1 / 17

The Doppler follow-up of COROT transit candidates

The Doppler follow-up of COROT transit candidates. F. Bouchy Laboratoire d’Astrophysique de Marseille. Corot Week 8 – 23/27 May 2005. Review of the Doppler follow-up of OGLE transit candidates. Follow-up of 60 candidates 56 hours with FLAMES . 137 transit candidates

ryder
Download Presentation

The Doppler follow-up of COROT transit candidates

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. The Doppler follow-up of COROT transit candidates F. Bouchy Laboratoire d’Astrophysique de Marseille Corot Week 8 – 23/27 May 2005

  2. Review of the Doppler follow-up of OGLE transit candidates Follow-up of 60 candidates 56 hours with FLAMES 137 transit candidates in bulge and carina field 1.30-m telescope (Las Campanas)

  3. The Zoo of the radial velocity follow-up eclipsing M-dwarfs [24] grazing EB [5] Multiple systems [12] Falses positives [7] Unsolved cases [7] Bouchy et al., 2005, A&A, 431, 1105 Pont et al., 2005, A&A, in press (astro-ph/0501615)

  4. Strategy of Doppler follow-up Step 0 – Careful analysis of light curve  shape, contrast, duration, periodicity, ellipsoidal modulation  color information  other informations (EXODAT)

  5. Strategy of Doppler follow-up Step 1 - One spectroscopic measurement  SB2  vsini / synchronization  spectral type  RV uncertainty (photon noise)

  6. Strategy of Doppler follow-up Step 2a - Two Doppler measurements at T0-P/4 and T0+P/4  SB1  not in phase with expected transit  no variation Step 2b - Two Doppler measurements at T0–DT/2 and T0+DT/2  Rossiter effect (in case of large vsini and long P)

  7. Mass characterization Step 3 – Make a choice :  Stop follow-up  repeat step 2 with a higher precision spectrograph  Re-analyze of the light curve  Start other follow-up (HAR photometry / …)  Start mass characterization

  8. CES 2m Tautenburg CORALIE 1.2m La Silla SOPHIE 1.93m OHP HARPS 3.6m La Silla FLAMES 8.2m Paranal

  9. CORALIE 1 hour - mv=12 - 15 m/s 1 hour - mv=14 - 40 m/s 1.0 ± 0.2 MJupiter - 10 days - G0  K= 95 ± 19 m/s mv=12  1.5 hour mv=14  9 hours ~ 1 nights 20 nights/semester already allocated for COROT Available for an immediate follow-up Pre-selection of the SOPHIE and/or HARPS targets But limited to bright targets

  10. CES - Tautenburg 1 hour - mv=12 - 50 m/s 1.0 ± 0.2 MJupiter - 10 days - G0  K= 95 ± 19 m/s mv=12  14 hours ~ 2 nights ? nights/semester allocated for COROT Available for an immediate follow-up Pre-selection of the SOPHIE and/or HARPS targets But limited to bright targets

  11. SOPHIE 1 hour - mv=12 - 4 m/s 1 hour - mv=14 - 12 m/s 1 hour - mv=16 - 45 m/s 0.5 ± 0.1 MJupiter - 10 days - G0  K= 47 ± 9 m/s mv=12  1 hour mv=14  4 hours mv=16  50 hours ~ 6 nights 20 nights/semester allocated for COROT Available for an immediate follow-up Mass characterization of hot Jupiters Pre-selection of the HARPS targets

  12. FLAMES + UVES 1 hour - mv=14 - 6 m/s (25 m/s in practice) 1 hour - mv=16 - 15 m/s (30 m/s in practice) 0.5 ± 0.1 MJupiter – 10 days - G0  K= 47 ± 9 m/s mv=14  15 heures ~ 2 nights (for 7 targets) mv=16  22 heures ~ 3 nights (for 7 targets) Software improvement  push systematics bellow 25 m/s Follow-up of ambiguous cases and fainter stars Mass characterization of hot Jupiters Pre-selection of the HARPS targets

  13. HARPS 1 hour - mv=12 - 2 m/s 1 hour - mv=14 - 6 m/s 1 hour - mv=16 - 20 m/s (30 m/s in practice) 15 m/s (with High Efficiency Mode) 20 ± 4 Mearth – 10 days - G0  K= 6.0 ± 1.2 m/s mv=12  6 hours mv=14  50 hours ~ 6 nights 10 nights/semester already allocated for COROT Available for an immediate follow-up Dedicate for high precision mass characterization of confirmed planets (hot Neptune)

  14. Semester telescope’s need Expected detections 1 – 10 MJ [~ 2 transits] 0.1 – 1 MJ [~ 20 transits] 10 – 30 Mearth [~ 6 transits] EB + BEB [~ 100 cases ?] First confirmation : 20 nights CORALIE (160 measurements) 10 nights SOPHIE (80 measurements) ? nights CES Tautenburg Precise mass characterization : 10 nights SOPHIE (80 measurements) 10 nights HARPS (80 measurements) + ESO Proposals ? Ambiguous cases : 7 nights FLAMES (400 measurements)

  15. Schedule

More Related