All Tables

Table 1: Characteristic velocity dispersions ( $\sigma _{U}$ , $\sigma _{V}$ , and $\sigma _{W}$ ) in the thin disk, thick disk, and stellar halo, used in Eq. (1). X is the observed fraction of stars for the populations in the solar neighbourhood and $V_{\rm asym}$ is the asymmetric drift. The values fall within the intervals that are characteristic for the thin and thick disks, see Sect. 1.
Table 2: Stellar parameters for our program stars. The first three columns give the identification of each star, Hipparcos, HD, and HR numbers. The fourth column gives the spectral class as listed in Simbad. The fifth to the seventh columns give V, $\pi$ , and $\sigma _{\pi }$ , all from the Hipparcos catalogue. Columns 8 to 10 give the fundamental parameters, metallicity, effective temperature, and surface gravity that we derive and Col. 11 the microturbulence (see Sect. 5). Column 12 gives the masses that we derive and Col. 13 the bolometric corrections used in Sect. 5.2.3. Columns 14 to 17 list the radial velocities measured by us and the subsequently calculated U, V, and W velocities relative to the local standard of rest (LSR). Columns 18 and 19 give the relative probabilities of the thick disk-to-thin disk and thick disk-to-halo memberships, respectively. The last three columns (20 to 22) give the results of our age determinations, see Sect. 8. In the last column an "s" indicates that Salasnich et al. (2000) isochrones were used when determining the stellar age, a "g" that Girardi et al. (2000) isochrones were used, and an "sg" that the combination of both sets of isochrones were used.
Table 3: Atomic line data. Columns 1 and 2 give the element and the degree of ionization ( $1={\rm neutral}$ , $2= {\rm singly}$ ionized). Column 3 gives the wavelength (in Å), Col. 4 the lower excitation potential (in eV), Col. 5 the correction factor to the classical Unsöld damping constant, and Col. 7 the radiation damping constant. A "S" in Col. 6 indicates that the broadening by collisions have been taken from Anstee & O'Mara (1995), Barklem & O'Mara (1997, 1998), and Barklem et al. (1998, 2000), instead of the classical Unsöld broadening (indicated by an "U"). Column 8 gives our adopted $\log gf$ -values and Col. 9 the references to the original sources. Astrophysical $\log gf$ -values are indicated by "asterisks" in the reference column. The full table is available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/410/527.
Table 4: Solar elemental abundances. Column 1 indicate the elements and ions and Cols. 2 and 3 give the meteoritic and solar photospheric standard abundances from Grevesse & Sauval (1998). Our solar abundances are given in Cols. 4 and 5 gives the differences between this study and the photospheric values. Asterisks indicate that we have used astrophysical $\log gf$ -values and thereby forced the abundance to the standard photospheric value. Asterisks in parenthesis indicate that some of the lines have astrophysical $\log gf$ -values.
Table 5: Estimates of the effects on the derived abundances due to internal (random) errors for four stars. When calculating $\Delta W_{\lambda }/\sqrt {N}$ we have assumed $\Delta W_{\lambda } = 5\%$ for Hip 88622, Hip 3142, and Hip 118115, and $\Delta W_{\lambda } = 10\%$ for Hip 103682, see Sect. 7.1.1. The total random errors ( $\sigma _{\rm rand}$ ) were calculated assuming the individual errors to be uncorrelated. The final line gives the average of the total random error for the four stars.
Table 6: Derived abundances relative hydrogen, [X/H], where X denotes the different elements as indicated. Each element has three columns, mean abundance ([X/H]), standard deviation of the mean abundance ( $\sigma _{\rm [X/H]}$ ), and the number of spectra lines (N) that has been used in computing the mean abundance. The abundances have been normalized with respect to the solar photospheric abundances as given in Grevesse & Sauval (1998), see also Table 4. The second column indicates if the star belongs to the thin disk ( ${\rm mem=1}$ ) or the thick disk ( ${\rm mem}=2$ ) ( ${\rm mem=3}$ indicates the Sun). The full table is available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/410/527.