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The origin of the mission The scientific requirements The global programme

An introduction to the CoRoT mission. 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. http://www.astrsp-mrs.fr/projets/corot http://cnes.mission.fr/corot.

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The origin of the mission The scientific requirements The global programme

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

  2. 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 Annie Baglin, Natal, October 30th 2004

  3. 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 • High resolution Spectroscopy • Large telescopes • Limited to low Vr • Photometry • limited by scintillation on the ground 2 10-4 / mHz Goal: < ppm in 5 days : ~ 2 10-7 / mHz ~ 1000 times less ! from E. Fossat, San Diego Workshop, Annie Baglin, Natal, October 30th 2004

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

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

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

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

  8. Seismology requirements/2 16 14 12 10 10ppm , 40d 8 6 10ppm , 5d 4 2 2ppm , 5d 0 -1 -0.5 0 0.5 1 1.5 2 2.5 3 log D * A periodic signal in a white noise S/N = N2 a 2 t/ 4 s2 in the power spectrum • N mean counting rate (ph/s), • a amplitude • variance of a white noise t = inf (T, t ) T total duration of the observation, t life-time of the mode If Photon noise limitedS/N = N a 2 t / 4 Detection probability 99 % : S/N ≥ 9 a= 2 ppm, T = 5 days, ---->>N ≥ 5 106 ph/s log(D/25cm) ≥ 0.2 (mv - 6) • * Frequency resolution:<< 2 mHz0.1 mHzT > 120 days • * No window alias: duty cycle > 90% mv=6 D=27cm Annie Baglin, Natal, October 30th 2004

  9. Detection of small planets F/F ≈10 hrs 100 ppm t(hrs) In photometry, through transits.. * Brightness variation during a transit DF/F= (Rpl/Ret)2 Earth : 10-4 , Jupiter : 10-2 * Duration of a transit t t= P 2R*/2pa a1/2 R* Earth: 14h, Jupiter 31h, 51 Peg 3h Telluric planets are detectable if photon noise < 10-4 in a few h * Periodicity During a run T >> P Number of observed transits : N = T/P  a-3/2 Cumulated signal : N t a-1 Favors planets close to the star • Low probability to be in the orbital plane: • observe a large number of targets Annie Baglin, Natal, October 30th 2004

  10. Exoplanet programme requirements Exoplanet Field On focus (prism) * Seismology specifications compatible with transit detection of earth-like planets D ≥ 25 cm Nphot= 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 Three colors aperture photometry on dispersed images * Confusion transit/activity chromatic device can separate …… Annie Baglin, Natal, October 30th 2004

  11. Mission profile Mission profile 180 ° Rotation of SC Beginning of observation zone 2 B A Sun 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 Earth orbit Corot Orbital plane Beginning of observation zone 1 Constraint of Low Earth Orbit / Requirement Run duration ≥ 120 days Limited regions of the sky accessible Wide set of stars --> mv ~ 6 Annie Baglin, Natal, October 30th 2004

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

  13. Photometric performances in the seismology field Aperture photometry on highly out of focus images 50 pixels (1px = 2.32 arcsec) 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 Photon noise and total white noise as a function of magnitude in ppm for a five days observation Annie Baglin, Natal, October 30th 2004

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

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

  16. 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 Annie Baglin, Natal, October 30th 2004

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

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

  19. 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 Annie Baglin, Natal, October 30th 2004

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

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

  22. Seismology GBO 1-Photometric & spectroscopic observations of targets up to mV=8 for scenarii 1.2.3.4 Stromgren photometry from OSN, Spain High res. spectroscopy from ELODIE/OHP FEROS (ESO+BRASIL) SARG/TNG +Coralie + Tautenburg • All observations complete: about 1500 stars .Data in GAUDI • Teff, log g, MV, [Fe/H], vsini, VR derived from these data, in Corotsky and GAUDI • 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 ≤ mV ≤ 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 Annie Baglin, Natal, October 30th 2004

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

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

  25. A possible HD 49933/49434 long run Exobasket Annie Baglin, Natal, October 30th 2004

  26. 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 Annie Baglin, Natal, October 30th 2004

  27. The COROT Team CNES : global responsability of the mission • FRANCE: 3 space laboratories : • LAM Marseille, • LESIA Observatoire de Paris, • IAS Orsay • Contributions ofGEPI,OMP, IAP, OCA, OHP • 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)…... Annie Baglin, Natal, October 30th 2004

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

  29. The Scientific Committee COROT WEEKS twice a year Open scientific Meetings + CS and WGs 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 • Chairperson : PI • CNES Programmes Directorate • Project Scientist • Representatives • major laboratory (6) • participating countries( • Chairs of the Working Groups (5) • Project Manager (invited) Marseille 2003 Nice 1999 7th in Granada (Spain), Dec 14th to 17th You are all welcome! Meetings:Twice a year or more At each CW Annie Baglin, Natal, October 30th 2004

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

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

  32. 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 Annie Baglin, Natal, October 30th 2004

  33. KEPLER Terrestrial planets finding NASA Launch 2008? 5 years on one field 95 cm Schmidt telescope FOV 100deg2 100 CCDs Trailing orbit Annie Baglin, Natal, October 30th 2004

  34. EDDINGTON: the mission Culmination of the European efforts Horizon 2000 + medium size mission Seismology + Planet finding 4 identical co-aligned 60 cm Schmidt telescopes On a Herschel bus FOV = 35 deg2 At L2 Programmatic difficulties….??? Annie Baglin, Natal, October 30th 2004

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

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

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