PLAnetary Transits and Oscillations of stars PLATO Consortium kick-off meeting

Day 1: - plenary meeting - hosted by CNES (thank you!) - goal = browse all aspects of the mission - opportunity for each consortium participant to learn about the parts of the project that he (she) doesn’t know Messages to all speakers: Please respect your time allocation (includes discussion): very tight schedule today !! Please send your presentation to AS SOON AS This evening: reception in Salle Cassini at Observatoire de Paris, starting at 19:30 Day 2: - splinter meetings at Observatoire de Paris: payload, PDC, PSPM - goal = organize the work of the three elements of the project - joint PDC + PSPM splinter in the morning A few details on the meeting organization

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

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

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:  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

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

~ 50% of the sky ! CoRoT Kepler PLATO 1. two long pointings : 3 years or 2 years 2. « step&stare » phase (1 or 2 years) : N fields 2-5 months each Observation strategy and sky coverage

Expected noise level shot noise + readout noise + background noise + jitter + digitization noise 27 ppm 80 ppm 800 ppm fast cam 8 cam 16 cam 24 cam32 cam jitter/confusion + background photon noise photon noise limited up to m V =11

Performances as a function of noise level as a function of magnitude PLATO (4300 deg 2 )20,000 deg 2 KEPLER (100 deg 2 ) noise level (ppm/√hr) nb of cool dwarfs & subgiants long monitoring mVmV nb of cool dwarfs & subgiants incl. step&stare nb of cool dwarfs & subgiants mVmV 2720, ,4001, , ,000,00025, ,32683, , ,0001,30011

PLATO Mission Consortium - Study, develop and deliver instrument: cameras + DPS - Study, develop and operate PLATO Data Centre - Milestones: Oct. 29, 2010: Answer to the ESA AO Nov. 9 &10, 2010: PMC kick-off meeting May 2011: Preliminary Instrument Requirement Review (PIRR) provide documentation by end of April on all aspects of the mission Jun. 2011: M2 down-selection by SPC Oct. 2011: Instrument Design Consolidation Review (IDCR) Dec 2011: Official end of definition phase Jun. 2012: Instrument Preliminary Design Review (PDR)

ESA project team End-to-end Simulator W. Zima PLATO Payload Management PIPM: P. Bodin PDC PDPM: L. Gizon Instrument System Coordinator P. Levacher Science Coordination H. Rauer Target/field Characterization G. Piotto FU Coordination S. Udry Stellar Science M.J. Goupil Exoplanet science D. Pollacco TOU R. Ragazzoni Fast DPU G. Peter Normal DPU Ph. Plasson PLATO Mission Consortium Science Preparation Management Algorithms R. Samadi Mission management AEU S. Fredon ICU R. Cosentino Prototype & FM AIV P. Levacher main / ancillary database system architecture R. Burston exoplanet analysis System N. Walton data processing implementation I. Pardowitz stellar analysis system T. Appourchaux Input Catalogue P. Giommi Data Centre Normal TOU R. Ragazzoni Fast TOU W. Benz Project Manager Project ScientistScience Team - 6 PMC members - 2 Legacy Scientists PMC Board ancillary database content management M. Deleuil data analysis support tools L. Gizon FPA/FEE D. Walton/M. Mas Hardware & boot software M. Mas Application software Ph. Plasson PMC Lead C. Catala Camera Management D. Laubier DPS Management B. Pontet Payload SOC data processing algorithms R. Samadi Additional programs W. Weiss