\begin{table}%t2
\par
\caption{\label{t2}{\it XMM-Newton} and {\it Chandra} spectral fitting results (errors 
are at 90\% confidence).}         
%\centerline
{\tiny \begin{tabular}{c c c c c c c c c c c c c c}   
\hline\hline 
\noalign{\smallskip}     
 Year & Satellite & Source & 
 {\tt mekal} & {\tt mekal} & {\tt mekal} & {\tt mekal} & Gauss & Gauss & Gauss
& Gauss & $\chi^2$ & $\chi^2$ & GOES-10 \\ 
of & (observation & net &  $kT$\tablefootmark{a} & norm\tablefootmark{b} & flux\tablefootmark{c} & 0.2--2.0 
keV & energy & norm\tablefootmark{e} & flux\tablefootmark{f} & emitted &/dof\tablefootmark{g} &/dof\tablefootmark{g}
 & 1--8~\AA \\
 obs. & number) & counts & & & & emitted  & (keV) & & & 
power\tablefootmark{d} (MW) & & no line & flux\tablefootmark{i} 
\\
&&&&&& power\tablefootmark{d} (MW)&&&&&&\\\hline
\noalign{\smallskip}           
2002 & {\it XMM-Newton} (1) & 112 &0.28$^{\rm +0.06}_{\rm -0.04}$ 
 & 4.3$^{\rm +1.2}_{\rm -1.1}$ & 1.04$^{\rm +0.36}_{\rm -0.28}$ & 
 230$^{\rm +80}_{\rm -62}$ & 0.48$^{\rm +0.04}_{\rm -0.05}$ 
 & 2.6$^{\rm +1.7}_{\rm -1.8}$ &0.20$^{\rm +0.13}_{\rm -0.14}$ & 
 44$^{\rm +29}_{\rm -30}$ & 0.9/5 & 7.0/7 & 1.13 \\[1mm]
\vspace{1 mm}
2003 & {\it Chandra} (1) & 137 & $0.65\pm{0.19}$  
 &1.3$\pm${0.4} & 0.37$^{\rm +0.10}_{\rm -0.12}$ & 
 94$^{\rm +25}_{\rm -30}$ & 0.55$^{\rm +0.02}_{\rm -0.01}$
 & $5.9\pm{1.5}$ & $0.53\pm{0.13}$ & $135\pm{34}$ & 8.6/9 & 32.6/11 & 2.12 \\[1mm]
\vspace{1 mm}
2004 & {\it Chandra} (2) & 112 & 0.59$^{\rm +0.15}_{\rm -0.28}$  & 
 3.1$^{\rm +0.7}_{\rm -0.8}$ & 0.90$^{\rm +0.10}_{\rm -0.35}$ & 
 167$^{\rm +19}_{\rm -65}$ & 0.57$\pm${0.03}
 & 4.9$^{\rm +2.3}_{\rm -2.1}$ & 0.44$^{\rm +0.21}_{\rm -0.19}$ & 
 82$^{\rm +38}_{\rm -35}$ & 12.2/10 & 16.7/12 & 3.23 \\[1mm]
\vspace{1 mm}
2004 & {\it Chandra} (3) & 42 & 0.61$^{\rm +0.84}_{\rm -0.36}$  
 & 0.7$^{\rm +0.8}_{\rm -0.4}$ & 0.19$^{\rm +0.15}_{\rm -0.12}$ & 
 36$^{\rm +28}_{\rm -23}$ & 0.56$^{\rm +0.05}_{\rm -0.03}$
 & 4.3$^{\rm +1.8}_{\rm -2.4}$ & 0.39$^{\rm +0.16}_{\rm -0.22}$ & 
 74$^{\rm +31}_{\rm -41}$ & 0.22/1 & 5.2/3 & 0.16 \\[1mm]
\vspace{1 mm}
2005 & {\it XMM-Newton} (2) & 146 & 0.33$^{\rm +0.12}_{\rm -0.08}$ &
 $1.1\pm{0.4}$ & 0.27$^{\rm +0.15}_{\rm -0.10}$ & 
 65$^{\rm +36}_{\rm -24}$ & $0.52\pm{0.02}$ & $1.7\pm{0.7}$ & 
 $0.15\pm{0.06}$ & $36\pm{15}$ &
 17.4/16 & 33.3/18 & 0.22 \\[1mm]
2005 & {\it XMM-Newton} (3) & $<$44$^h$ & 0.33 & $<$0.3$^h$ 
& $<$0.08$^h$ & $<$19$^h$ & 0.52 & $<$0.51$^h$ & $<$0.05$^h$ & $<$12$^h$ 
& & & 0.004 \\
\hline             
\end{tabular}}
\tablefoot{\tablefoottext{a}{{\tt mekal} temperature in~keV.}
\tablefoottext{b}{{\tt mekal} normalisation at 1~keV in units of 
  10$^{\rm -6}$ ph cm$^{\rm -2}$ s$^{\rm -1}$~keV$^{\rm -1}$.}
\tablefoottext{c}{Total 0.2--2.0~keV energy flux in the {\tt mekal} component 
  in units of 10$^{\rm -14}$ erg cm$^{\rm -2}$ s$^{\rm -1}$; the errors
  on the fluxes were obtained by varying the {\tt mekal} temperatures
  and normalisations between their 90\% confidence limits.}
\tablefoottext{d}{Powers and errors calculated by multiplying the values 
  in the previous column by 4$\pi${\it d}$^2$, where {\it d} is the geocentric 
  distance of Saturn at the given epoch.}
\tablefoottext{e}{Gaussian line normalisation in units of 
  10$^{\rm -6}$ ph cm$^{\rm -2}$ s$^{\rm -1}$.}
\tablefoottext{f}{Total energy flux in the line in units of
  10$^{\rm -14}$ erg cm$^{\rm -2}$ s$^{\rm -1}$.}
\tablefoottext{g}{$\chi^2$ value and degrees of freedom.}
\tablefoottext{h}{3$\sigma$ upper limit.}
\tablefoottext{i}{Solar X-ray flux (1.5--12.4~keV) in units of 10$^{\rm -6}$ Watt~m$^{\rm -2}$, corrected for solar rotation (see text).}}
\vspace*{2mm}
\end{table}