\begin{table}%t2
\caption{\label{t:corrrmsg}Pearson's correlation coefficients, degrees of freedom and 
significance for relations with iron spread in our GC sample.}
\small%\centerline
{
\begin{tabular}{llll}
\hline \hline 
Parameter                        & $r_{\rm p}$ &d.o.f.&signif.  \\
\hline     		
$M_V$                            &$-$0.49& 17& 95--98\%    \\
$R_{\rm perig.}$                 &  +0.47& 15& 90--95\%    \\
$\log T_{\rm eff}^{\rm max}$ (HB) &  +0.38& 17& 90\%       \\
$x$(MF)                            &  +0.60& 11& 95--98\%    \\
rel.Age                          &$-$0.49& 17& 95--98\%    \\
$\sigma$(h)                      &  +0.59& 16& 99\%       \\
P	                         &  +0.65& 17& $>$99\%    \\
I	                         &$-$0.67& 17& $>$99\%    \\
E	                         &  +0.52& 17& $\sim$98\% \\
$[$(Mg+Al+Si)/Fe$]$              &$-$0.48& 16& 95--98\%    \\
$[\langle \rm Si,Ca\rangle$/Fe]                 &$-$0.70& 17& $>$99\%    \\
$[$Ca/Fe$]$ 	                 &$-$0.78& 17& $>$99\%    \\
$[<$$\alpha$$>]$/Fe]                  &$-$0.72& 17& $>$99\%    \\
$[$Mg/Fe$]_{\rm max}$            &$-$0.52& 17& 98\%    \\
$[$Mg/Fe$]_{\rm min}$            &$-$0.56& 17& 98--99\%    \\
$[$Si/Fe$]_{\rm min}$            &$-$0.44& 17& 90--95\%    \\
\hline  
\end{tabular}}
\smallskip
-- $M_V$ from the on-line version of the Harris (\cite{Harris1996}) catalogue.\\
-- Peri-galactic distance $R_{\rm perig.}$ in kpc from Dinescu et~al. (\cite{Dinescu1999}) 
or Casetti-Dinescu et~al. (\cite{Casetti2007}).\\
--  Maximum temperature along the HB $\log T_{\rm eff}^{\rm max}$(HB) 
from Recio Blanco et~al. (2006) or derived in Carretta et~al. (\cite{Carretta2009c}).\\
--  Exponent $x$ of the power-law relation for global mass function from
Djorgovski et~al. (\cite{Djorgovski1993}). \\
--  Relative age parameter from De Angeli et~al. (\cite{Angeli2005}) and Rosenberg et~al.
(\cite{Rosenberg1999}).\\
--  Velocity dispersion at the half-mass radius $\sigma(h)$ from Gnedin et~al. (\cite{Gnedin2002}).\\
--  Fractions of primordial~$P$, intermediate~$I$ and extreme~$E$ components from
Carretta et~al. (\cite{Carretta2009a}; Paper VII).\\
--  The other abundance ratios are derived from UVES spectra (Carretta et~al.
\cite{Carretta2009b}; Paper VIII); here [$\alpha$/Fe] is the average of [Mg/Fe]$_{\rm max}$, 
[Si/Fe]$_{\rm min}$ and [Ca/Fe].
\end{table}