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

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 Target/Field-of-View selection Global planification of observations 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 : 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 (c.f. poster describing the graphical application CorotSky) (The tool CorotSky is being developped by GMV and is the Spanish contribution to COROT)

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 ParameterSourceIdentifiersSIMBAD RA (2000) SIMBAD DEC (2000) SIMBAD VSIMBAD B-VSIMBAD/HIP Spectral Type SIMBAD Proper Motion SIMBAD ParallaxHIPPARCOS VradSIMBAD/GBO Teff MvMv

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 M v, 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] H  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

The Seismology Database: Adopted Teff, Mv, log g & [Fe/H] PMethod Conditions / Comments Source1Literature Only for a few stars C. Soubiran 2 Parallax > 10 mas π > 10 mas S. Charpinet/Hip. Catalog 3Stromgren/Templogg m V ≤ 8 R. Garrido, W. Weiss et al. 4Spectroscopy/Tgmet m V ≤ 8; Teff ≤ 8,000 K; V sin i ≤ 30 km/s C. Catala, E. Poretti, C. Soubiran 5 Parallax ≤ 10 mas 3 mas ≤ π ≤ 10 mas S. Charpinet/Hip. Catalog 6 Parallax Default π < 3 mas or no value S. Charpinet/Hip. Catalog M V AdoptedPMethod Conditions / Comments Source1 Detailed analysis Only for a few stars P. Magain et al. 2 H  line wings 5500 K ≤ Teff ≤ 8500 K C. Van’t Veer et al. 3Literature Only for a few stars C. Soubiran 4Stromgren/Templogg m V ≤ 8 R. Garrido, W. Weiss et al. 5Spectroscopy/Tgmet m V ≤ 8; Teff ≤ 8,000 K; V sin i ≤ 30 km/s C. Catala, E. Poretti, C. Soubiran 6V-I/Allen Not yet available 7B-V/Allen Almost all stars S. Charpinet T eff 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.

The Seismology Database: Adopted Teff, Mv, log g & [Fe/H] [Fe/H] AdoptedPMethod Conditions / Comments Source1 Detailed analysis Only for a few stars P. Magain et al. 2 MgI triplet Not yet implemented 3Literature Only for a few stars C. Soubiran 4Stromgren/Templogg m V ≤ 8 R. Garrido, W. Weiss et al. 5Spectroscopy/Tgmet m V ≤ 8; Teff ≤ 8,000 K; V sin i ≤ 30 km/s C. Catala, E. Poretti, C. Soubiran log g AdoptedPMethod Conditions / Comments Source1 Detailed analysis Only for a few stars P. Magain et al. 2Literature Only for a few stars C. Soubiran 3Stromgren/Templogg m V ≤ 8 R. Garrido, W. Weiss et al. 4Spectroscopy/Tgmet m V ≤ 8; Teff ≤ 8,000 K; V sin i ≤ 30 km/s C. Catala, E. Poretti, C. Soubiran

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

What Do We Need to Complete the Seismology Database ? 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 Database updates : Who: The OMP CorotSky Team When: Every month or so…