Content of the CorotSky Content of the CorotSky DatabaseDatabase

S. Charpinet (LA)S. Charpinet (LA)J. Platzer (LA)J. Platzer (LA)J. Cuvilo (CESR)J. Cuvilo (CESR)E. Bourrec (LA)E. Bourrec (LA)G. Vauclair (LA)G. Vauclair (LA)D. ToublancD. Toublanc (CESR)(CESR)

What is behind CorotSky ?What is behind CorotSky ?

Objectives of CorotSky :Objectives of CorotSky : – Simulate Simulate thethe sky visible by COROT sky visible by COROT

in both seismology and exoplanet in both seismology and exoplanet channelschannels

– Provide specific informations on Provide specific informations on potential targets in both channelspotential targets in both channels

– Provide overall informations Provide overall informations (histograms, HR diagrams, …) (histograms, HR diagrams, …)

Optimization of: Optimization of: • Target/Field-of-View selection Target/Field-of-View selection • Global planification of observations Global planification of observations

The database behind CorotSky The database behind CorotSky →→See the document « Content description of the See the document « Content description of the CorotSky asteroseismology database » available CorotSky asteroseismology database » available (soon) from the Corotsky web page :(soon) from the Corotsky web page : http://smsc.cnes.fr/COROT/A_corotsky.htmhttp://smsc.cnes.fr/COROT/A_corotsky.htm

CorotSky

SeismologyDatabase

Exoplanet SearchDatabase

• 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:The Seismology Database:Data From CataloguesData From Catalogues

The Core of the Database :The Core of the Database : – Contains all the stars referenced Contains all the stars referenced

in the CDS/SIMBAD database : in the CDS/SIMBAD database : Brighter than V=9.5Brighter than V=9.5 Within the 15° cones around the Within the 15° cones around the

Center / Anticentre directions Center / Anticentre directions (Scenario 4)(Scenario 4)

11,911 stars11,911 stars

Parameters from Catalogues :Parameters from Catalogues :– Main sources: Simbad / HipparcosMain sources: Simbad / Hipparcos– Values, errors, sourcesValues, errors, sources

ParameterParameter SourceSource

IdentifiersIdentifiers SIMBADSIMBAD

RA (2000)RA (2000) SIMBADSIMBAD

DEC (2000)DEC (2000) SIMBADSIMBAD

VV SIMBADSIMBAD

B-VB-V SIMBAD/HIPSIMBAD/HIP

Spectral TypeSpectral Type SIMBADSIMBAD

Proper MotionProper Motion SIMBADSIMBAD

ParallaxParallax HIPPARCOSHIPPARCOS

VradVrad SIMBAD/GBOSIMBAD/GBO

Teff

Mv

The Seismology Database: The Seismology Database: Data from Ground Based ObservationsData from Ground Based Observations

Stromgren photometry : Stromgren photometry : – Observations at Obs. of Sierra NevadaObservations at Obs. of Sierra Nevada

(R. Garrido et al.)(R. Garrido et al.)– Stars V ≤ 8 (~ 1000 objects; Scenario 4)Stars V ≤ 8 (~ 1000 objects; Scenario 4)– Photometric data available from the Photometric data available from the

GAUDI database (E. Solano; LAEFF)GAUDI database (E. Solano; LAEFF)

High resolution spectroscopy :High resolution spectroscopy :– Observations at/with OHP/ELODIE, Observations at/with OHP/ELODIE,

LaSilla/FEROS, TNG/SARG, …LaSilla/FEROS, TNG/SARG, …

(C. Catala, E. Poretti et al.)(C. Catala, E. Poretti et al.)– Stars V ≤ 8 (~ 1000 objects; Scenario 4) Stars V ≤ 8 (~ 1000 objects; Scenario 4) – Spectra available from the GAUDI Spectra available from the GAUDI

database (E. Solano; LAEFF)database (E. Solano; LAEFF)

Templogg Templogg MMvv, Teff, log g, [Fe/H] , Teff, log g, [Fe/H]

(R. Garrido, W. Weiss et al.)(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: The Seismology Database: Adopted Teff, Mv, log g & [Fe/H]Adopted Teff, Mv, log g & [Fe/H]

PP MethodMethod Conditions Conditions / / CommentsComments SourceSource

11 LiteratureLiterature Only for a few starsOnly for a few stars C. SoubiranC. Soubiran

22 Parallax > 10 masParallax > 10 mas ππ > 10 mas > 10 mas S. Charpinet/Hip. CatalogS. Charpinet/Hip. Catalog

33 Stromgren/TemploggStromgren/Templogg mmV V ≤ 8≤ 8 R. Garrido, W. Weiss et al.R. Garrido, W. Weiss et al.

44 Spectroscopy/TgmetSpectroscopy/TgmetmmV V ≤ 8; Teff ≤ 8,000 K; ≤ 8; Teff ≤ 8,000 K;

V sin i ≤ 30 km/sV sin i ≤ 30 km/s

C. Catala, E. Poretti, C. Catala, E. Poretti,

C. SoubiranC. Soubiran

55 Parallax Parallax ≤ 10 mas≤ 10 mas 3 mas 3 mas ≤ ≤ ππ ≤ 10 mas ≤ 10 mas S. Charpinet/Hip. CatalogS. Charpinet/Hip. Catalog

66 Parallax DefaultParallax Default ππ < 3 mas or no value < 3 mas or no value S. Charpinet/Hip. CatalogS. Charpinet/Hip. Catalog

