1. 1 COROT, COnvection ROtation and planetary Transits Ennio PORETTI INAF – Osservatorio Astronomico di Brera COROT mission: scientific profile and preparatory ground-based observations

2. 2 Woman with a pearl Louvre Jean Baptiste Camille COROT (1795-1875)

3. 3 The Bridge at Nantes Louvre Jean Baptiste Camille COROT (1795-1875)

4. 4 OUTLINES OUTLINES THE MISSION The consortium, the persons, the satellite The orbital plane, the observing modes The scientific profiles THE PREPARATORY WORK FOR ASTEROSEISMOLOGY Target selection in the Center and Anticenter directions Target characterisation Future activities

5. 5 7 countries or organizations are officially collaborating and supporting the mission Austria Electronic parts Spain Mission Center Germany On-fly software Belgium Case and Baffle Brasil Secondary antenna ESA Optics SSD Processors Instrument Ground segment International Partners International Partners

6. 6 Launched on December 27, 2006  New SOYUZ rocket from Baïkonour A. Baglin Principal Investigator Th. Lam-Trong Project Manager M. AuvergneProject Scientist L. Boisnard Mission Engineer Documentation : http://corot-mission.cnes.fr http://www.obspm.fr/planets http://www.astrsp-mrs/projets/corot

7. 7

8. 8 General characteristics Aperture : 4.20 m x 9.60 m PROTEUS platform Developed by CNES and Alcatel Space for low orbits. First flight in 2001 : JASON oceanographic satellite 5 missions are scheduled Mass : 600 kg (launch configuration)

9. 9 Telescope (COROTEL)  entrance pupil 270 mm  2 parabolic mirrors  cylindric external baffle  cylindric internal baffle  shutter Instrument (COROTCAM)  6 lents  Detectors: 4 CCD 2048 x 2048  Radiation shielded  2 CCD seismology, 2 CCD exoplanets  Field of view : 3.05° x 2.70° Optical design

10. 10 OUTLINES OUTLINES THE MISSION The consortium, the persons, the satellite The orbital plane, the observing modes The scientific profiles THE PREPARATORY WORK FOR ASTEROSEISMOLOGY Target selection in the Center and Anticenter directions Target characterisation Future activities

11. 11 Winter : line of sight at 6 h 50 Sun at 90 o from COROT: rotation of the satellite Summer: line of sight at 18 h 50 Orbital parameters a= 7274 km (altitude =896 km) e= 1.27.10 -3 i= 90 o T orb = 6174 sec (1 h 43 min) Orbit Polar orbite, low altitude It allows to maintain the same direction of observation for 6 months without be disturbed by sun light or undergo Earth eclipses

12. 12 The two COROT eyes

13. 13 0 E2 CCD A1CCD E1 CCD E2 CCD A2 0 E1 0 A1 0 A2 3.05° 2.70° Asteroseismology Bright stars 5.5 < V < 9.5 10  in each field Exoplanetary search Faint stars 11.0 < V < 16.5 12 000  in each field Mission life expected : 2.5 y 5 long runs (150 d each) 10 short runs (20 - 30 d) V = 6 --> ~2.5 10 4 photons cm -2 s –1 outside atmosphere, T ~ 6000°K mv = 16 --> ~2.5 photons cm -2 s -1 The observing modes

14. 14 Stellar photometry with a very high accuracy on a long time baseline Seismology : 6 micromag, V=6.0 in 5 days Planetary transits : 0.1 mmag on a V=15.5 star Two scientific goals, simultaneously performed in two adjacent sky regions The communalities Asteroseismology Exoplanet search

15. 15 OUTLINES OUTLINES THE MISSION The consortium, the persons, the satellite The orbital plane, the observing modes The scientific profiles THE PREPARATORY WORK FOR ASTEROSEISMOLOGY Target selection in the Center and Anticenter directions Target characterisation Future activities

16. 16 The Sun Parameters Helium content and core radius, depth of convection zones, internal rotation profile… Asteroseismology Sounding to stellar interiors and physical processes  Frequencies of the oscillation modes (both pression and gravity) on a a wide range of values  photometric precision of 6 ppm (white noise) on a V=6 star in 5 days of continuous monitoring

