1. Solar-like oscillations with HARPS …and SOPHIE
F. Bouchy
Laboratoire d’Astrophysique de Marseille
COROT week 8 – May 2005

2. ~ 3 magnitudes more efficient
HARPS
Fiber-fed cross-dispersed Echelle spectrograph
Wavelength coverage: 380nm < l < 690nm
Simultaneous reference (ThAr)
Spectral resolution: R=100’000
Vacuum operation, T-control
~ 3 magnitudes more efficient
than ELODIE/CORALIE

3. Doppler uncertainty due to photon noise
magnitude
1 m/s
20 cm/s 3
6.3
(S/Npix = 500)
K G F
For a non-rotating K5 dwarf

4.  Cen B observed with HARPS
RMS = 51 cm/s

5.  Cen B observed with HARPS
2.9 cm/s
2.3 cm/s
19 cm/s
160 Hz

6. Bouchy et al., 2004, Nature, 423(7015), 2

7. Other HARPS results

8. All stars are singing

9. Bouchy et al, 2005, A&A, in press (astroph/0504043)
HD G3IV-V - mv=5.1
noise 4.5 cm/s
Bouchy et al, 2005, A&A, in press (astroph/ )
Bazot et al., 2005, A&A, in press (astroph/???)

10. Mosser, et al., 2005, A&A, 431, L13

11. Expected capability of HARPS on some main COROT targets
Name mV
Spe. type
v sin i
(km/s)
dVRMS
for 1 mn exp.
anoise
10 nights
HD43587
5.7
F9V 6
1.4 m/s
5.5 cm/s
HD49933
5.8
F5V 10
3.1 m/s
12.2 cm/s
HD52265
6.3
G0V 4
1.3 m/s
5.1 cm/s

12. SOPHIE New spectrograph on the 1.93-m OHP  end of 2005
North counter part of HARPS
~ 2 magn. more efficient than ELODIE
but 1.5 magn. less efficient than HARPS

13. Photon noise uncertainties
(K5V - vsini=2 km/s - texp=1 mn)
ELODIE
1.9-m OHP
SOPHIE
1.9-m OHP
HARPS
3.6-m ESO

14. Complementarity COROT / HARPS
On solar-like stars :
Help and constrain modes identification
Doppler amplitude
Give eventually higher angular modes (l=3)
Give the possibility to find line profil deformation
due to higher angular degree or activity
Povide huge number of high S/N spectra