1. 1Annie Baglin, Natal, October 30th 2004 The origin of the mission The scientific requirements The global programme The focal plane and the targets The scientific organisation COnvection, ROtation and planetary Transits An introduction to the CoRoT mission http://www.astrsp-mrs.fr/projets/corot http://cnes.mission.fr/corot

2. 2Annie Baglin, Natal, October 30th 2004 The COROT concept * Ultra high precision stellar variability * Very long duration of observations * without interruption * on a large variety of stars Relative variations of stellar quantities mainly in the optical domain, Analysis in the time/frequency space  Photometry from Space  Ministallite  World wide pioneer

3. 3Annie Baglin, Natal, October 30th 2004 The early days of the space adventure First Colloquium Observatoire de Paris in 1984 Workshop on Improvements to photometry San Diego 1984 Stating the importance of space for stellar seismology and activity from E. Fossat, San Diego Workshop, High resolution Spectroscopy Large telescopes Limited to low Vr Photometry limited by scintillation on the ground Goal: < ppm in 5 days : ~ 2 10 -7 /  Hz ~ 1000 times less ! 2 10 -4 /  Hz

4. 4Annie Baglin, Natal, October 30th 2004 EVRIS Telescope 15 cm, Built in Meudon, Marseille and Austria On board the Soviet spacecraft Mars 96 Observation of 10 very bright stars During the cruise to Mars MOST (  sat Canada), analogous to EVRIS is now flying….. CRASH! But……. After many proposals on different programmes EVRIS accepted by CNES…… in 89

5. 5Annie Baglin, Natal, October 30th 2004 Several european projects Combining seismology and activity (visible and UV instruments) PRISMA(1993) 1m visible, 3° FoV Far UV 10cm monitor CII Large phot (40,1.5°) Small phot (15 cm, 3°) UVSpectro (57cm, R=30 000) XUV tel (40cm, 13nm) STARS (1996) But not selected

6. 6Annie Baglin, Natal, October 30th 2004 The long way to go…. But……. crash of Mars 96, ……..discovery of exoplanets in 95 ……..improvement of detectors …..New proposal in 97 Started in 93 as an answer to a AO for minisats by CNES As a second generation mission…… Preselected in 98 Selected in 2000 launch in 2004..! Confirmed in 2002 after some threat….. European and Brasilian partners

7. 7Annie Baglin, Natal, October 30th 2004 Seismology requirements/1 The solar template (only star observed in photometry) 2 ppm 5 days Amplitude behavior from spectroscopic stellar seismology a v ~ (L/M) 0.7 Parameters of a stellar mode ? Amplitudes in Vr relative to the Sun (27cm/s) From Samadi et al (2004) HD 49933

8. 8Annie Baglin, Natal, October 30th 2004 Seismology requirements/2 a= 2 ppm, T = 5 days, ---->> N ≥ 5 10 6 ph/s N mean counting rate (ph/s), a amplitude  variance of a white noise t = inf (T,  ) T total duration of the observation,  life-time of the mode S/N = N 2 a 2 t/ 4   in the power spectrum If Photon noise limited S/N = N a 2 t / 4 log(D/25cm) ≥ 0.2 (m v - 6) 0 2 4 6 8 10 12 14 16 -0.500.511.522.53 log D 2ppm, 5d 10ppm, 5d 10ppm, 40d * A periodic signal in a white noise * Frequency resolution: 120 days * No window alias: duty cycle > 90% Detection probability 99 % : S/N ≥ 9 m v =6 D=27cm

9. 9Annie Baglin, Natal, October 30th 2004 Detection of small planets * Brightness variation during a transit  F/F= (R pl /R et ) 2 Earth : 10 -4, Jupiter : 10 -2  F/F t(hrs) 100 ppm ≈10 hrs Telluric planets are detectable if photon noise < 10 -4 in a few h * Duration of a transit   = P 2R * /2  a R *  = P 2R * /2  a  a 1/2 R * Earth: 14h, Jupiter 31h, 51 Peg 3h * Periodicity During a run T >> P Number of observed transits : N = T/P  a -3/2 Cumulated signal : N   a -1 Favors planets close to the star Low probability to be in the orbital plane: observe a large number of targets In photometry, through transits..

10. 10Annie Baglin, Natal, October 30th 2004 Exoplanet programme requirements * Seismology specifications compatible with transit detection of earth-like planets D ≥ 25 cm N phot = 10 -4 in 3 hours for mv=14 T ≥ 120 days 3 transits for a < 0.3 u.a. * ~ 12 000 * mv < 16 FOV ~ 4 sq deg --> specific regions of the sky * Confusion transit/activity chromatic device can separate …… Three colors aperture photometry on dispersed images Exoplanet Field On focus (prism)

11. 11Annie Baglin, Natal, October 30th 2004 Mission profile 1 Long run ~150 days 1 Short run ~(180-150-10) each half year (duration can be modulated) A few short runs at the beginning Mission profile Beginning of observation zone 1 Sun Earth orbit Beginning of observation zone 2 180 ° Rotation of SC Corot Orbital plane Constraint of Low Earth Orbit / Requirement Run duration ≥ 120 days Limited regions of the sky accessible Wide set of stars --> mv ~ 6 A B

