1. Giampaolo Piotto Dipartimento di Astronomia - Università di Padova Giampaolo.Piotto@unipd.it PLAnetary Transits & Oscillations of stars Search for and characterisation of exoplanets + asteroseismology going beyond CoRoT & Kepler PLATO KOM+1 meeting & Telescope Group Meeting Roma, January 29, 2009

2. Agenda: 09:15-09:30 Giampaolo Piotto - Welcome and Communications 09:30-10:00 Claude Catala - PPLC: Status and future steps 10:00-10:30 Roberto Ragazzoni - TOU: Status and future steps 10:30-10:45 Break 10:45-11:15 Andrea Baruffolo - ICU: Status and future steps 11:15-11:45 Giampaolo Piotto (Silvano Desidera) - PSC: Status and future steps 11.45-12:00 Isabella Pagano - PLATO Management in Italy: info 12:00-13:00 Discussion 13:00 - 14:00 lunch 14:00 - 14:20 Demetrio Magrin - Report on Optical Design 14.20 - 14:40 Daniele Piazza - Report from Mechanical Design 14:40 - 15:00 Stefano Basso - Report from Thermo-mechanical Analysis 15:00 - 15:30 Jose Luis San Juan - I/F between FPA and TOU 15:30 - 15:45 Mauro Ghigo - Report from Optical Material Analysis 15:45 - 16:00 Matteo Munari - Report from Straylight Analysis & BafflingReport from Straylight Analysis & Baffling 16:00 - 17:00 Plans for future activities (chair Ragazzoni) Roma, Jan 29, 2009G. Piotto

4. Science Objectives The evolution of planets and that of their stars are intimately linked. A complete and precise characterization of host stars is necessary to: Measure exoplanet properties: mass, radius, age Compare planetary systems of various ages Observe exoplanets at different stages of dynamical evolution and at different stages of physical and chemical evolution Correlation of planet evolution with that of their hosts stars Roma, Jan 29, 2009G. Piotto The evolution of exoplanetary systems = comparative exoplanetology

5. Mission Objectives The Search for, and characterization of, exoplanets and their host stars Logical step forward after CoRoT and Kepler (and TESS?) Search for exoplanetary transits and asteroseismology for the same star samples Roma, Jan 29, 2009G. Piotto

6. The PLATO Science Consortium PI: Don Pollacco Co-PIs: Connie Aerts Heike Rauer Giampaolo Piotto Stephane Udry Kick-Off meeting, Paris, Nov 13, 2009 Roma, Jan 29, 2009G. Piotto

7. PSC Don Pollacco S: Planet detection and characterization Heike Rauer F: Field Section and Simulations Giampaolo Piotto P: Characterization of host stars Cconnie Aerts D: Data base interface Heike Rauer U: Ground based observations Stephan Udry PLATO Science Consortium (DLP) Science Requirements Roma, Jan 29, 2009G. Piotto

8. S: Planet detection and characterization HR S1 Overview of PLATO Science HR S2 Planet detection and statistics WB, CAF S3: Characterization of planets and planetary system evolution HR; HL; LG; RN S4: Additional Science WW S: Planet detection and characterization (HR) Roma, Jan 29, 2009G. Piotto

9. S2 Planet detection and statistics WB; CAF S2.1 General Overview ??? S2.2 Detection of Earth – Analog systems DLP; DQ et Al. S2.3 Expected detection statistics ??? S2.4 Additional detections (TTV, Phase variations etc.) DLP S2: Planet detection and statistics (WB; CAF) Roma, Jan 29, 2009G. Piotto

10. S3: Characterization of planets and planetary system evolution HR; HL; LG; RN S3.1: General Introduction ??? S3.2: Constraints on planetary system evolution ??? S3.3: Planetary Characterization with PLATO ??? S3.4: PLATO Planets Char. (JWST; ELT etc.) SD S3.5: Star Planet Interaction CM, IP, SA S3: Characterization of Planets and Planetary system evolution (HR; HL; LG; RN) Roma, Jan 29, 2009G. Piotto

11. F: Field Selection and Simulations GP F1: Input parameters RC F2: Image simulations TA F3: Light curve Analysis GP F: Field selection and simulation (GP) Roma, Jan 29, 2009G. Piotto

12. F1: Input Parameters RC F1.1: Field Selection MB F1.2: Planetary system simulation WB F1.3: Instrumental Noise sources DW F1.4: Astrophysical Noise Source RC F1.5: Jitter RSa F1: Input Parameters (GP) Roma, Jan 29, 2009G. Piotto

13. F2: Image simulation TA F2.1: Photometric Algorithms TA; WZ F2.2: Light curve extraction WZ; TA F2: Image simulation (TA) Roma, Jan 29, 2009G. Piotto

14. F3: Light Curve Analysis GP F3.1: Transit light curve analysis MB (opp AB) F3.2: Seismic light curve analysis RC F3.3: Stellar Activity IP (opp AB) F3.4 (former P1): Micro variability detection and pre- whitening CA F3: Light Curve Analysis Roma, Jan 29, 2009G. Piotto

15. Characterization of host stars CA P1: Internal angular momentum mapping ??? P2: Stellar ages and radii for solar-like stars BC P3: Surface magnetic activity mapping NL or ACC P: Characterization of host stars (CA)

16. Data Base Interface HR D1: Scientific requirements from DB ??? D2: Mining Tools BC D: Data Base Interface (HR)

17. Ground Based Observations SU U1: Preparatory Observations required Italy? U2: Dem. of requirements and Fup cap. etc. ??? U: Ground Base Observations (SU)

18. Evolution of Scientific Requirements high level science requirements redefined by PSST and PSC - P1: > 20,000 bright (~ m V 11) cool dwarfs (>F5V); noise < 27 ppm in 1hr - P2: > 80,000 bright cool dwarfs; noise < 80 ppm in 1hr during long pointing but < 27 ppm in 1 hr during step & stare phase - P3: ~ 1000 very bright stars (4 m V 8) for 3 years - P4: ~ 3000 very bright stars (4 m V 8) for > 5 months - P5: > 250,000 cool dwarfs; noise < 80 ppm in 1 hr for 3 years

19. New baseline design four-l.o.s. 42 telescopes 3.60 m 40 normal telescopes 2 fast telescopes 56° Roma, Jan 29, 2009G. Piotto

20. 10 20 40 pupil size 120mm pixel size 15 arcsec 40+2 telescopes total field of view (2 pointings) = 3600 sq deg 42° as proposed by optics/telescope team PLATO 4 OVERLAPPING L.O.S CONCEPT Roma, Jan 29, 2009G. Piotto

21. Performance of baseline design magnitude for noise 27 ppm in 1 hr compliant non compliant

22. Performance of baseline design

23. Simulations Main goal for the Assessment phase is to test the PLATO photometric performances Should be a tool for an independent test of the PLATO onboard and GB software It is a tool for both the PPLC and the PSC Roma, Jan 29, 2009G. Piotto

24. Simulations start-up We started from the Eddington Simulation Tool (Torben Arentoft) We used PSFs from the TG (D. Magrin) We simulated 2 512x512pxs sets of images at center of the field, with a 12.5 and a 15 arcsec/pixel PSFs 2 fields: a crowded Carina field, and less crowded field CCD noise and Jitter from Eddington Unweighted mask aperture photometry Roma, Jan 29, 2009G. Piotto

25. Roma, Jan 29, 2009G. Piotto Carina Field Standard field

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