1. CW9 - Asteroseismology with HARPS 1 Observations with HARPS Benoît Mosser Obs. Paris, LESIA François Bouchy LAM/OHP/IAP benoit.mosser@obspm.fr

2. CW9 - Asteroseismology with HARPS 2 Asteroseismology with HARPS HARPS Photon noise limited performances (according to Bouchy et al 2001) HARPS at ESO 3.6-m telescope, 5 nights, mV = 4, duty cycle = 33% ‘’SNR’’ of observable targets

3. CW9 - Asteroseismology with HARPS 3 Observations and results HD 49933 COROT 6th magnitude Target Mosser et al 2005 F6V, mV = 5.8 - stellar activity / seismic signal - large separation and amplitude - eigenfrequency pattern, modelling in progress  Ara Exoplanet hosting star Bouchy et al 2005 ; Bazot et al 2005 G3IV-V, mV = 5.1 - 43 identified eigenfrequencies - 2 possible models: primordial overmetallicity / enrichment during the planetary formation  Hydri  CenA G2IV, mV = 3.2 G2V, mV = 0.0 … HARPS

4. CW9 - Asteroseismology with HARPS 4 Time allocation / strategy HARPS Pressure on ES0 3.6-m : 7 - 10 About 1 asteroseismic programme is selected each semester, with 6 - 8 nights allocated HARPS is unique, limited to single site measurement High gain in sensitivety No gain in duty cyle

5. CW9 - Asteroseismology with HARPS 5 Further observations HARPS Single site asteroseismic observations For precise scientific programs with a high potential scientific return…not focussed on precise determination of eigenfrequencies Networking with SOPHIE at OHP (> summer 2006) Possible network, for ~ 14 hours / day Limited to bright targets with –10° <  < +20° As UVES (VLT Chili) + UCLES (AAT Australia) SONG network project SIAMOIS project at Dome C in Antarctica Acompagnying COROT observations Simultaneous observations - monitoring the stellar activity (high SNR ; limited observing time) - radial velocity time series