17. 17 Search for Earth-like planets  detection by means of transits across the disk of parent star  photometric precision around 10 -4 down to V=15.5  Detection criterium : repetitivity (150 d runs)  colour information (3 ‘filters’ available) to disentangle between stellar activity and transits Terre : 10 -4, Jupiter : 10 -2 Exoplanet Search Planets searched by COROT (transits)

18. 18 Exoplanetary CCDs Acquisition  5 000 x 2 windows in 3 colours  40% in red, 30% in blue for a K0 star  1 000 x 2 windows monocromatic  20 imagettes (10x15 pixels) Aperture photometry  Exposure time 16 x 32 s  oversampling on request  ADDITIONAL PROGRAMS Exoplanet search

19. 19 (Butler et al. 2000, ApJ 545, 504) Asteroseismic target. Known to host at least one planet. Visit the site http://media4.obspm.fr/pianeti-extrasolari/ HD 52265

20. 20e Festival d'Astronomie de Haute Maurienne20 E. Michel COROT

21. 21 ADDITIONAL PROGRAMS (seismology in the exoplanetary channel)

22. 22 THE FUTURE OF THE EXOPLANETARY SEARCH

23. 23

24. THE PHOTOMETRIC AND SPECTROSCOPIC MONITORING OF THE COROT TARGETS

25. 25 OUTLINES OUTLINES THE MISSION The consortium, the persons, the satellite The orbital plane, the observing modes The scientific profiles THE PREPARATORY WORK FOR ASTEROSEISMOLOGY Target selection in the Center and Anticenter directions Target characterisation Future activities

26. 26 SUMMARY OF THE PREPARATORY WORK Ground-based observations: high-resolution spectroscopy using FEROS at ESO and SARG at TNG and detailed reductions Solano et al., 2003 (GAUDI ARCHIVE) Identification of new primary targets in the Center direction Poretti et al., 2003 Identification of secondary targets in the AntiCenter direction Poretti et al., 2005 Preliminary asteroseismic characterisation of primary targets (in progress) Target selection in the instability strip is based on the matching between theory and observation. Large experience from ground-based campaigns SPECTROSCOPIC GROUND-BASED CHARACTERISATION OF COROT TARGET Large Programmes at ESO and OHP, complementary runs in other sites

27. GALACTIC CENTER DIRECTION The summer 2002 challenge : find new variables in the Lower Instability Strip for COROT Too few primary targets. Necessity to enlarge the primary targets list. Which stars are actually variable ones ?

28. 28 Challenge won !!! Observations performed mainly at OSN and SPM New targets proposed to the COROT Scientific Committee (December 2002, Corot Week 3)

29. 29 Short list of candidate primary targets in the Center direction Solar like star HD 177552 Gamma Dor star HD 171834 Delta Sct stars HD 181555 * HD 170699 ** Beta Cephei stars HD 170580 ** HD 180642 *

30. 30 ANTICENTER DIRECTION uvby (OSN and SPM) and CCD (STARE) photometry down to V=10.0 around primary targets only RED SQUARES : new DSCT stars OTHER SYMBOLS : constant stars SMALL DOTS : stars far from primary targets

31. 31 OUTLINES OUTLINES THE MISSION The consortium, the persons, the satellite The orbital plane, the observing modes The scientific profiles THE PREPARATORY WORK FOR ASTEROSEISMOLOGY Target selection in the Center and Anticenter directions Target characterisation Future activities

32. THE TARGET CHARACTERISATION: photometry Sierra Nevada Summer 2004 P. Amado and S. Martin S. Pedro Martir Summer 2004 E. Poretti Mt. Piszekesteto September 2004 M. Paparò and coll. Sierra Nevada Winter 2004-05 P. Amado and S. Martin S. Pedro Martir Winter 2004-05 M. Alvarez and E. Poretti APT Winter 2004-05 W.W. Weiss Mercator Summer 2005 C. Aerts and coll. Mt. Piszkesteto Summer 2005 M. Paparò and coll. Sierra Nevada Summer 2005 S. Martin S. Pedro Martir Summer 2005 M. Alvarez S. Pedro Martir Winter 2005-06 E. Poretti, M. Alvarez and STEPHI Sierra Nevada Winter 2005-06 S. Martin and E. Rodriguez Mt. Piszekesteto Winter 2005-06 M. Paparò and coll. S. Pedro Martir November 2006 E. Poretti and K. Uytterhoeven Sierra Nevada Winter 2006-07 E. Rodriguez and S. Martin

