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Content of the CorotSky Database

Content of the CorotSky Database. S. Charpinet (LA) J. Platzer (LA) J. Cuvilo (CESR) E. Bourrec (LA) G. Vauclair (LA) D. Toublanc (CESR). Stars brighter than V=9.5 Centre/Anticentre directions ~12,000 stars Large amount of data from catalogs and dedicated GBO

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Content of the CorotSky Database

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  1. Content of the CorotSky Database S. Charpinet (LA) J. Platzer (LA) J. Cuvilo (CESR) E. Bourrec (LA) G. Vauclair (LA) D. Toublanc (CESR)

  2. Stars brighter than V=9.5 • Centre/Anticentre directions • ~12,000 stars • Large amount of data from catalogs and dedicated GBO • Mostly Implemented • Stars with 12 ≤ V ≤ 16 • Centre/Anticentre directions • ~10,000,000 stars from cat. • BVRI data + identification for ~3,000,000 stars from GBO around principal targets • Under construction What is behind CorotSky ? Objectives of CorotSky : • Simulate the sky visible by COROT in both seismology and exoplanet channels • Provide specific informations on potential targets in both channels • Provide overall informations (histograms, HR diagrams, …) • Optimization of: • Target/Field-of-View selection • Global planification of observations The database behind CorotSky → See the document « Content description of the CorotSky asteroseismology database » available (soon) from the Corotsky web page : http://smsc.cnes.fr/COROT/A_corotsky.htm (c.f. poster describing the graphical application CorotSky) (The tool CorotSky is being developped by GMV and is the Spanish contribution to COROT)

  3. The Seismology Database:Data From Catalogues The Core of the Database : • Contains all the stars referenced in the CDS/SIMBAD database : • Brighter than V=9.5 • Within the 15° cones around the Center / Anticentre directions (Scenario 4) • 11,911 stars Parameters from Catalogues : • Main sources: Simbad / Hipparcos • Values, errors, sources Teff Mv

  4. The Seismology Database: Data from Ground Based Observations Stromgren photometry : • Observations at Obs. of Sierra Nevada (R. Garrido et al.) • Stars V ≤ 8 (~ 1000 objects; Scenario 4) • Photometric data available from the GAUDI database (E. Solano; LAEFF) High resolution spectroscopy : • Observations at/with OHP/ELODIE, LaSilla/FEROS, TNG/SARG, … (C. Catala, E. Poretti et al.) • Stars V ≤ 8 (~ 1000 objects; Scenario 4) • Spectra available from the GAUDI database (E. Solano; LAEFF) Templogg Mv, Teff, log g, [Fe/H] (R. Garrido, W. Weiss et al.) Tgmet (C.Soubiran) Mv, Teff, log g, [Fe/H] (OHP, FEROS?, SARG?) Detailed Analysis (P. Magain et al.) Teff, log g, [Fe/H] Ha line wings (C. Van’t Veer) Teff (OHP, FEROS?, SARG?) LSD (C. Catala) Vrad, Vsin i, SB2 (OHP, FEROS, SARG?) if Vsin i > 200 km/s (A.-M. Hubert) Vsin i

  5. The Seismology Database: Adopted Teff, Mv, log g & [Fe/H] Teff Adopted For each star in the database, a value is adopted for the folloqing parameters according to the data available and by order of priority (P) of the method used for the determination. MV Adopted

  6. The Seismology Database: Adopted Teff, Mv, log g & [Fe/H] log g Adopted [Fe/H] Adopted

  7. The Seismology Database: Star Type Catalogues Stars of specific interest : • Primary candidates • Variable stars • Peculiar stars • … • Catalogues that define star types in the database Current status : • Implementation of the VISAT catalogues (Obs. Vienna; W. Weiss et al.) for the seismology channel • 28 referenced startypes • Star types in the exoplanet channel are not yet implemented

  8. What Do We Need to Complete the Seismology Database ? Database updates : Who: The OMP CorotSky Team When: Every month or so… 1. Lists of star types : What: Add missing startypes Check catalogue contents Startypes in the Exo fields Who: Each scientist (GI?) is resp. for the catalogue she/he has provided Contact: W. Weiss 2. Mv and Teff values : Prob: ~75% of the database, Mv relies on the « Parallax by Default » method… About the same fraction relies on Teff values coming from a B-V/Teff conversion (Allen)… What: Include V-I Results from spectroscopy Additional Ground Based photometry/spectroscopy? Who: Contact: C. Catala 3. What else ? - Include spectrophotometry - Improve Teff, logg, [Fe/H] using better calibrations for photometry and spectrocopy Contact: Caroline Soubiran

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