Presentation on theme: "Radial Velocity follow-up of SWASP-North candidates with SOPHIE (1.93-m OHP) G. Hébrard & F. Bouchy (IAP/OHP)"— Presentation transcript:
Radial Velocity follow-up of SWASP-North candidates with SOPHIE (1.93-m OHP) G. Hébrard & F. Bouchy (IAP/OHP)
July 2006: telescope integration Aug 2006: first light
- Fiber fed cross-dispersed echelle spectrograph - Res = 40’000 (H.E.) = 75’000 (H.R.) - 2k x 4k EEV 15 m pixel CCD - 387-694 nm (39 orders) - two pairs of 3’’ optical fibers - gain of 10 in efficiency / ELODIE - present precision of 4-5 m/s in H.R. Perruchot. Kohler, Bouchy, et al. 2008 Bouchy, Hébrard, Udry, et al. 2010
mv RV [m/s] in 1 hour (H.E.) vsini < 2 km/svsini ~ 5 km/svsini ~ 10 km/s 1248 1361218 14153045 Photon noise uncertainties + 10-15 m/s of systematic in H.E. mode
1 - CCD Charge Transfer Inefficiency function of flux level at low S/N (Bouchy et al. 2008) Correction of systematic effects
2 - Seeing effect due to imperfect fiber scrambling effect (Boisse et al. 2010) Correction of systematic effects
3 - Moon light contamination Correction of systematic effects
Blended Eclipsing Binaries (inside seeing) Deep inspection of CCFs Bisector Span Amplitude change With CCF template
Reprocessing of all SOPHIE data in our IAP database: - moon light correction - computation of CCFs with F0, G2 and K5 masks - Bisector span computation - Complete listing of all observations
SOPHIE ++ ADC telescope 1 1 2 1 New N2 Dewar filling system + thermal isolation improvement 2 2 New Fiber scambling New Calibration Unit
Expected end of optimisation phase : mid 2011 Expected accuracy ~ 1-2 m/s Developpement of AstrAcad : an automatic 50-cm telescope for photometric follow-up (2012)
Goals : establish the true nature of transiting events characterize the true mass of secure planets determine central star parameters Main Actors : G. Hébrard, F. Bouchy (IAP/OHP) C. Moutou (LAM) / Udry (Geneva) B. Loeillet (IAP/LAM - 2006-2009) I. Boisse (IAP - 2010) A.Santerne (LAM -2011-2012) Cameron, Pollacco, Skillen, Barros, Faedi (WASP) SWASP-North follow-up with SOPHIE
WASP-11 3.7 days/ 0.5 M Jup West et al. (2009) WASP-12 1.9 day / 1.4 M Jup Hebb et al. (2009) WASP-14 2.2 days / 7.3 M Jup Joshi et al. (2009) WASP-3 1.8 day / 1.8 M Jup Pollacco et al. (2008) WASP-1 2.5 days / 0.9 M Jup Cameron et al. (2007) WASP-2 2.1 days / 0.9 M Jup Cameron et al. (2007) WASP-21 4.3 days / 0.3 M Jup Bouchy et al. (2010) WASP-13 4.4 days / 0.5 M Jup Skillen et al. (2009) Published SuperWASP planets with SOPHIE RVs WASP-10 3.1 days / 3.0 M Jup Christian et al. (2009)
New SuperWASP planets with SOPHIE RVs WASP-37 3.6 days / 1.7 M Jup Simpson et al.
New SuperWASP planets with SOPHIE RVs WASP-38 6.9 days / 2.7 M Jup Barros et al.
New SuperWASP planets with SOPHIE RVs WASP-39 4.1 days / 0.3 M Jup Faedi et al.
New SuperWASP planets with SOPHIE RVs WASP-40 3.0 days / 0.6 M Jup West et al. Another planet? CaII emission: active star
New SuperWASP planets with SOPHIE RVs? 2.1 days / 0.7 M Jup
WASP-3 SOPHIE WASP-3b = 15° (+10°/-9°) Simpson et al. (2010) Miller et al. (submitted)
``French’’ team involved : G. Hébrard, F. Bouchy (OHP) C. Moutou, A. Santerne (LAM) - Close to the instrument - In charge of the observations - In charge of the upgrade & optimization of instrument - In charge of the Data Reduction Software - Close interaction with observers in case of service mode
Means to optimize SWASP-North follow-up - Increase Nb nights (Opticon + French applications) (5.7 + 4 = 9.7 nights in 2010B) - Large flexibilities with other Large programs CoRoT (PI: C. Moutou) SOPHIE consortium (PI: F. Bouchy) 9.7 SWASP nights spread over all the semester - One identified RV responsible in close contact with one identified SWASP responsible for each semester - Better coordination with other facilities (FIES and Coralie)
Proposed Schedule for 2010B 15 - 20 Oct [5 nights] 4 nights SWASP 8 - 13 Nov [5 nights] 3.5 nights SWASP + 2.2 nights spread over the semester Observers : G. Hébrard, F. Bouchy, A. Santerne, & C. Moutou and some others SOPHIE consortium observers (service mode).