33. Positions of the DSCT+GDOR targets in the CMD 1HD 44195 GDOR+DSCT 2HD 181147 DSCT 3HD 50870 DSCT 4HD 170782 DSCT 5HD 170699 DSCT 6HD 44283 DSCT 7HD 172189 EA+SB2+DSCT 8HD 181555 DSCT (revised) 9HD 49434 GDOR 10HD 171834 GDOR 11HD 180642 BCEP 12HD 170580 BCEP (Poretti et al. 2005, AJ 129, 2461)

34. Metallicities, masses and luminosities of the DSCT+GDOR targets 1HD 44195 GDOR+DSCT 2HD 181147 DSCT 3HD 50870 DSCT 4HD 170782 DSCT 5HD 170699 DSCT 6HD 44283 DSCT 7HD 172189 EA+SB2+DSCT 8HD 181555 DSCT 9HD 49434 GDOR 10HD 171834 GDOR Evolutionary tracks calculated by Y. Lebreton and J.C. Suarez. Temperatures and Magnitudes calculated by P. Amado from Stromgren photometry.

35. THE LOWER PART OF THE INSTABILITY STRIP : the DSCT bookmarks Stars in different physical conditions ZAMS : 1 HD 181555 7.98 170 primary target 2 HD 44195 7.57 58 HD43587 UNEVOLVED : 3 HD 181147 8.74 --- HD181555 4 HD 50870 8.86 17 HD52265 5 HD 170782 7.81 197 HD170580 6 HD 170699 6.95 >200 HD170580 ZIGZAGS (TAMS) 7 HD 44283 9.29 19 HD43587 8 HD 172189 8.85 EA HD171834

36. (Poretti, 2000) (Garrido and Poretti 2004) The investigations of Delta Sct stars are of course very preliminary. The frequency detection depend on the S/N. Target selection in the instability strip is based on the matching between theory and observation. Large experience from ground-based campaigns

37. 20e Festival d'Astronomie de Haute Maurienne 37 HD 44195, new DSCT star in the HD 43587 field Power spectrum showing variability at low frequencies (f<5 c/d; GDOR regime ?) and at high frequencies (f>20 c/d; DSCT regime). Unevolved object. Slow rotator : v sin i = 58 km/s PERFECT Delta Sct FOUND Unevolved : no dense frequency spectrum, no mixed modes Slow rotator : a relief for theoreticians, though progresses have been made in the treatment of fast rotators.

38. NOVEMBER 2003 (8 nights)JANUARY 2005 (4 nights) HD 44195, the hybrid GDOR + DSCT star v sin i = 58 km/s, in the field of HD 43587, f 1 =20.48 c/d NOVEMBER 2005 (6 nights) The DSCT variability seems to be monoperiodic, The GDOR variability seems to be multiperiodic

39. 20e Festival d'Astronomie de Haute Maurienne 39 HD 44195 Hybrid variable, just one pulsation at high frequency. Power spectra from Stromgren photometry. Light curves from Mt Piszekesteto Observatory.

40. HD 44283, multiperiodic DSCT variable, small v sin i (19 km/s), evolved (?) 15.00 c/d, predominant mode (ampl. 0.014 mag in v) Second term, f=15.96 c/d, (ampl. 0.005 mag in v ) Asteroseismic peaks around 10 and 20 c/d, (ampl. < 0.003 mag in v)

41. HD 49434, confirmation of the light variability High precision photometry (s.d. better than 0.002 mag) on four consecutive nights. Peak-to-peak amplitudes 0.022 mag in violet 0.019 mag in blue 0.016 mag in yellow Multiperiodicity probable. Observations recently obtained (OSN, SPM and Mt. Piszekesteto) will be decisive to detect periodicities. Additional APT timeseries available.

42. HD 50870, a DSCT star in the field of HD 52265 f 1 =17.15 c/d f 2 =14.00 c/d ………. Slow rotator, V eq sin i = 17 km/s Predominant mode STEPHI campaign in November 2005

43. Field of HD 171834 HD 172189 : DSCT and eclipsing binary in the open cluster IC 4756

44. HD 172189, orbital period has been detected: 5.702 d. Eccentric orbit with only one minimum. DSCT pulsation: frequencies in the 18-20 c/d interval. (Martin et al., 2005, A&A 440, 711) The RV curve has been the goal of successful spectroscopic observations in past summer (OHP, SLN, ESO). Target of a STEPHI campaign in 2004.

