\begin{table}%T3
\caption{\label{tab:correlation}Radio relic properties.}
\small%\centerline
{
\begin{tabular}{llllll}
\hline
\hline\noalign{\smallskip}
Source Name& $\alpha_{74~{\rm MHz}}^{1400~{\rm MHz}}$& spectral curvature   & $P_{1.4}$& size$^{a}$& $R_{{\rm projected}}$\\
                          &         &$\alpha_{74~{\rm MHz}}^{610~{\rm MHz}} - \alpha_{610~{\rm MHz}}^{1400~{\rm MHz}}$        & $10^{24}$ W Hz$^{-1}$  & kpc  & kpc\\
\noalign{\smallskip}\hline
VLSS J1133.7+2324 & $-1.69$& 0.96&24.1&570 \\ %S5
VLSS~J1431.8+1331$^{d}$ &  \ldots& \ldots & \ldots & 125 & 175\\ %S6
 24P73 (VLSS J2217.5+5943)  & $-2.20$ &  2.0& \ldots& \ldots &\ldots\\ % S14
 \object{MACS J0717.5+3745} & $-1.09^{b}$ & $-0.02$ & 138$^{b}$ & 700 & 320\\ % S21 
Abell 2048 (VLSS~J1515.1+0424) &$-1.50$& 1.60& 0.566 & 310& 310 \\
Abell 2256 &$-1.2$&\ldots & 3.95 &1100 & 300\\
Abell 1240-N &$-1.2$&\ldots &0.427&650& 700\\
Abell 1240-S &$-1.3$& \ldots&0.730&1250& 1100\\
Abell 2345-E &$-1.3$& \ldots  &2.62 &1500& 890\\
Abell 2345-W  &$-1.5$&\ldots &2.83 & 1150&1000\\
Abell 13 &$-1.79$& 0.65& 0.853& 260 & 170\\% Slee 
Abell 85 &$-2.30$&1.36&0.322&150&430 \\% Slee
Abell 133 &$-1.70$&1.39 &1.07&55 & 40\\ % Slee
Abell 4038 &$-1.88$& 1.03& 0.0983 &55 & 35\\% Slee
Abell 3667 &$-1.1$&\ldots &17.4&1920 &1950 \\
Abell 548b A&$\sim$$-2$&\ldots & 0.260& 310 & 500 \\ 
Abell 548b B&$<$$-2.0$& \ldots & 0.250 & 370 & 430\\
Abell 521 &$-1.48$& \ldots &2.90 &1000 &930\\
Coma cluster$^{c}$ & $-1.18$&\ldots & 0.284& 850& 1940\\
Abell 2163 &$-1.02$& \ldots & 2.23& 450 & 1550 \\ 
Abell 2744 &$-1.1$& \ldots& 6.20 & 1620 & 1560 \\
Abell S753 &$-2.0$&\ldots & 0.205&350  & 410  \\
Abell 115 &$-1.1$& \ldots & 16.7 & 1960 & 1510\\  %used brightest peak Govoni et al. (2001)
%Abell 1664 &$\ldots$&  \ldots &2.20 &830 & 825\\  no spectral index available
Abell 610 &$-1.4$& \ldots& 0.444 & 330 & 310\\
%Abell 1300 &&&\\ Venturi 2007, now results yet
RXC~J1314.4-2515-E & $-1.41$ & \ldots&2.08 & 920& 685\\
RXC~J1314.4-2515-W& $-1.40$ & \ldots& 4.81 & 920& 685\\
%Abell 3367 &&&\\ Joydeep Bagchi
\hline 
\end{tabular}}
\smallskip 
$^{a}$ Largest linear scale.\\
$^{b}$ Excluding the flux of the halo and central head-tail source \citep[see also][]{2009arXiv0905.3650V, 2009AetA...503..707B}.\\
$^{c}$ 1253+275.\\
$^{d}$ Blended with a nearby AGN (except in the GMRT 610~MHz image), therefore no spectral index or spectral curvature could be calculated.
\end{table}