%1% Age10%2.5%

22. Asteroseismology: Objectives Precise stellar densities permit improvement of planet parameters 1) Accurate characterization of the physical properties of the star (mass, radius, age, chemical composition,…) 2) Improve our understanding of the stellar structure and evolution 3) Understand the planetary systems origin and evolution 4) Discovering new planets (timing)

23. Error (with asteroseismology + Gaia) Asteroseismology Consequences of observing stellar pulsations

24. Preliminary requirements 1) Photometric precision of 50 ppm with integrations of 10 min, stars m v <8 2) To be able to monitore any position in the sky at least at once during the year 3) Flexible duration of the monitoring between 3 hours and 3 months 4) Three well separated photometric bands 5) FOV > few to tens of sq deg (tbd) 6) Temporal resolution as short as 1s should be available 7) Duty cycle > 90% (95%), minimizing periodic gaps between 0.002-10 mHz 8) High dynamic range

25. Payload: 1) 3-6 Telescopes (tbd) 2) 15-30 cm primary each (tbd) 3) Backside-illuminated CMOS + NIR detectors, each telescope separately Specs and observing strategy, field selection, all to be fine-tuned using the PLATO simulator tool (already developed in Leuven) Preliminary design

26. Dedicated observations for individual objects or small groups Preliminary observation strategy

27. Platform: Ingenio Ingenio is a mission for the optical observation of the Earth. Orbit: Likely an ETO, as Kepler, Spitzer,... This mission has already almost all the required characteristics (pointing, size, cost, data transmission, etc.)

28. ~2.5 m 1.5 m Platform: Ingenio Dimensions Approximate weight: 800 kg

29. Time schedule phaset0t0 t 0 +1+2+3+4+5+6+7+8+9+10 0 / A B C/D Laun. Exploit. = expected launch of M3 (approx)

30. Phase 0 objectives 1. Scientific consortium consolidation 2. Accurate determination of the scientific requirements 3. First approach to the satellite system 1.Direct contacts 2.Workshop 3.Technical support. Phase 0 main actions

31. PlanetVision in context: other missions

32. The project in context Main characteristics: 1)Pointing flexibility 2)Different photometric bands Unique project at the present time Main objective: Accurate determination of physical properties of planets already discovered from ground.

33. PlanetVision in context: other missions Future space projects: EChO and Plato PLAVI is needed by EChO, since they need accurate physical properties of the planets they plan to study. PLAVI will deliver the much needed bright tarjets for EChO

34. The Spanish and Belgian scientific communities

35. KUL (Conny Aerts, Joris De Ridder) ROB (Peter de Cat) ULg (M.A. Dupret) Belgian scientific community Exoplanetary science and asteroseismology Some 50 Belgian scientists BISA (Frank Daerden, Severine Robert) ULB (Alain Jorissen) FUNDP (Anne Lemaitre)

36. IAC (Hans Deeg and Pere Pallé) CAB, INTA-CSIC (Andrés Moya, David Barrado, Miguel Mas, Enrique Solano) U Vigo (Ana Ulla) UV (Juan Fabregat) IAA, CSIC (Rafael Garrido, J.C. Suárez, P.J. Amado) Spanish scientific community ICE, CSIC (M. López- Morales) Exoplanetary science and asteroseismology Some 40 Spanish scientists

37. Portuguese, Danish and Hungarian scientific communities CAUP (Mario Monteiro, Nuno Santos) University of Århus (Hans Kjeldsen, Joergen Christensen-Dalsgaard) Observatory of Konkoly (Laszlo Kiss, Robert Szabo) University of Aveiro (Alexandre Correia, Helena Morais)

38. Thanks!