\begin{table}%t3
\caption{Radio information of halos and mini halos taken from the literature
and reanalyzed in this work with the exponential model fit.}
%\centerline
{
\begin{tabular}{cclcccccccc} 
\hline\hline\noalign{\smallskip}
Cluster & Type & Reference           & $z$     & kpc/$''$ & $FWHM$ &  $I_0$               &  $r_e$      &  $r_e$    &  $\langle J\rangle$ & $\chi^2_{\rm RED}$ \\
        &      &                     &       &          & arcsec & $\mu$Jy/arcsec$^2$    &  arcsec    &  kpc &   erg s$^{-1}$~Hz$^{-1}$~cm$^{-3}$ &              \\ 
\hline\noalign{\smallskip}
A2744   &H & Govoni et~al. (\cite{Govoni2001})      &0.3080 & 4.50 & 50 & $3.05^{\rm +0.12}_{-0.12}$  & $61^{\rm +2}_{-2}$ & $275^{\rm +9}_{-9}$ & $2.5^{\rm +0.17}_{-0.16}\times 10^{-42}$  & 1.5  \\
\noalign{\smallskip}
A665    &H & Giovannini Feretti (\cite{Giovannini2000}) &0.1819 & 3.03 & 53 & $1.09^{\rm +0.08}_{-0.08}$  & $78^{\rm +6}_{-5}$ & $236^{\rm +18}_{-15}$ & $7.0^{\rm +1.0}_{-1.0}\times 10^{-43}$  & 0.9  \\ 
\noalign{\smallskip}
A2219   &H & Bacchi et~al. (\cite{Bacchi2003})      &0.2256 & 3.59 & 53 & $1.10^{\rm +0.08}_{-0.08}$  & $100^{\rm +5}_{-4}$ & $359^{\rm +18}_{-14}$ & $5.4^{\rm +0.6}_{-0.6}\times 10^{-43}$  &3.7  \\    
\noalign{\smallskip}
A2255   &H & Govoni et~al. (\cite{Govoni2005})      &0.0806 & 1.50 & 25 & $0.65^{\rm +0.02}_{-0.02}$ & $135^{\rm +4}_{-4}$ &  $203^{\rm +6}_{-6}$  & $3.4^{\rm +0.20}_{-0.19}\times 10^{-43}$  &  4.8  \\ 
\noalign{\smallskip}
A773    &H & Govoni et~al. (\cite{Govoni2001})      &0.2170 & 3.48 & 30 & $0.75^{\rm +0.07}_{-0.07}$  & $32^{\rm +3}_{-3}$ &  $111^{\rm +10}_{-10}$& $1.1^{\rm +0.24}_{-0.2}\times 10^{-42}$  &  0.7 \\ 
\noalign{\smallskip}
A545    &H & Bacchi et~al. (\cite{Bacchi2003})      &0.1540 & 2.64 & 45 & $1.31^{\rm +0.15}_{-0.13}$  & $57^{\rm +4}_{-4}$ &  $150^{\rm +11}_{-11}$& $1.2^{\rm +0.22}_{-0.19}\times 10^{-42}$  & 0.6   \\ 
\noalign{\smallskip}
A2319   &H & Feretti et~al. (\cite{Feretti1997})     &0.0557 & 1.07 & 30 & $1.11^{\rm +0.04}_{-0.04}$  & $185^{\rm +7}_{-6}$ & $198^{\rm +7}_{-6}$ & $5.4^{\rm +0.35}_{-0.36}\times 10^{-43}$  & 2.4   \\ 
\noalign{\smallskip}
A2218   &H & Giovannini Feretti (\cite{Giovannini2000}) &0.1756 & 2.94 & 35 & $1.06^{\rm +0.34}_{-0.27}$  & $26^{\rm +9}_{-6}$ &  $76^{\rm +26}_{-18}$& $2.0^{\rm +1.4}_{-0.9}\times 10^{-42}$  &1.0   \\     
\noalign{\smallskip}
A2163   &H & Feretti et~al. (\cite{Feretti2001})     &0.2030 & 3.31 & 62 & $2.23^{\rm +0.07}_{-0.07}$  & $119^{\rm +2}_{-2}$ &  $394^{\rm +7}_{-7}$& $9.2^{\rm +0.4}_{-0.4}\times 10^{-43}$  &2.1    \\  
\noalign{\smallskip}
A401    &H & Bacchi et~al. (\cite{Bacchi2003})      &0.0737 & 1.38 & 45 & $0.44^{\rm +0.06}_{-0.05}$  & $79^{\rm +15}_{-11}$ &  $109^{\rm +21}_{-15}$& $4.1^{\rm +1.3}_{-1.0}\times 10^{-43}$  &0.7   \\  
\noalign{\smallskip}
A2254   &H & Govoni et~al. (\cite{Govoni2001})      &0.1780 & 2.98 & 45 &  $1.56^{\rm +0.22}_{-0.20}$  & $80^{\rm +19}_{-13}$ &  $238^{\rm +57}_{-39}$& $9.7^{\rm +3.4}_{-2.8}\times 10^{-43}$  &1.1    \\  
\noalign{\smallskip}
RXJ1314 &H & Feretti et~al. (\cite{Feretti2005})     &0.2439 & 3.81 & 45 & $1.05^{\rm +0.31}_{-0.25}$  & $42^{\rm +16}_{-10}$ &  $160^{\rm +61}_{-38}$& $1.2^{\rm +0.8}_{-0.5}\times 10^{-42}$  &0.1    \\  
\noalign{\smallskip}
RXJ1347 &MH& Gitti et~al. (\cite{Gitti2007})       &0.4510 & 5.74 & 18 &  $26.0^{\rm +40.7}_{-15.4}$  & $9^{\rm +3}_{-2}$ &  $52^{\rm +17}_{-11}$& $1.8^{\rm +0.7}_{-0.5}\times 10^{-40}$  &0.2  \\ 
\noalign{\smallskip}
A2390   &MH& Bacchi et~al. (\cite{Bacchi2003})      &0.2280 & 3.62 & 20 & $60.8^{\rm +27.0}_{-21.1}$  & $10^{\rm +1}_{-1}$ &  $ 36^{\rm +4}_{-4} $ & $3.1^{\rm +1.0}_{-0.8}\times 10^{-40}$  &1.2   \\ 
\noalign{\smallskip}
Perseus & MH  & Pedlar et~al. (\cite{Pedlar1990})   &0.0179 & 0.36 & 45 & $99.6^{\rm +10.9}_{-10.6}$ & $64^{\rm +4}_{-3}$ &  $23^{\rm +1}_{-1}$ &   $3.6^{\rm +0.5}_{-0.5}\times 10^{-40}$  &2.4 \\    
\hline
\end{tabular}}
\medskip
\par
Column 2: type of diffuse emission contained (H = halo, MH = mini halo);
Col. 6: \textit{FWHM} of the circular Gaussian beam;
Col. 10: average radio emissivity over the volume of a sphere of radius 3$r_{e}$, $k$-corrected with $\alpha=1$.
\label{tab3}
\end{table}