12. 12Annie Baglin, Natal, October 30th 2004 The focal plane 12000 targets sampling 512 s * * * * * * * * * * 1.3 ° field of view Seismology field highly out of focus main target (≤ 6) secondary targets (≤ 9.5) 10 targets sampling 1 s Exoplanet field On focus + bi-prism faint stars (11-16) Short duration mission (2.5 y) -->Simultaneity of the two programmes

13. 13Annie Baglin, Natal, October 30th 2004 Photometric performances in the seismology field For mv=5.7 in five days photon noise Np = 0.6ppm total noise Nt = 0.61ppm Nt= 0.61 10 0.2(mv-5.7) for mv<9 For mv > 9 increase of the readout noise Very low jitter and background noises Aperture photometry on highly out of focus images 50 pixels (1px = 2.32 arcsec) Photon noise and total white noise as a function of magnitude in ppm for a five days observation

14. 14Annie Baglin, Natal, October 30th 2004 Photometric performances in the exoplanet field Exoplanet Field On focus (prism) The jitter is the major source of instrumental noise It will be corrected on ground, See Fabio’s talk Blue (resp. red) :30±8 (resp. 40 ±15) % of the total flux do not correspond to a fixed photometric system

15. 15Annie Baglin, Natal, October 30th 2004 The planet hunting RaceKEPLER(2008/9)EDDINGTON(?) Habitable zone zone Vr (2003) COROT (2006) GAIA (2011/2)

16. 16Annie Baglin, Natal, October 30th 2004 High precision photometric data Secondary science with CoRoT ? Described e.g. in Weiss et al 2004 Palermo Eddington colloquium Wide variety of subjects and interest *Large and complete stellar data base of more than 100000 stars 11 < V < 16 *Also a few selected targets Creation of the Additional Programmes

17. 17Annie Baglin, Natal, October 30th 2004 Browsing in the exoplanet data Measuring limb darkening with binaries Defining the  Dor domain COROT Detecting infalling comets

18. 18Annie Baglin, Natal, October 30th 2004 Observing specific objects EX: NGC 2264 from WEBDA v<8.5 8.5<v<9.5 9.5<v<12 + v>12 Up to 10 stars in CCDA1 and CCDA2 Or many faint ones in exo field

19. 19Annie Baglin, Natal, October 30th 2004 The global programme Core programme Seismology +Exoplanet (In the corresponding focal planes) Central programme ≥ 5 long runs (150 days) 50 S targets mv < 9.5 60 000 E targets mv < 15.5 Exploratory programme ~ 4 short runs (10 to 20 days) 50 S targets mv < 9.5 60 000 E targets mv < 15.5 Restricted to Co-Is and their teams Additional programmes Any scientific field except Core Programme ~ 4 specific short runs 50 S targets mv < 10.5 ? 60 000 E targets mv < 16 ? A few targets in the exoplanet field Use of the data of the core programme Open AO, GIs

20. 20Annie Baglin, Natal, October 30th 2004 The eyes of COROT C1: density dwarfs ≥ 1500 per square degree at mv<15.5 C2: ≥ 5 main targets FGK IV, V mv< 6.5 Delta scuti < 9 Scientific Constraints  =102.5 and 282.5 Early feasibility studies based on catalogues and plates

21. 21Annie Baglin, Natal, October 30th 2004 Ground based complementary observations Effort supported by Laboratories and Participating Countries Collection of data on potential targets to determine the fundamental parameters (T eff, logg, [Fe/H], Vsini..) select the targets prepare ground-based support and follow-up Bright for the seismology field > 250 nights > 250 nights 0.9 to 3.5 m telescopes 0.9 to 3.5 m telescopes > 1500 stars > 1500 stars Data base: GAUDI at LAEFF Faint stars for the exoplanet field ≥ 2.5m telescopes 100 million stars Data base: EXODAT at LAM

22. 22Annie Baglin, Natal, October 30th 2004 Seismology GBO 1-Photometric & spectroscopic observations of targets up to m V =8 for scenarii 1.2.3.4 All observations complete: about 1500 stars.Data in GAUDI Teff, log g, M V, [Fe/H], vsini, V R derived from these data, in Corotsky and GAUDI Stromgren photometry from OSN, Spain High res. spectroscopy from ELODIE/OHP FEROS (ESO+BRASIL) SARG/TNG +Coralie + Tautenburg 2- New targets to be observed because of possible drift of orbital plane (552 new targets, 68 near primary objects) Work started on ESO/FEROS (Renan ) 3- Observations of targets with 8 ≤ m V ≤ 9.5 in 1.4° x 2.8° field around main targets (386 stars) photometric Stromgren observations: IAA/OSN in 2004/2005 spectroscopic observations: proposal for CFHT/Espadons for 2005A (all 386 stars in 3 nights) additional proposal for ESO/FEROS

