\begin{table}%t2
%\centering
\par
\caption{\label{tab1}Mean value of element abundance in dust phase in ppm  with 1$\sigma$ error.}
\begin{tabular}{lllllll} 
\hline\hline
\noalign{\smallskip}
& \multicolumn{1}{c}{$\langle$[Mg/H]$_{\rm d} \rangle$} &
\multicolumn{1}{c}{$\displaystyle\frac{\langle[{\rm Mg/H}]_{\rm d} \rangle}{[{\rm Mg/H}]_{\rm cosmic}}$} &
\multicolumn{1}{c}{$\langle$[Si/H]$_{\rm d} \rangle$} &
\multicolumn{1}{c}{$\displaystyle\frac{\langle[{\rm Si/H}]_{\rm d} \rangle}{[{\rm Si/H}]_{\rm cosmic}}$} &
\multicolumn{1}{c}{$\langle$[Fe/H]$_{\rm d} \rangle$} &
\multicolumn{1}{c}{$\displaystyle\frac{\langle[{\rm Fe/H}]_{\rm d} \rangle}{[{\rm Fe/H}]_{\rm cosmic}}$} \\
\noalign{\smallskip}
\hline
\noalign{\smallskip}
all sightlines &  $33.13 \pm 2.35$  & $0.832 \pm 0.059$ (147)\tablefootmark{*} &  $25.01 \pm 2.91$  & $0.772 \pm 0.090$ (39)     &  $30.64 \pm 0.41$  & $0.970 \pm 0.013$ (134)    \\
stars with $|b|\leq 30\degr$ \\
~~~$E(B-V) \leq 0.20$ & $32.31 \pm 2.60$  & $0.812 \pm 0.065$ (48)& $23.97 \pm 3.03$  & $0.740 \pm 0.093$ (14)&  $30.65 \pm 0.40$  & $0.970 \pm 0.013$ (47)\\
~~~$E(B-V) > 0.20$ & $34.11 \pm 1.96$  & $0.857 \pm 0.049$ (85)& $29.30 \pm 1.48$  & $0.904 \pm 0.046$ (15)&   $30.86 \pm 0.31$  & $0.977 \pm 0.010$ (78)\\
   & $36.90 \pm 1.44$  & $0.927 \pm 0.036$ (14) &  $30.25 \pm 0.76$  & $0.934 \pm 0.023$ (6) & $31.16 \pm 0.31$  & $0.986 \pm 0.010$ (17)\\
stars with $|b|> 30\degr$ & $29.98 \pm 3.92$  & $0.753 \pm 0.099$ (14)&  $20.03 \pm 4.90$  & $0.618 \pm 0.151$ (10)&   $28.68 \pm 1.30$  & $0.908 \pm 0.041$ (9) \\
\hline
\end{tabular}
\tablefoot{\tablefoottext{*}{Number of sightlines. Results for stars with $D\leq 400$~pc and
$|b|\leq 30\degr$,  $E(B-V) > 0.20$ are given in italics.}}\vspace*{2.5mm}
\end{table}