Chair : M. Deleuil

3.5º Main target m v  6 Secondary targets m v < 9 Exoplanet field 2.8º N Focal plane:

Targets selection Criteria:  Scientific: - Favourite: late type dwarves  Instrumental: - the shape of the PSF changes as a function of:  Environmental: - crowding effects  the location of the stars on the CCD  star’s colors  star’s magnitude A0 F0 G2 K2 M MagnitudeSpectral type

Targets selection Criteria:  Scientific: - Favourite: late type dwarves  Instrumental: - the shape of the PSF changes as a function of:  Environmental: - crowding effects  the location of the stars on the CCD  star’s colors  star’s magnitude

HD : Potential main target for the astero. program Exoplanet domain ~20 

Long runs: (~ 20 □ )  ~ stars with m v < 16  ~ stars with m v < 16 UBVRI Photometry - since 2001 UBVRI Photometry - since INT/La Palma : 24 nights INT/La Palma : 24 nights Will be complete at the end 2005 Will be complete at the end CFHT/12K  a few deep exposures in R filter in order to characterize background stars. - CFHT/12K  a few deep exposures in R filter in order to characterize background stars. Catalogues:  Used for the spectral classification  will be used for the targets selection for short runs  DENIS/2Mass  USNO-A2  Hipparcos/Tycho

 Archive the ground-based observations  Cross-correlate these data with existing catalogues  Perform the spectral classification  Validate algorithms: - allocation of the best photometric mask - estimate the contamination for each potential target  Prepare the scientific analysis  Validate the data provided to CoRotSky for the Exoplanet channel

1) Dwarf / Giant sorting : Ground – based observations cross-correlated with 2Mass and/or DENIS data Ground – based observations cross-correlated with 2Mass and/or DENIS data

i < 16 AND V-i < 1.0 i 1.0 i V-i MS Giants HD field Giants Main Seq. V - i i

1) Dwarf / Giant sorting : From ground – based observations cross-correlated with 2Mass and/or DENIS data From ground – based observations cross-correlated with 2Mass and/or DENIS data  luminosity class – good level of confidence for stars brighter than 15 in R  luminosity class – good level of confidence for stars brighter than 15 in R 2) UBVRIJHK data compared with SEDs from a spectral library : Estimate of the spectral type of each star – the 3 “best” solutions are saved. Potential binarity is included.

 density of stars with R ≤ 15: ~ 6000 (HD ) % overlapping : ~ 30%  4200 potential targets / deg 2 i.e potential targets per CCD  density of stars with R ≤ 15: ~ 3100 (HD 49434) % overlapping : ~ 20%  2480 potential targets / deg 2 i.e potential targets per CCD

 GIRAFFE/VLT : observations Dec 2004 & Jan 2005 (Guaranteed time + Open time)  A.M. Hubert on monday  VIMOS/VLT  V. Repipi on tuesday  Brazilian observational facilities  discussion on tuesday Goal : for stars with m v < 15 check & improve the spectral classification identify binaries derive stellar parameters: T eff, logg, vsini.. identify hot Jupiter in COROT fields 

BEST (H. Rauer ) monitoring of the Exo-fields (m v < 14.5) 1 or 2 field per season Interest : binaries identification variable stars identification Geneva system (C. Aerts ) Goal : classification of variable stars BUT FOV 6.5’x6.5’ ! Interest and feasibility to be demonstrated (next CW) (F. Favata ) Interest: stellar activity, identify young stars.. (under study)   

α, δ + error mag_U+err mag_B+err mag_V+errmag_R+err mag_I+err mag_J+err mag_H+errmag_K+err Colors Images Spect. type Lum. class Binarity Broad Band Photom. Spect. Classif. Soft. Spect. type Logg, vsini, Radius, metal... Spectroscopic obs. Variability, X-rays.. Ground Surveys + Add Prog. α,δ + error mag_R … Background m V > 16 m v < 11 Contamination Mask design catalogues Contamination CoRoTSky

α,δ + error mag_R Background m V > 16 m v < 11 catalogues α,δ + error mag_B+err mag_V+err mag_R+err mag_I+err Contamination Spect. Type Lum. Class Binarity V_min/V_max + star type Star type = information from add. programs

Necessary in order to  remove ambiguities,  better characterize the nature of the detected planet  derive accurate spectral parameters of the parent star.

 SOPHIE – 1.93m OHP/France Fiber-fed cross-dispersed Echelle spectrograph 1 st commissioning by the end of m/s in 1 hour for m v = 12.5  2m TLS - TAUTENBOURG Germany  Remove ambiguities  HR Spectrocopy of the parent star  Characterization of all the companions with masses  Jupiter  Filter the targets for HARPS and UVES+FLAMES

 HARPS – 3.6m La Silla 3 – 30 M  (10 M  AU - G0 - mv=14) 50 nights already allocated in HARPS guaranteed time Possibility to follow-up immediately a detected transit Additional nights  ESO proposals  UVES+FLAMES – 8.2m Paranal 0.1 – 1 M Jup (0.3 M Jup AU - G0 - mv=16) ESO proposal  ~ 12 months of delay…

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