Astronomy & Astrophysics

All Tables

Table 1: Kinematical data for the new stellar sample. Column 1 gives the Hipparcos number; Col. 2 gives the radial velocities (as measured by us); Cols. 3-5 give the space velocities relative to the local standard of rest; Cols. 6 and 7 give the calculated ${\it TD}/D$ and ${\it TD}/H$ ratios. The radial velocity for HIP 116740 have been taken from Barbier-Brossat et al. (1994).
Table 2: Wavelength coverage for the different spectral orders (SO) for the two settings (Blue and Red) of the CCD.
Table 3: Our program stars. Columns 1-3 give the identifications for each star, Hipparcos, HD, and HR numbers; Col. 4 gives the spectral class as listed in the SIMBAD database; Cols. 5-7 give V magnitude, parallax ( $\pi$ ), and accuracy of the parallax ( $\sigma _{\pi }$ ), all from the Hipparcos catalogue; Cols. 8-10 give the stellar atmospheric parameters, metallicity ([Fe/H]), effective temperature ( $T_{\rm eff}$ ), and surface gravity ( $\log g$ ); Col. 11 gives the microturbulence ( $\xi _{\rm t}$ ); Col. 12 gives the stellar mass ( $\mathcal{M}$ ); Col. 13 the bolometric correction (BV). The last column indicates which instrument was used to obtain the spectrum.
Table 4: Atomic line data. Column 1 gives the element; Col. 2 the wavelength, Col. 3 the lower excitation potential; Col. 4 the correction factor to the classical Unsöld damping constant; Col. 5 indicates if the broadening by collisions have been taken from Anstee et al. (1995), Barklem & O'Mara (1997, 1998), and Barklem et al. (1998, 2000) (indicated by an "S") instead of the classical Unsöld broadening (indicated by an "U"). Column 6 gives the radiation damping constant; Col. 7 gives the $\log gf$ -values; Col. 8 gives the references for the $\log gf$ -values. The full table is available in electronic form at the CDS.
Table 5: Elemental abundances from the solar analysis. The first column gives the element and degree of ionization. An asterisk in the second column indicates that the $\log gf$ -values for these lines are astrophysical (originating from Bensby et al. 2003), and an asterisk within parenthesis that a part of the lines have astrophysical $\log gf$ -values. In the lower part of the table, Col. 2 is used to indicate the wavelength of the spectral line. The third column gives the standard solar photospheric abundance as given in Grevesse & Sauval (1998). Columns 4-6 give our solar analysis based on the FEROS spectra (see Bensby et al. 2003), Cols. 7-9 our solar analysis based on the SOFIN spectra, and Cols. 10-12 our solar analysis based on the UVES spectra. For each study we give the number of lines that were analyzed ( $N_{\rm lines}$ ), the mean abundance from these lines ( $\epsilon (X)$ ), and the difference (Diff.) compared to the standard photospheric value in Col. 3.
Table 6: Estimates of the effects on the derived abundance ratios due to internal (random) errors. The estimates are the average of four stars (see Bensby et al. 2003).
Table 7: Metallicities and $\alpha$ -enhancements for the Y² isochrones that were used in the age determination.
Table 8: Age estimates for the stars in this study and those in Bensby et al. (2003). The minimum (Min age) and maximum (Max age) ages are based on the uncertainties in the Hipparcos parallaxes and $\pm 70$ K in the effective temperatures. The full table is available in electronic form at the CDS.
Table 9: Derived abundances relative to hydrogen. Each element has three columns, mean abundance ([X/H]), standard deviation of the mean abundance ( $\sigma _{\rm [X/H]}$ ), and the number of spectral lines ( $N_{\rm X}$ ) that were used in the abundance analysis (Cols. 4 and onwards). The abundances have been normalized with respect to the Sun (see Sect. 5.1 and Table 5). Column 1 gives the Hipparcos number; Col. 2 indicates with which spectrograph the star was observed (S = SOFIN, F = FEROS, U = UVES); Col. 3 indicates if the star belongs to the thin disk (Mem. = 1), the thick disk (Mem. = 2), or a "transition object'' (Mem. = 3). The full table is available in electronic form at the CDS.
Table 10: Abundances for deviating stars. Each star has three columns; abundance; line-to-line scatter (1 $\sigma$ standard deviation); and (in parenthesis) number of lines that were used to derive the abundance.
Table A.1: Characteristic velocity dispersions ( $\sigma _{\rm U}$ , $\sigma _{\rm V}$ , and $\sigma _{\rm W}$ ) in the thin disk, thick disk, and stellar halo, used in Eq. (A.1). $V_{\rm asym}$ is the asymmetric drift.
Table A.2: The number of stars in given ${\it TD}/D$ intervals for different values on the local density of thick disk stars ( $X_{\rm TD}$ ). The second column indicates the factor by which the ${\it TD}/D$ ratios change when varying the normalization (with the 10% density as base). The corresponding CM-diagrams can be seen in Fig. A.2.