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1
Seismology Ground-Based Observation Working
Group PROGRESS REPORT CW5 Berlin, December
2003
2
Photometric target characterization(R. Garrido
et al.)

• observations complete uvbyH??CaII HK
• stars mV8 for scenario 4 12
• Teff, log g, Fe/H determination complete
  templogg
• data available in GAUDI database (LAEFF)
• Teff, log g, Fe/H inserted in COROTSKY

done
3
Status of spectroscopic observationsstars mV
8 in scenario 4(E. Poretti, C. Catala, L.
Mantegazza, W. Weiss, )

• all stars with mV 8 in COROT eyes observed
  (OHP, FEROS, SARG, )
• OHP and FEROS data reduced and included in GAUDI
  database
• OHP spectra analyzed with tgmet Teff, logg,
  Fe/H
• OHP spectra used for Teff determination using Ha
  line wings
• OHP and FEROS spectra analyzed for Vrad, vsini,
  SB2 detection
• SARG data (almost) reduced (Vienna Coralie
  Neiner)

done
lt CW6
4
Detailed analysis of primary targets(P. Magain,
H. Bruntt,)

• on going work by several groups with different
  methods
• provides accurate and reliable (?) Teff, log g,
  abundances
• BUT, methods rely on model atmospheres which
  cannot be
• trusted blindly be cautious (cf F.
  Kupka)
• need to analyze new primary candidate targets
• - HD 46558
• - HD 52265
• - HD 175726
• - HD 177552
• - HD 181555
• - HD 171234

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Corotsky strategy for Teff and MV
determination(S. Charpinet et al.)
Teff Adopted

• for stars mV gt 8, we rely only on B-V
• include IR photometry for Teff determination (I.
  Ribas)
• use existing data (GAUDI Stromgren V 2MASS)

MV Adopted

• for most stars mV gt 8, we have nothing to rely
  only on
• need for more photometric - spectroscopic -
  spectrophotometric data?

6
New observations?(stars mV 9.5 in COROT eyes)

• proposed strategy
• 1. select CCD position/orientation based on mV
  8 stars exofield AP targets
• identify stars with mV 9.5 falling on the
  seismology CCDs
• 33 stars per principal target lt 500 stars
  altogether
• Stromgren photometry 2 x 2-3 weeks (add stars
  around fov when
• duration 1 year CCD position not
  constrained)
• high resolution spectroscopy 2 x 2 nights on
  4m telescope (CFH, TNG)
• duration 1 year
• spectrophotometry collaboration ASTRA?
• collaboration Catania, Bangalore?
• obs 1 (anticenter) 2004B analysis 1 2005B
• obs 2 (center) 2005A analysis 2 2006A

7
Spectroscopic/photometric database GAUDI(E.
Solano)

• operational
• photometric data complete
• spectroscopic data almost complete
• stellar parameters soon included
• need to ingest new data
• (e.g. spectroscopic/photometric monitoring)
• homogeneize and standardize reduction and format

database becoming public in January 2004
! http//ines.laeff.esa.es/corot/
8
Ca II H K monitoring(G. Cutispoto, I. Pagano,
)

• on going work at Catania Observatory
• goal measure activity level and rotation
  period
• most main targets have been monitored
• no variability of S index down to 0.01 for
  monitored targets
• is it necessary to continue monitoring for these
  targets?
• yes if precision can be improved
• no if not
• BUT need to include new primary candidate targets

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That's all, folks !
10
Spectroscopic observations(stars mV 8 out of
scenario 4)

• drift 4 degrees increase 20 in number of
  potential targets 200 stars
• Stromgren observations 2 weeks - duration 1 year
• high resolution spectroscopy 4 to 5 nights on
  FEROS ?
• 30 nights OHP ?
• duration 1 year
• schedule obs 1 2004B obs 2 2005A analysis
  2006A