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 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 68 493 Stars with spectroscopic [Fe/H]
table3.dat 68 1165 Stars with photometric [Fe/H]
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See also:
I/239 : The Hipparcos and Tycho Catalogues (ESA 1997)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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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)
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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)
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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 1986ApJ...303..724B),
Smith & Lambert (1986ApJ...303..226S 1986ApJ...303..226S),
Smith & Lambert (1987MNRAS.226..563S 1987MNRAS.226..563S),
Hartmann & Gehren (1988A&A...199..269H 1988A&A...199..269H),
Abia et al. (1988A&A...206..100A 1988A&A...206..100A), Magain (1989A&A...209..211M 1989A&A...209..211M),
Cayrel & Bentolila (1989A&A...211..324C 1989A&A...211..324C),
Gratton & Sneden (1991A&A...241..501G 1991A&A...241..501G),
Berthet (1991A&A...251..171B 1991A&A...251..171B),
Edvardsson et al. (1993, Cat. J/A+A/275/101),
Pilachowski et al. (1993ApJ...407..699P 1993ApJ...407..699P),
Smith et al. (1993ApJ...417..287S 1993ApJ...417..287S),
Nissen et al. (1994A&A...285..440N 1994A&A...285..440N),
Beveridge & Sneden (1994AJ....108..285B 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 1997AJ....114..363C),
Castro et al. (1997, Cat. III/200),
Giridhar et al. (1997PASP..109.1077G 1997PASP..109.1077G),
Gonzalez (1998A&A...334..221G 1998A&A...334..221G),
Feltzing & Gustafsson (1998, Cat. J/A+AS/129/237),
King et al. (1998AJ....115..666K 1998AJ....115..666K),
Jehin et al. (1999A&A...341..241J 1999A&A...341..241J),
Clementini et al. (1999MNRAS.302...22C 1999MNRAS.302...22C),
Sadakane et al. (1999PASJ...51..505S 1999PASJ...51..505S),
Santos et al. (2000A&A...363..228S 2000A&A...363..228S),
Thoren & Feltzing (2000A&A...363..692T 2000A&A...363..692T),
Chen et al. (2000, Cat. J/A+AS/141/491),
Gonzalez & Laws (2000AJ....119..390G 2000AJ....119..390G),
Fulbright (2000AJ....120.1841F 2000AJ....120.1841F).
Note (G3): Ages are derived by using Isochrones by Yi et al.
(2001ApJS..136..417Y 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 1996ApJ...458..120S). We identified the populations of stars by using
their rotational velocities with respect to the Galaxy centre.
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Acknowledgements: Ibukiyama Akihiko
(End) Akihiko Ibukiyama [Tokyo Univ., Japan], Patricia Bauer [CDS] 08-Nov-2002