\begin{table}%t2
\par
\caption{The measured equivalent widths $W_{\lambda}$ ({in m\AA})
for the \Ci~ and \Oi~ features detected in the 15 newly observed
halo stars used in this study, together with the {\it S/N} near the
features of interest. \label{fabt:eqwidths}}
%\centerline
 {\begin{tabular}{cccccccccccccc}
\hline \hline
  & C~{\sc i} & C~{\sc i} & C~{\sc i} & C~{\sc i} & C~{\sc i} & C~{\sc i} & & C~{\sc i} &
  & O~{\sc i} & O~{\sc i} & O~{\sc i} & \\
  & $\lambda 9061.4$ & $\lambda 9062.5$ & $\lambda 9078.3$ &
$\lambda 9088.5$$^{a}$ & $\lambda 9094.8$ & $\lambda 9111.8$ & $S/N$ &
$\lambda 9405.7$ & $S/N$ & $\lambda 7771.9$ & $\lambda 7774.2$ & $\lambda 7775.4$ & {\it S/N}\\
$\chi_{\rm exc}$ [eV]     & 7.48 & 7.48 & 7.48 & 7.48 & 7.49 & 7.49 & & 7.69 & & 9.15 & 9.15 & 9.15 & \\
\mbox{log($gf$)} & --0.35 & --0.46 & --0.58 & --0.43 & 0.15 &--0.30 & & 0.29 & & 0.37 & 0.22 & 0.00 & \\
   & & & & & & & & & & & & & \\
ID & & & & & & & & & & & & & \\
\hline
{\bf UVES (2004)} & & & & & & & & & & & & & \\
CD-24~17504           & --    & --    & --    & --    & 9.5 & --    & 150
& 10.5 & 80 & 1.7$^{b}$ & --    & --    & 400 \\
CD-71~1234            & 10.3 & --    &  5.6 & 13.3 & --    & 11.4 & 140 & 23.6 & 150 &  8.6 &  8.0 &  6.3 & 160 \\
CS 22943-0095         & 16.0 & 16.3 & 11.0 & 14.7 & 48.8 & 21.7 &  70 & 46.3 &  70 & 18.4 & 14.1 &  9.8 & 230 \\
G004-037              & 10.8 &  6.9 &  3.8 &  7.2 & 26.0 & 14.1 & 150 & 27.5 & 110 & 12.4 &  9.5 &  5.9 & 300 \\
G048-029$^{c}$    &  8.0 &  5.9 &  3.6 &  3.2 & 18.2 &  8.6 & 200 & 20.8 & 100 & 10.9 &  5.7 &  2.5 & 200 \\
G059-027              & 27.5 & 21.6 & 18.1 & 22.6 & 55.9 & 31.4 & 150 & 59.7 &  70 & 25.1 & 20.9 & 14.9 & 170 \\
G126-052              & 13.0 & 12.4 &  6.7 & 13.5 & 40.2 & 17.2 & 150 & 42.3 & 150 & 16.6 &  9.4 &  6.9 & 240 \\
G166-054              &  6.6 & --   & --    & --    & 14.5 &  7.9 & 170 & --    & 110 &  8.0 &  6.8 &  4.0 & 200 \\
HD~84937               & 17.3 & 12.7 & 17.6 & 15.3 & 44.0 & 22.5 & 220 & 48.1 & 170 & 19.1 & 14.0 &  8.9 & 170 \\
HD~338529              & 18.0 & 13.0 & --    & 12.9 & 48.7 & --    & 220 & 43.0 & 150 & 19.6 & 12.6 &  9.2 & 400 \\
LP635-014             & 10.8 & 10.3 & 11.8 & 11.8 & 35.1 & 17.5 & 300 & 38.0 & 220 & 14.3 &  8.0 &  5.8 & 230 \\
LP651-004             &  7.6 &  6.7 &  5.1 &  3.6 & 16.7 &  9.1 & 115 & 22.4 & 120 & 10.3 &  9.4 &  5.1 & 250 \\
\hline
{\bf MIKE (2003)} & & & & & & & & & & & & & \\
G041-041              & -- & -- & -- & --    & 18.1   & --     &  80 & -- & 40 &  7.7$^{d}$ &  
5.2$^{d}$ &  3.3$^{d}$ & 250 \\
G048-029$^{c}$    & -- & -- & -- & -- & 19.6 & 10.3 & 200 & -- & 40 & 7.7 & 4.8 & 4.5 & 360 \\
G084-029              & -- & -- & -- &  7.1 & 17.1   & --      & 130 & -- & 40 &  8.4$^{d}$ &  5.8$^{d}$ &  3.7$^{d}$ & 500 \\
LP831-070             & -- & -- & -- & --    & $<$8.0 & $<$3.0 & 130 & -- & 40 & $<$2.0 & $<$2.0 & -- & 380 \\
\hline
\end{tabular}
}
\smallskip
$^{a}$ Where this \Ci~ feature was detected, blending with
\Fei~ was taken into account in the equivalent width determination.
$^{b}$ The oxygen abundance derived with this measurement was
confirmed for this star also via synthetic spectrum fitting, as
described in the text.
$^{c}$ This star was observed in both UVES (2004) and MIKE
(2003) runs.
$^{d}$ Since equivalent widths for the \Oi~ IR triplet were
measured for these stars also in the $^{6}$Li program (Asplund et~al. 2006), with typical 
${\it S/N}\sim 400$ at the relevant
wavelengths, a weighted mean of the determinations was used.
\par
\end{table}