MV Adopted

PP MethodMethod Conditions Conditions / / CommentsComments SourceSource

11 Detailed analysisDetailed analysis Only for a few starsOnly for a few stars P. Magain et al.P. Magain et al.

22 HH line wings line wings 5500 K 5500 K ≤ Teff ≤ 8500 K≤ Teff ≤ 8500 K C. Van’t Veer et al.C. Van’t Veer et al.

33 LiteratureLiterature Only for a few starsOnly for a few stars C. SoubiranC. Soubiran

44 Stromgren/TemploggStromgren/Templogg mmV V ≤ 8≤ 8 R. Garrido, W. Weiss et al.R. Garrido, W. Weiss et al.

55 Spectroscopy/TgmetSpectroscopy/TgmetmmV V ≤ 8; Teff ≤ 8,000 K; ≤ 8; Teff ≤ 8,000 K;

V sin i ≤ 30 km/sV sin i ≤ 30 km/s

C. Catala, E. Poretti, C. Catala, E. Poretti,

C. SoubiranC. Soubiran

66 V-I/AllenV-I/Allen Not yet availableNot yet available

77 B-V/AllenB-V/Allen Almost all starsAlmost all stars S. CharpinetS. Charpinet

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.

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

[Fe/H] Adopted

PP MethodMethod Conditions Conditions / / CommentsComments SourceSource

11 Detailed analysisDetailed analysis Only for a few starsOnly for a few stars P. Magain et al.P. Magain et al.

22 MgMgI tripletI triplet Not yet implementedNot yet implemented

33 LiteratureLiterature Only for a few starsOnly for a few stars C. SoubiranC. Soubiran

44 Stromgren/TemploggStromgren/Templogg mmV V ≤ 8≤ 8 R. Garrido, W. Weiss et al.R. Garrido, W. Weiss et al.

55 Spectroscopy/TgmetSpectroscopy/TgmetmmV V ≤ 8; Teff ≤ 8,000 K; ≤ 8; Teff ≤ 8,000 K;

V sin i ≤ 30 km/sV sin i ≤ 30 km/s

C. Catala, E. Poretti, C. Catala, E. Poretti,

C. SoubiranC. Soubiran

log g Adopted

PP MethodMethod Conditions Conditions / / CommentsComments SourceSource

11 Detailed analysisDetailed analysis Only for a few starsOnly for a few stars P. Magain et al.P. Magain et al.

22 LiteratureLiterature Only for a few starsOnly for a few stars C. SoubiranC. Soubiran

33 Stromgren/TemploggStromgren/Templogg mmV V ≤ 8≤ 8 R. Garrido, W. Weiss et al.R. Garrido, W. Weiss et al.

44 Spectroscopy/TgmetSpectroscopy/TgmetmmV V ≤ 8; Teff ≤ 8,000 K; ≤ 8; Teff ≤ 8,000 K;

V sin i ≤ 30 km/sV sin i ≤ 30 km/s

C. Catala, E. Poretti, C. Catala, E. Poretti,

C. SoubiranC. Soubiran

The Seismology Database: The Seismology Database: Star Type CataloguesStar Type Catalogues

Stars of specific interest :Stars of specific interest : – Primary candidatesPrimary candidates– Variable starsVariable stars– Peculiar starsPeculiar stars– …… Catalogues that define star types Catalogues that define star types

in the databasein the database

Current status :Current status :– Implementation of the VISAT Implementation of the VISAT

catalogues (Obs. Vienna; W. Weiss catalogues (Obs. Vienna; W. Weiss et al.) for the seismology channelet al.) for the seismology channel

28 referenced startypes28 referenced startypes Star types in the exoplanet channel Star types in the exoplanet channel

are not yet implementedare not yet implemented

What Do We Need to Complete the What Do We Need to Complete the Seismology Database ?Seismology Database ?

1. Lists of star types :1. Lists of star types :

What: Add missing startypes What: Add missing startypes Check catalogue contents Check catalogue contents Startypes in the Exo Startypes in the Exo fieldsfields

Who: Each scientist (GI?) is Who: Each scientist (GI?) is resp. for the catalogue resp. for the catalogue she/he has providedshe/he has provided

Contact: W. WeissContact: W. Weiss

2. Mv and Teff values :2. Mv and Teff values :

Prob: ~75% of the database, Mv Prob: ~75% of the database, Mv relies on the « Parallax by relies on the « Parallax by Default » method…Default » method…

About the same fraction About the same fraction relies on Teff values relies on Teff values coming from a B-V/Teff coming from a B-V/Teff conversion (Allen)…conversion (Allen)…

What: Include V-IWhat: Include V-I

Results from spectroscopy Results from spectroscopy

Additional Ground Based Additional Ground Based photometry/spectroscopy?photometry/spectroscopy?

Who: Who:

Contact: C. Catala Contact: C. Catala

3. What else ?3. What else ?

- Include spectrophotometry- Include spectrophotometry

- Improve Teff, logg, [Fe/H] using - Improve Teff, logg, [Fe/H] using

better calibrations for photometrybetter calibrations for photometry

and spectrocopyand spectrocopy

Contact: Caroline Soubiran Contact: Caroline Soubiran

Database updates :Database updates :

Who: The OMP CorotSky TeamWho: The OMP CorotSky Team

When: Every month or so…When: Every month or so…