\begin{table}
%\centering
\par
\caption {\label{TabFitCHp}CH$^{+}$ $(0{-}1)$ absorption line analysis results.}
\begin{tabular}{l  l  c  c  c  c }
\hline\hline
\noalign{\smallskip}
Source     & Remark\tablefootmark{a} & $\upsilon_0$ & $\Delta \upsilon$ & $\tau_0$ & $N$(CH$^{+}$) \\
           &        & (km s$^{-1}$)& (km s$^{-1}$)     &          & ($10^{12}$ cm$^{-2}$) \\
\hline
{\bf \object{W33A}} &        &  2.47 $\pm$  0.13 &  5.18 $\pm$  0.23 &  0.28 $\pm$  0.01 &  4.68 $\pm$  0.40  \\
           &        & 10.08 $\pm$  1.17 &  8.38 $\pm$  4.55 &  0.03 $\pm$  0.01 &  0.95 $\pm$  0.66  \\
           &        & 16.82 $\pm$  0.05 &  2.56 $\pm$  0.15 &  0.28 $\pm$  0.01 &  2.37 $\pm$  0.24  \\[0.4cm]
{\bf \object{W49N}} &   E    & --3.62 $\pm$  0.06 &  3.63 $\pm$  0.13 &  0.18 $\pm$  0.01 & 
$>$2.1  \\[0.4cm]
{\bf \object{W51}}  &        &  0.91 $\pm$  0.05 &  2.21 $\pm$  0.12 &  0.18 $\pm$  0.01 &  1.26 $\pm$  0.13  \\
           &        &  7.37 $\pm$  0.03 &  5.13 $\pm$  0.07 &  0.83 $\pm$  0.01 & 13.90 $\pm$  0.35  \\
           &        & 13.14 $\pm$  0.07 &  2.73 $\pm$  0.18 &  0.21 $\pm$  0.01 &  1.88 $\pm$  0.20  \\
           &        & 17.34 $\pm$  0.16 &  3.41 $\pm$  0.48 &  0.10 $\pm$  0.01 &  1.11 $\pm$  0.23  \\
           &        & 23.44 $\pm$  0.06 &  5.83 $\pm$  0.15 &  0.35 $\pm$  0.01 &  6.56 $\pm$  0.28  \\
           &        & 39.97 $\pm$  0.11 &  3.76 $\pm$  0.22 &  0.18 $\pm$  0.01 &  2.24 $\pm$  0.21  \\
           &   E    & 47.16 $\pm$  0.47 &  5.25 $\pm$  0.55 &  0.84 $\pm$  0.09 & $>$14.3  \\
           &   E    & 49.32 $\pm$  0.06 &  2.40 $\pm$  0.27 &  0.94 $\pm$  0.16 & $>$7.3  \\
           &   E    & 53.97 $\pm$  0.11 &  7.26 $\pm$  0.15 &  1.94 $\pm$  0.03 & $>$45.9  \\
           &   E    & 71.56 $\pm$  0.03 &  3.73 $\pm$  0.07 &  0.48 $\pm$  0.01 & $>$5.8  \\
\hline
\noalign{\smallskip}
           & remark & $\upsilon_{\rm min}$ & $\upsilon_{\rm max}$ & $\int \tau \rm d\upsilon$   &  $N$(CH$^{+}$) \\
Source     &        & (km s$^{-1}$)        & (km s$^{-1}$)        & (km s$^{-1}$)           & ($10^{12}$ cm$^{-2}$) \\
\hline
{\bf \object{W33A}} &  E, S   & 20.0 & 45.0 & $>$53.6         & $>$166.5  \\[0.4cm]
{\bf \object{W49N}} &  E, S   &  0.0 & 22.0 & $>$39.3         & $>$122.2  \\
           &   E    & 22.0 & 30.0 & $>$13.5         & $>$41.9  \\
           &   S    & 30.0 & 49.0 & $>$41.1         & $>$127.6  \\
           &   S    & 49.0 & 77.5 & $>$48.1         & $>$149.5  \\[0.4cm]
{\bf \object{W51}}  &  E, S   & 60.0 & 70.0 & $>$17.7         & $>$54.9  \\
\hline
\end{tabular}
\tablefoot {The column
  densities are derived assuming an excitation temperature of 3~K, a lower
  limit for the absorption components detected at velocity intervals
  corresponding to the source itself. The first part of
  the table are the results of the multi-Gaussian decomposition procedure. The
  second part results from the analysis of the spectra over given velocity
  ranges: for the saturated \CHp\ features, lower limits on the column
  densities are inferred assuming a conservative lower limit on the optical
  depth of~2.3 (Neufeld et~al. 2010).\\
\tablefoottext{a}{E = absorption line profile observed in the star-forming
  region. $T_{\rm ex}$ may be underestimated, hence the lower limit on $N(\CHp)$. 
S = saturated line profile.}}
\end{table}