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J/A+A/394/927   Age-metallicity relation for nearby stars     (Ibukiyama+, 2002)
HIPPARCOS age-metallicity relation of the solar neighbourhood disc stars.
     Ibukiyama A., Arimoto N.
    <Astron. Astrophys. 394, 927 (2002)>
    =2002A&A...394..927I
ADC_Keywords: Milky Way ; Stars, nearby ; Abundances ; Stars, distances ;
              Stars, ages

Keywords : stars: abundances - stars : distances - Galaxy: abundances -
           Galaxy : evolution - Galaxy: solar neighbourhood -
           Galaxy: kinematics and dynamics

Description:
    Ages, Fe and Ca abundances, orbits, and populations for 1658 solar
    neighbourhood stars are presented. Stars are selected from Hipparcos
    (Cat. II/239 Catalogue.

File Summary:

       FileName      Lrecl  Records   Explanations

ReadMe            80        .   This file
table2.dat        68      493   Stars with spectroscopic [Fe/H]
table3.dat        68     1165   Stars with photometric [Fe/H]


See also:
     I/239 : The Hipparcos and Tycho Catalogues (ESA 1997)


Byte-by-byte Description of file: table2.dat

   Bytes Format Units   Label    Explanations

   1- 11  A11   ---     Name     Star name
  13- 24  A12   ---     SpType   MK Spectrum type
  26- 30  F5.2  [Sun]   [Fe/H]   Metallicty [Fe/H] (G2)
  32- 36  F5.2  [Sun]   [Ca/Fe]  ? [Ca/Fe] abundance (G3)
  39- 43  F5.2  Gyr     Age      ? Age
  45- 50  F6.2  kpc     R        ? Galactocentric mean distance
  53- 56  F4.2  ---     ecc      Orbital eccentricity
  58- 62  F5.2  kpc     zmax     Maximum deviation from the Galactic plane
  64- 68  A5    ---     Pop      Population (G1)


Byte-by-byte Description of file: table3.dat

   Bytes Format  Units   Label     Explanations

   1- 11  A11    ---     Name      Star name
  13- 24  A12    ---     SpType    MK spectrum type
  26- 30  F5.2   [Sun]   [Fe/H]    Metallicty [Fe/H] (G2)
  39- 43  F5.2   Gyr     Age       ? Age
  45- 50  F6.2   kpc     R         ? Galactocentric mean distance
  53- 56  F4.2   ---     ecc       Orbital eccentricity
  58- 62  F5.2   kpc     zmax      Maximum deviation from the Galactic plane
  64- 68  A5     ---     Pop       Population (G1)


Global notes:

Note (G1): Populations are designated:
     halo: star of the halo
     thin: star of the thin disk
    thick: star of the thick disk
Note (G2):
    [Fe/H] are taken from the spectroscopic data by Cayrel de Strobel et
    al. (2001, Cat. III/221) or derived from the photometric data by
    Hauck & Mermilliod (1998, Cat. II/215).

    [Ca/Fe] are taken from:
      Boesgaard & Tripicco (1986ApJ...303..724B),
      Smith & Lambert (1986ApJ...303..226S),
      Smith & Lambert (1987MNRAS.226..563S),
      Hartmann & Gehren (1988A&A...199..269H),
      Abia et al. (1988A&A...206..100A), Magain (1989A&A...209..211M),
      Cayrel & Bentolila (1989A&A...211..324C),
      Gratton & Sneden (1991A&A...241..501G),
      Berthet (1991A&A...251..171B),
      Edvardsson et al. (1993, Cat. J/A+A/275/101),
      Pilachowski et al. (1993ApJ...407..699P),
      Smith et al.  (1993ApJ...417..287S),
      Nissen et al. (1994A&A...285..440N),
      Beveridge & Sneden (1994AJ....108..285B),
      Nissen & Schuster (1997, Cat. J/A+A/326/751),
      Tomkin et al. (1997, Cat. J/A+A/327/587),
      Carney et al. (1997AJ....114..363C),
      Castro et al. (1997, Cat. III/200),
      Giridhar et al. (1997PASP..109.1077G),
      Gonzalez (1998A&A...334..221G),
      Feltzing & Gustafsson (1998, Cat. J/A+AS/129/237),
      King et al. (1998AJ....115..666K),
      Jehin et al. (1999A&A...341..241J),
      Clementini et al. (1999MNRAS.302...22C),
      Sadakane et al. (1999PASJ...51..505S),
      Santos et al. (2000A&A...363..228S),
      Thoren & Feltzing (2000A&A...363..692T),
      Chen et al. (2000, Cat. J/A+AS/141/491),
      Gonzalez & Laws (2000AJ....119..390G),
      Fulbright (2000AJ....120.1841F).
Note (G3): Ages are derived by using Isochrones by Yi et al.
    (2001ApJS..136..417Y) based on colour magnitude diagrams derived by
    Hipparcos Catalogue. Orbital parameters are calculated numerically by
    using a four-component Miyamoto-Nagai potential model (Sofue,
    1996ApJ...458..120S). We identified the populations of stars by using
    their rotational velocities with respect to the Galaxy centre.


Acknowledgements: Ibukiyama Akihiko 

(End)   Akihiko Ibukiyama [Tokyo Univ., Japan], Patricia Bauer [CDS] 08-Nov-2002