All Tables

Table 1: Log of the UVES observations. The S/N ratio per pixel is given for three representative wavelengths. (Due to the large number of pixels in each resolution element, the S/N ratios of the table need to be multiplied by a factor of 1.3 in order to compare them to the values available in the literature).
Table 2: Precise coordinates of the BPS programme stars. Four of our stars have duplicate names. The second name is given in italics. The coordinates of the HD and BD stars of our sample can be found in SIMBAD.
Table 3: Parameters and equivalent widths of the lines. In the first raw of the table is given the number of the star (from 1 to 35, see Table 1 for the corresponding name). This table is available in its entirety at the CDS.
Table 4: Photometry and derived temperatures for the programme stars. The V-I and V-R colours are on the Johnson system, while J-K and V-K have been transformed to the TCS system (see Alonso et al. 2001).
Table 5: Adopted model parameters ( $T_{{\rm eff}}$ , log g, $v_ {{\rm t}}$ , [Fe/H]_m) and final iron abundances [Fe/H] $_{\rm c}$ for the programme stars.
Table 6: Abundance uncertainties linked to stellar parameters. Case of the cool star HD 122563.
Table 7: Abundance uncertainties linked to stellar parameters. Case of the "warm" star CS 22948-066.
Table 8: Abundances of the elements in the stars. Here is a sample of the table which is available in electronic form for all the 35 stars at the CDS. Note that Na Al and K are NOT corrected for non-LTE effects (see Sect. 4.4.1 for corrections) and that O is computed with 1D models.
Table 9: Coefficients of the adopted regression lines. In Cols. 2 and 3 are given the coefficients a and b of the relation [X/Fe] = a [Fe/H] + b. In Col. 4 is given the scatter measured in the total interval, and in Cols. 5 and 6 the scatter in two different intervals of metallicity. Column 7 lists an estimate of the scatter expected from measurement errors only. For some elements the total scatter is hardly larger than the expected error.
Table 10: Mean [X/Mg] ratios for stars with [Mg/H]<-2.9, corresponding to the yields of the first supernovae. The r.m.s. is the scatter around the mean.