\begin{table}%T3
\caption{\label{table3}A comparison between the \hi~halo cloud samples observed with
  different telescopes.}
  \small%\centering
\par
\begin{tabular}{cc c c c c c c c}
\hline\hline
    &  $|z|$  & $d$   &  \NH &  \FWHM & $s$ & $D$  & $\langle n \rangle $ & $M_{\hi}$     \\
 & kpc &~kpc & $10^{19}{\rm cm^{-2}}$ & \kms & \arcmin & pc & ${\rm cm^{-3}}$ & \msun  \\
\hline 
Effelsberg & 0.9--5.4  & 3--11  & 0.4--7.4 & 2--21.1   &   9--27  & 8--70   & 0.07--1.2 & 3--770\\ 
WSRT&          &       & 1.2--3.2 & 2.5--4.0  & 0.9--2.1 & 2--6    & 1.3--3.1 & 1--24 \\
VLA&          &       & 2.9--7.6 & 2.8--5.8  & 0.9--2.1 & 2--6    & 2.2--5.7 & 7--32 \\
\citet{Lockman2002}& 0.6--1.2  &       & 0.7--6.3 & 5.4--26.3 &         &19--35   & 0.1--0.9  &12--290 \\
\citet{Snezana2006}& 0.06--0.9 &0.2--3  & 1--3      & 3--7.6  & 6--12    &0.6--8   &          & 0.03--7\\
\citet{Ford2008ApJ}& 0.3--1.7  &       & 0.4--6.6  &5.8--26.2  &         & 46--100 &          & 120--4850 \\ 
\citet{Stil2006}& 0.01--0.16&4.2--7.7& 8--39     &3.4--16.5  & 1.8--29.4&3.4--36.7&3--24      &9--2500\\ 
\hline                 
\end{tabular}
\tablefoot{The table gives the range of values of the clouds for
  the following properties: $|z|$ which is the absolute height above the plane
  (defined in the inner  part of the disk) in~kpc. $d$ the distance in~kpc. \NH\ is the column   density of \hi~gas in $10^{19}{\rm cm^{-2}}$. \FWHM\ is the line
  width  in \kms. $s$ is the observed angular size  in \arcmin. $D$ is the
  diameter in pc.  $\langle n \rangle $  is the average volume density  in
  ${\rm cm^{-3}}$. $M_{\hi}$  is the visible \hi~mass in \msun.}
\end{table}