Table 2: Derived stellar atmosphere parameters and elemental abundances for the sample. The entire table is available only electronically. This portion of the table is given as a guide to its form. For each star we report the average signal-to-noise ratio per pixel for the whole observed spectrum, the stellar parameters with their respective relative and absolute rms error estimates, $\sigma ^{\rm rel}$ and $\sigma ^{\rm abs}$, then for each element X the abundance $\log \epsilon_{\rm X}$ and its relative and absolute rms error estimates $\sigma_{\log\epsilon_{\rm X}}$, [X/Fe] and its relative and absolute rms error estimates $\sigma _{\rm [X/Fe]}$. N gives the number of features of the element used in each star, noting that this varies from star to star as certain features may be automatically rejected if the star has a strong G band, if the feature is near a Balmer line in warmer stars (see Sect. 3.2), or if they are determined to be affected by a cosmic ray hit or bad pixel. N3 then gives the number of those features classified as 3$\sigma $ detections. In the case of CH bands we simply classify detections and non-detections with 1 and 0 respectively. In the case of a non-detection, this is signified by an abundance of -9.99 and error of 0.00.
Star $S/N_{\rm av}$ $T_{\rm eff}$ $\sigma_{T_{\rm eff}}$ $\log g$ $\sigma_{\log g}^{\rm rel}$ $\sigma_{\log g}^{\rm abs}$ [Fe/H] $\sigma_{\rm [Fe/H]}^{\rm rel}$ $\sigma_{\rm [Fe/H]}^{\rm abs}$ $\xi $ $\sigma_\xi^{\rm rel}$ $\sigma_\xi^{\rm abs}$ $\log\epsilon_{\rm C}$ $\sigma_{\log\epsilon_{\rm C}}^{\rm rel}$ $\sigma_{\log\epsilon_{\rm C}}^{\rm abs}$ [C/Fe] $\sigma_{\rm [C/Fe]}^{\rm rel}$ $\sigma_{\rm [C/Fe]}^{\rm abs}$ N N3 ...
    [K]   [cm s-2]           [km s-1]                     ...
CS 22175-007 31 5108 100 2.46 0.26 0.36 -2.81 0.13 0.18 1.67 0.14 0.24 5.77 0.19 0.26 0.19 0.18 0.27 1 1 $\ldots$
CS 22186-023 55 5066 100 2.19 0.24 0.34 -2.72 0.13 0.18 1.58 0.11 0.21 5.97 0.19 0.25 0.30 0.18 0.27 1 1 $\ldots$
CS 22186-025 32 4985 100 1.70 0.26 0.36 -2.87 0.14 0.19 2.14 0.13 0.23 4.83 0.20 0.27 -0.68 0.19 0.29 1 1 $\ldots$
CS 22886-042 39 4881 100 1.85 0.25 0.35 -2.68 0.12 0.18 1.84 0.12 0.22 5.72 0.19 0.26 0.01 0.19 0.28 1 1 $\ldots$
CS 22892-052 46 4884 100 1.81 0.26 0.36 -2.95 0.14 0.19 1.67 0.12 0.22 6.44 0.19 0.26 1.00 0.18 0.28 1 1 $\ldots$
CS 22945-028 31 5126 100 2.55 0.26 0.36 -2.66 0.13 0.18 1.53 0.14 0.24 5.93 0.19 0.26 0.21 0.18 0.27 1 1 $\ldots$
CS 22957-013 35 4904 100 1.96 0.25 0.35 -2.64 0.14 0.19 1.79 0.12 0.22 5.85 0.19 0.26 0.10 0.17 0.27 1 1 $\ldots$
CS 22958-083 32 5101 100 2.40 0.26 0.36 -2.79 0.12 0.18 1.50 0.13 0.23 6.24 0.20 0.26 0.64 0.18 0.27 1 1 $\ldots$
CS 22960-010 35 5737 100 4.85 0.25 0.35 -2.65 0.12 0.17 1.53 0.17 0.27 6.56 0.17 0.24 0.82 0.16 0.25 1 1 $\ldots$
CS 29491-069 57 5103 100 2.45 0.24 0.34 -2.81 0.13 0.18 1.54 0.12 0.22 5.76 0.19 0.25 0.18 0.17 0.27 1 1 $\ldots$
$\vdots$ $\vdots$ $\vdots$ $\vdots$ $\vdots$ $\vdots$ $\vdots$ $\vdots$ $\vdots$ $\vdots$ $\vdots$ $\vdots$ $\vdots$ $\vdots$ $\vdots$ $\vdots$ $\vdots$ $\vdots$ $\vdots$ $\vdots$ $\vdots$ $\ldots$
HE 2338-1618 40 5515 100 3.38 0.27 0.37 -2.65 0.12 0.18 1.43 0.16 0.26 6.22 0.18 0.25 0.47 0.18 0.27 1 1 $\ldots$
HE 2345-1919 44 5617 100 4.46 0.25 0.35 -2.46 0.12 0.18 1.47 0.16 0.26 6.17 0.19 0.24 0.24 0.17 0.26 1 1 $\ldots$
HE 2347-1254 80 6132 100 3.95 0.24 0.34 -1.83 0.13 0.18 1.67 0.12 0.22 6.83 0.15 0.22 0.27 0.16 0.26 1 1 $\ldots$
HE 2347-1334 81 4453 100 0.95 0.24 0.34 -2.55 0.12 0.19 2.38 0.11 0.21 5.33 0.21 0.26 -0.50 0.18 0.27 1 1 $\ldots$
HE 2347-1448 43 6162 100 3.98 0.27 0.37 -2.31 0.12 0.18 0.84 0.17 0.27 6.58 0.18 0.24 0.50 0.19 0.27 1 1 $\ldots$


Source LaTeX | All tables | In the text

Article Contents
1 Introduction
2 Observations and sample
3 Automated spectrum analysis
4 Results
5 Discussion
6 Conclusions
References
Online Material
Appendix A: Line list
Appendix B: Error estimates
List of tables
List of figures