J/A+A/469/309    Chromospheric activity in late-type stars   (Cincunegui+, 2007)
Hα and the CaII H and K lines as activity proxies for late-type stars.
    Cincunegui C., Diaz R.F., Mauas P.J.D.
   <Astron. Astrophys., 469, 309-317 (2007)>
   =2007A&A...469..309C 2007A&A...469..309C
ADC_Keywords: Stars, late-type ; Spectroscopy
Keywords: stars: late-type - stars: activity - stars: chromospheres
Abstract:
    The main chromospheric activity indicator is the S index, which is 
    the ratio of the flux in the core of the CaII H and K lines to the
    continuum nearby, and is well studied for stars from F to K. Another
    chromospheric proxy is the Halpha line, which is believed to be
    tightly correlated with the CaII index.
    In this work we characterize both chromospheric activity indicators,
    the one associated with the H and K CaII lines and the other with
    Halpha, for the whole range of late type stars, from F to M.
Description:
    We present periodic medium-resolution echelle observations covering
    the complete visual range, taken at the CASLEO Argentinean Observatory
    over 7 years. We use a total of 917 flux-calibrated spectra for 109
    stars that range from F6 to M5. We statistically study these two
    indicators for stars of different activity levels and spectral types.
File Summary:
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 FileName   Lrecl  Records   Explanations
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ReadMe         80        .   This file
table2.dat    127      109   Stars included in the sample
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See also:
    J/A+A/331/581  : Rotation and activity in field M dwarfs (Delfosse+ 1998)
    J/A+AS/124/359 : CaII triplet lines in cool stars (Mallik 1997)
Byte-by-byte Description of file: table2.dat
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   Bytes Format Units   Label    Explanations
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   1-  9  A9    ---     Name     HD or GJ name
  11- 16  A6    ---     GJ       GJ or Gliese designation
  18- 32  A15   ---     OName    Other name
  33- 36  A4    ---     Note     Notes (1)
  38- 45  A8    ---     SpType   MK spectral type
  47- 52  F6.3  mag     Vmag     V magnitude
  54- 58  F5.3  mag     B-V      B-V colour index
      60  A1    ---   n_B-V      [a] a: photometry from Simbad, else from
                                     HIP (Cat. I/239)
  62- 67  F6.2  mas     plx      ?=- Parallax
      69  A1    ---   n_plx      [b] b: parallax from Simbad, else from
                                     Jenkins (1952, UCTP, Cat. I/81)
  70- 74  F5.2  ---     logg     ?=- Gravity surface
      76  A1    ---   l_[Fe/H]   Limit flag on [Fe/H]
  77- 81  F5.2 [Sun]    [Fe/H]   ?=- Metallicity
      83  A1    ---   n_[Fe/H]   [c] c: logg and [Fe/H] from Cayrel de Strobel
                                 et al. (2001, Cat. III/221), else from
                                 Cayrel de Strobel et al. (1997, Cat. III/200)
      85  A1    ---   l_Prot     Limit flag on Prot
  86- 90  F5.2  d       Prot     ?=- Rotational period
      92  A1    ---   r_Prot     [edfghiZz] Reference for Prot (2)
  94- 95  I2    ---     Nobs     Number of observations
  97-100  F4.2  ---           Mean activity index (in Mount Wilson units)
 102-107  F6.2 hW/m2/nm     Average surface flux in CaII HK line (4)
     109  A1    ---     ---      [(] FHa excluded from our analysis (3)
 110-114  F5.2 kW/m2/nm <FHa>    Average flux in Halpha line (4)
     115  A1    ---     ---      [)] FHa excluded from our analysis (3)
 117-121  F5.2  ---     m        ?=- Slope of the linear regression between
                                 F(Halpha) and F(HK) for the individual spectra
                                 of each star
 123-127  F5.2  ---     rho      ?=- Correlation coefficient corresponding to m
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Note (1): Notes as follows:
     *  = stars with planets
     +  = RS CVn type
     ++ = BY Dra type
     S  = stars reported in CTIO as non-variable, which were used to
          calibrate the S indices
     t  = dMe stars, or stars presumably active
Note (2): Prot references as follows:
      e = Baliunas et al. (1996ApJ...457L..99B 1996ApJ...457L..99B),
      d = Saar & Osten (1997MNRAS.284..803S 1997MNRAS.284..803S),
      f = Noyes et al. (1984ApJ...279..763N 1984ApJ...279..763N),
      g = Saar et al. (1990A&A...235..291S 1990A&A...235..291S),
      h = Hooten & Hall (1990ApJS...74..225H 1990ApJS...74..225H)
      i = Pettersen (1989AetA...209..279P).
      Z = periods estimated from vsini using Glebocki & Stawikowski
          (2000AcA....50..509G 2000AcA....50..509G)
      z = periods estimated from vsini using Reiners & Schmitt
          (2003A&A...398..647R 2003A&A...398..647R).
Note (3): The Halpha fluxes between parentheses were excluded from our
     analysis in Section 4.1, since they might be subject to larger errors
     due to the use of B-V as a proxy for Teff for stars with B-V≤1.4.
Note (4): CaII flux in 104erg/cm2/s/Å, and 
          Hα flux in 105erg/cm2/s/Å.
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History:
    From electronic version of the journal
(End)                                      Patricia Vannier [CDS]    26-Oct-2007