45. HD 172189 not only an Eclipsing Binary, but probably also a Spectroscopic Binary (SB2) FEROS spectrum, June 2004

46. HD 181555 – Candidate primary target Fast rotator : Vsin i > 200 Km/s Observed both at OSN and SPM. Evident multiperiodicity: set of frequencies in the 8-11 c/d interval.

47. HD 180642, Beta Cep variable Monitored at SPM and OSN in Stromgren photometry, with Mercator telescope in the Geneva system and and with M. Piszkesteto telescope in V filter Main pulsational frequency term identified as the Fundamental radial mode; additional terms probable (Aerts et al., in preparation)

48. Reminiscent of the case of BW Vul (Sterken and coll.) HD 180642, Mercator and Mt. Piszkesteto light curves in V light BW Vul

49. HD 44195 hybrid HD 43587 f=20.5 c/d f< 5c/d 7.56 F0 58 km/s HD 50870 DSCT HD 52265 f=17.5 13-15 8.88 F0 17 km/s HD 44283 DSCT HD 43587 f=15.0 10-25 9.29 F5 19 km/s HD 181147 DSCT HD 181555 f=15.4 14-17.5 c/d 8.74 A5 98 km/s HD 170782 DSCT HD 170580 13-25 c/d 7.81 A2 197 km/s HD 170699 DSCT HD 170580 10-15 c/d 6.95 A3 >200 km/s HD 172189 DSCT HD 171834 17-19 c/d EA +SB2 8.85 A2 48 and 75 HD 181555 DSCT primary target 8-18 c/d 7.98 A5 170 km/s HD 49434 GDOR photometric variability CONFIRMED 5.75 F1 90 km/s HD 171834 GDOR no photometric variability 5.43 F5 72 km/s HD 180642 BCEP HD 181555 f=5.49 c/d, standstill 8.29 B1 37 km/s HD 170580 BCEP no photometric variability, multiple system 6.68 B2V Target Type Field Frequencies V Sp V sin i

50. 50 OUTLINES OUTLINES THE MISSION The consortium, the persons, the satellite The orbital plane, the observing modes The scientific profiles THE PREPARATORY WORK FOR ASTEROSEISMOLOGY Target selection in the Center and Anticenter directions Target characterisation Future activities

51. Future activities supporting COROT observations Multicolour photometry : OSN, SPM, Mercator, Hungary, APT,… detection of predominant modes and frequency ranges low degree identification by phase shifts & amplitude ratios High resolution spectroscopy : OHP, SLN radial velocity curves characterization of GDOR variables Line Profile Variations for BCEP and DSCT stars

52. The spectroscopic counterpart of the COROT observations FG Vir (Zima et al. 2006)

53. TARGETS FOR COORDINATED GROUND-SPACE OBSERVATIONS Preliminary list (ESO and OHP targets) P78 IR1 P79 LRc1 P80 LRa1 P81 LRc2 HD 50844 DSCT 9.1 HD 180642 BCEP 8.3 HD 49434 GDOR 5.8 1° field HD 181555 DSCT 8.0 HD 50209 Be 8.4 HD 171834 GDOR 5.4 HD 181231 Be 8.6 HD 49330 Be 8.9 HD 172189 DSCT 8.8 2° field SR1 (?) HD 170580 BCEP 6.7 HD 183324 LBOO 5.8 HD 170699 DSCT 6.9 HD 183656 Be 6.1 HD 170782 DSCT 7.8 HD 171219 Be 7.6 SR2 (?) HD 175337 bona-fideGDOR 7.4 HD 174966 DSCT 7.7 HD 174936 DSCT 8.6 A careful planning of the observations (which star at which site) is mandatory. Bright targets can more conveniently observed at Calar Alto.

54. CONCLUSIONS In the past decades we performed a lot of observational efforts to make progress in asteroseismology. All the know-how is now at the service of the COROT mission. In turn, CoRoT is offering us the possibility to improve rapidly our knowledge of stellar interiors. We have the possibility to consign a more mature science to young researchers. We are happy to be in the play, though it is not a simple one. But it’s challenging, and we like that.