23. 23Annie Baglin, Natal, October 30th 2004 Preselected fields for long runs 1 Winter 2006/7 2 Summer 2007

24. 24Annie Baglin, Natal, October 30th 2004 Seismology targets Principal targetsA possible choice for secondary targets Need of more precise fundamental parameters

25. 25Annie Baglin, Natal, October 30th 2004 A possible HD 49933/49434 long run Exobasket RrangecontamE1E2Total 11-150.1263022214851 11-150.2425265690 15-160.1184512003045 15-160.26019261527 11-160.25501461210113 11-14> 0.2181173354

26. 26Annie Baglin, Natal, October 30th 2004 Next steps 1- CW7 in Granada December 2004 - confirm the two first fields for the long runs: LR1a, LR1c star densities for exo, set of secondary targets for sismo 2- January 2005 AO for AP CoRoT year 1 3- CW8 in Toulouse June 2005 - prepare the first short runs SR0a (split in 2? Also technical), SR1a - define the next two other long runs: LR2a, LR2c - select the AP for CoRoT year 1 4- CW9 December 2005 - Selection of the first short runs SR0a, SR1a, SR1c: AP? - define the next two other long runs: LR3a, LR3c 5- January 2006 AO for AP CoRoT year 2………. Still preliminary…….subject to modifications

27. 27Annie Baglin, Natal, October 30th 2004 The COROT Team RSSD/ESTEC: MDP Unit SPAIN: Ground segment AUSTRIA: participation to the DPU ESA Scientific programme: Optics and AIT contribution BELGIUM: Baffle, cover, mechanics of the service module GERMANY: onboard software BRAZIL : antenna, ground segment software Contributions : Italy, Romania, Hungary.. (ground + science)…... FRANCE : 3 space laboratories : LAM Marseille, LESIA Observatoire de Paris, IAS Orsay Contributions of GEPI, OMP, IAP, OCA, OHP CNES : global responsability of the mission

28. 28Annie Baglin, Natal, October 30th 2004 The Scientific Organisation Seismology W.G. E. Michel Scientific Committee Additional Prog.W.G. W. Weiss CORE programme Central + Exploratory Exoplanet W.G. P. Barge Seismology Ground based obs. C. Catala Sc. Teams Co_Is Sc. Teams Co_Is Sc. Teams Co_Is Sc. Teams Co_Is/GIs Sc. Teams Co_Is Exoplanet Complement obs. M. Deleuil

29. 29Annie Baglin, Natal, October 30th 2004 The Scientific Committee Chairperson : PI CNES Programmes Directorate Project Scientist Representatives major laboratory (6) participating countries( Chairs of the Working Groups (5) Project Manager (invited) In charge of - the scientific specifications - the programme of observations - the data distribution policy - the list of Co-Is and Gis - Programme of CWs - Public relations COROT WEEKS twice a year Open scientific Meetings + CS and WGs 7th in Granada (Spain), Dec 14th to 17th Meetings:Twice a year or more At each CW Nice 1999 Marseille 2003

30. 30Annie Baglin, Natal, October 30th 2004 The data policy Public release Observation Data reduction Distribution of I(t) to the CoIs and GIs 150 days ~ a few months ~ 1 year Responsability: Project Team * Publications will be put on a secured site To be Referred by the SC within 15 days (TBC)

31. 31Annie Baglin, Natal, October 30th 2004 Do sonho ate a realidade ~ Junho 2006…..!

32. 32Annie Baglin, Natal, October 30th 2004 MOST a pionner microsat 1st canadian microsatellite Launched June 30th 2003 Suitcase size 15 cm collector Mono-object Heliosynchroneus LEO A few bright stars, 30 days mv = [ 0,5] of all types Procyon, amplitude spectrum a) observed by MOST for 32 days b) simulated signal: p modes 10ppm and 3 days lifetime

33. 33Annie Baglin, Natal, October 30th 2004 KEPLER Terrestrial planets finding NASA Launch 2008? 95 cm Schmidt telescope FOV 100deg 2 100 CCDs Trailing orbit 5 years on one field

34. 34Annie Baglin, Natal, October 30th 2004 EDDINGTON: the mission 4 identical co-aligned 60 cm Schmidt telescopes On a Herschel bus FOV = 35 deg 2 At L2 Programmatic difficulties….??? Culmination of the European efforts Horizon 2000 + medium size mission Seismology + Planet finding

35. 35Annie Baglin, Natal, October 30th 2004 GAIA ESA Cornerstone 2010-2012 Stellar physics Fundamental parameters Luminosity calibration Variability levels Binaries…… Planet finding Astrometry >10 000 P ~yrs Photometry > 5000 P ~days HR diagram Hyades HIPPARCOS Age 625±50 Myr Y=0.26±0.02

36. 36Annie Baglin, Natal, October 30th 2004 DARWIN/TPF 2015 ? Imaging the planets Interferometry or coronography