\begin{table}%t5
\caption{\label{t5}Pal~4 abundances relative to comparison clusters.}
%\centering
\par
\renewcommand{\footnoterule}{} 
\begin{tabular}{rccrccccc}
\hline
\hline\noalign{\smallskip}
Name & [Fe/H] & $R_{\rm GC}$ [kpc] & $N$ & $\langle\Delta$[X/Fe]$\rangle_{\rm all}$   & $\langle\Delta$[X/Fe]$\rangle_{Z<39}$ & 
${\langle}{\Delta}$[X/Fe]/${\sigma}{\rangle}_{\rm all}$   & $\langle\Delta$[X/Fe]/${\sigma}{\rangle}_{Z<39}$ & Reference\tablefootmark{a}\\ 
(1) & (2) & (3) & (4) & (5) & (6) & (7) & (8) & (9) \\
\hline
NGC 6752 & $-$1.61 &  5.2 & 17 & 0.18 $\pm$ 0.06 &    \phs0.10 $\pm$ 0.08 & 1.0 &    \phs0.5 & (1), (2) \\
M 13     & $-$1.56 &  8.7 & 17 & 0.15 $\pm$ 0.06 &     \phs0.04 $\pm$ 0.06 & 0.8 &    \phs0.2 & (1), (3) \\
M 3      & $-$1.39 &  12.3 & 18 & 0.09 $\pm$ 0.06 & $-$0.01 $\pm$ 0.08 & 0.5 &    \phs0.0 & (1), (3) \\
NGC 7492 & $-$1.87 & 24.9 & 16 & 0.09 $\pm$ 0.05 &     \phs0.02 $\pm$ 0.05 & 0.4 &    \phs0.1 & (1), (4) \\
NGC 5694 & $-$2.06 & 29.1 & 10 & 0.36 $\pm$ 0.12 &     \phs0.14 $\pm$ 0.06 & 1.8 &    \phs0.6 & (1), (5) \\
Pal 3    & $-$1.58 & 95.9 & 19 & 0.05 $\pm$ 0.05 & $-$0.05 $\pm$ 0.06 & 0.3 & $-$0.1 & (1), (6) \\
 \hline                  
\end{tabular}
\tablefoot{\tablefoottext{a}{(1) Web-version (2003) of Harris (\cite{Harris1996}); (2) Yong et~al. (\cite{Yong2005}); (3) Cohen \& Mel\'endez (\cite{Cohen2005b}b); (4) Cohen \& Mel\'endez (\cite{Cohen2005a}a); (5)~Lee et~al. (\cite{Lee2006});  (6) Paper~I.}}\vspace*{1.5mm}
\end{table}