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COROT Mission Overview: Scientific Profiles and Observations

Explore the scientific profiles, preparatory work, and international collaboration of the COROT mission for asteroseismology, exoplanetary search, and more.

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COROT Mission Overview: Scientific Profiles and Observations

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

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

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

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

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

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

  8. Optical design 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°

  9. 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

  10. Winter : line of sight at 6 h 50 Sun at 90o from COROT: rotation of the satellite Summer: line of sight at 18 h 50 Orbit Orbital parameters • a = 7274 km (altitude =896 km) • e = 1.27.10-3 • i = 90o • Torb= 6174 sec (1 h 43 min) 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

  11. The two COROT eyes

  12. 0E1 CCD A1 CCD E1 0A1 2.70° 0E2 CCD A2 CCD E2 0A2 3.05° The observing modes 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 --> ~2.5 104 photons cm-2 s –1 outside atmosphere , T ~ 6000°K mv = 16 --> ~2.5 photons cm-2 s -1

  13. The communalities 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 Exoplanet search Asteroseismology

  14. 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

  15. Parameters Helium content and core radius, depth of convection zones, internal rotation profile… The Sun 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

  16. Planets searched by COROT (transits) Exoplanet Search 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

  17. Exoplanet search 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

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

  19. E. Michel COROT

  20. ADDITIONAL PROGRAMS (seismology in the exoplanetary channel)

  21. THE FUTURE OF THE EXOPLANETARY SEARCH

  22. THE PHOTOMETRIC AND SPECTROSCOPIC MONITORING OF THE COROT TARGETS

  23. 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

  24. 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) SPECTROSCOPIC GROUND-BASED CHARACTERISATION OF COROT TARGET Large Programmes at ESO and OHP, complementary runs in other sites Target selection in the instability strip is based on the matching between theory and observation. Large experience from ground-based campaigns

  25. GALACTICCENTER DIRECTIONThe 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 ?

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

  27. 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 *

  28. 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

  29. 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

  30. 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. Aertsand 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

  31. Positions of the DSCT+GDOR targets in the CMD • HD 44195 GDOR+DSCT • HD 181147 DSCT • HD 50870 DSCT • HD 170782 DSCT • HD 170699 DSCT • HD 44283 DSCT • HD 172189 EA+SB2+DSCT • HD 181555 DSCT(revised) • HD 49434 GDOR • HD 171834 GDOR • HD 180642 BCEP • HD 170580 BCEP (Poretti et al. 2005, AJ 129, 2461)

  32. Metallicities, masses and luminosities of the DSCT+GDOR targets • HD 44195 GDOR+DSCT • HD 181147 DSCT • HD 50870 DSCT • HD 170782 DSCT • HD 170699 DSCT • HD 44283 DSCT • HD 172189 EA+SB2+DSCT • HD 181555 DSCT • HD 49434 GDOR • HD 171834 GDOR Evolutionary tracks calculated by Y. Lebreton and J.C. Suarez. Temperatures and Magnitudes calculated by P. Amado from Stromgren photometry.

  33. 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

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

  35. 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.

  36. HD 44195, the hybrid GDOR + DSCT star v sin i = 58 km/s, in the field of HD 43587, f1=20.48 c/d The DSCT variability seems to be monoperiodic, The GDOR variability seems to be multiperiodic NOVEMBER 2003 (8 nights) JANUARY 2005 (4 nights) NOVEMBER 2005 (6 nights)

  37. HD 44195 Hybrid variable, just one pulsation at high frequency. Power spectra from Stromgren photometry. Light curves from Mt Piszekesteto Observatory.

  38. 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)

  39. 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.

  40. HD 50870, a DSCT star in the field of HD 52265 f1=17.15 c/d f2=14.00 c/d ………. Slow rotator, Veq sin i = 17 km/s Predominant mode STEPHI campaign in November 2005

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

  42. 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.

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

  44. 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.

  45. 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)

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

  47. Target Type Field Frequencies V Sp V sin i HD 44195hybridHD 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

  48. 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

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