All Tables

Table 1: The sample. The entire table is available only electronically. Coordinates of the HES stars (prefix HE) have been derived from the Digitized Sky Survey I and are accurate to 1 $^{\prime \prime }$ ; the coordinates of the HK survey stars (prefix CS) are from identifications of the sources in the 2MASS All Sky Release. Barycentric radial velocities $v_{\rm rad}$ were measured from the snapshot spectra and are accurate to a few km s^-1.
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.
Table 3: Comparison of our final stellar parameters with those adopted in the literature for the comparison stars. $T_{\rm eff}$ derived with the reddening maps of Burstein & Heiles (1982) instead of Schlegel et al. (1998) are also given for comparison.
Table 4: Comparison of results for CS 31082-001 using spectra with degraded S/N. The difference from our results using the original spectrum $S/N\approx 90$ in Table 2 is quoted, with the relative error in the derived abundance for the degraded S/N in parentheses. A blank means a non-detection (below 3 $\sigma$ ) at this S/N for this star.
Table 5: New r-II and s-II objects. Quoted error estimates are relative errors. N3 is defined in the caption to Table 2.
Table 6: Comparison of measured scatter in Figs. 17 and 18 with relative errors in the abundance ratios. For each plot we report the minimum, mean and maximum measured $1\sigma$ scatter $\sigma _{\rm meas}$ across the range of [Fe/H] or [Mg/H], which is compared to the average relative error in the abundance ratio $\sigma ^{\rm rel}$ . The ratio of the mean measured scatter to the estimated error $\langle \sigma_{\rm meas} \rangle /\sigma^{\rm rel}$ is reported in the last column.
Table A.1: Molecular line data for A-X system of the CH molecule near 4310 Å from Plez & Jorissen. The spectral windows employed for this molecular band are defined with respect to an arbitrary $\lambda$ and span from $\lambda +d\lambda _{\rm blue}$ to $\lambda +d\lambda _{\rm red}$ .
Table A.2: Molecular line data for A-X system of the CH molecule near 4363 Å from Plez & Jorissen. The spectral window employed for this molecular band is defined with respect to two arbitrary wavelengths $\lambda$ and span from $\lambda +d\lambda _{\rm blue}$ to $\lambda +d\lambda _{\rm red}$ .
Table A.3: Data for atomic lines for species lighter than Fe. The spectral window employed for the line is from $\lambda +{\rm d}\lambda _{\rm blue}$ to $\lambda +{\rm d}\lambda _{\rm red}$ . Lines which are removed in carbon-enhanced stars are marked with asterisks in the wavelength column.
Table A.4: Data for atomic lines of Fe. The spectral window employed for the line is from $\lambda +{\rm d}\lambda _{\rm blue}$ to $\lambda +{\rm d}\lambda _{\rm red}$ . Lines which are removed in carbon-enhanced stars are marked with asterisks in the wavelength column.
Table A.5: Data for atomic lines of species heavier than Fe. The spectral window employed for the line is from $\lambda +{\rm d}\lambda _{\rm blue}$ to $\lambda +{\rm d}\lambda _{\rm red}$ . Lines which are removed in carbon-enhanced stars are marked with asterisks in the wavelength column.
Table B.1: Assigned average values of $\sigma_{\log gf}$ for each element.
Full version
Table 1: Coordinates of the HES stars (prefix HE) have been derived from the Digitized Sky Survey I and are accurate to 1 $^{\prime \prime }$ ; the coordinates of the HK survey stars (prefix CS) are from identifications of the sources in the 2MASS All Sky Release. Barycentric radial velocities $v_{\rm rad}$ were measured from the snapshot spectra and are accurate to a few km s^-1.
Table 2: Derived stellar atmosphere parameters and elemental abundances for the sample. 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 r.m.s. error estimates, $\sigma^\mathrm{rel}$ and $\sigma^\mathrm{abs}$ , then for each element X the abundance $\log \epsilon_\mathrm{X}$ and its relative and absolute r.m.s. error estimates $\sigma_{\log\epsilon_\mathrm{X}}$ , [X/Fe] and its relative and absolute r.m.s. error estimates $\sigma_\mathrm{[X/Fe]}$ . 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.