\begin{table}%t2
%\centering
\par
\caption {\label{table:no2}Data for the 13 GRBs added to the old sample described in \citet{Amati09}. }  
\begin{tabular}{c c c c c c c c c}
\hline\hline  
\noalign{\smallskip}
$GRB$ & $z$ & $E_{p,o}$ (keV) & $\alpha$ ($\gamma$) & $\beta$  & $S_{\rm obs}$ (10$^{-6}$ ergs~cm$^{-2}$) & $band$ (keV) & $GCN$ \\
(1) & (2) & (3) & (4) & (5) & (6) & (7) & (8) & (9)\\
\hline % inserts single horizontal line
090516  &  4.109 & 190 $\pm$ 65    &   --1.5  $\pm$ 0.3 &  [--2.2] $\pm$ [0.4] &  15 $\pm$ 3 & 20--1200 & 9422\\ % inserting body of the table
090715B  &  3.00 & 134 $\pm$ 56  &   --1.1 $\pm$ 0.4 & [--2.2] $\pm$ [0.4] & 9.3 $\pm$ 1.5 & 20--2000 & 9679\\
090812  &  2.452 & 586 $\pm$ 243  &   --1.03   $\pm$ 0.07 & [--2.2] $\pm$ [0.4] & 26.1 $\pm$ 3.4 & 15--1400 & 9821 \\
090926B  &  1.24 & 91 $\pm$ 2  &   --0.13  $\pm$ 0.06 & [--2.2] $\pm$ [0.4] & 8.7 $\pm$ 0.3 & 10--1000 & 9957\\
091018  &  0.971 & 28 $\pm$ 16  &   --1.53   $\pm$ 0.59 & [--2.2] $\pm$ [0.4] & 1.44 $\pm$ 0.19 & 10--1000 & 10~045\\
091029  &  2.752 & 61.4 $\pm$ 17.5  &    --1.46  $\pm$ 0.27 & [--2.2] $\pm$ [0.4] & 2.4 $\pm$ 0.1 & 15--150 & 10~103\\
090618  &  0.54 & 155.5  $\pm$ 11  &  --1.26 $\pm$ 0.06 &  --2.50 $\pm$ 0.33 & 270 $\pm$ 6 & 8--1000 & 9535\\
090902B  &  1.822 & 775 $\pm$ 11  &  --0.696 $\pm$ 0.012 &  --3.85  $\pm$ 0.31 & 374 $\pm$ 3 & 50--10~000 & 9866\\
090926  &  2.1062 & 314 $\pm$ 4  &   --0.75 $\pm$ 0.01 &   --2.59  $\pm$ 0.05 &  145 $\pm$ 4 & 8--1000 & 9933\\
091003  &  0.8969 & 486.2  $\pm$ 23.6  &  --1.13 $\pm$ 0.01   &   --2.64  $\pm$ 0.24 &  37.6 $\pm$ 0.4 & 8--1000 & 9983\\
091020  &  1.71 & 103 $\pm$ 68 &  --0.93 $\pm$ 0.6 & --1.9 $\pm$ 0.8 &  10.4 $\pm$ 2.1 & 20--2000 & 10~057\\
091127  &  0.49 & 36 $\pm$ 2  &   --1.27   $\pm$ 0.06    &   --2.20  $\pm$ 0.02 &  18.7 $\pm$ 0.2 & 8--1000 & 10~204\\
091208B  &  1.0633 & 124 $\pm$ 20.1  &   --1.44 $\pm$  0.07    &  --2.32 $\pm$ 0.47 &  5.8 $\pm$ 0.2 & 8--1000 & 10~266\\
\hline
\end{tabular}
\tablefoot{In this table we show (1) the name of GRB, (2) the spectral model used for the fitting of the spectra, (3) the redshift, (4) the peak energy observed, (5) the softer spectral index, absent for the cut-off power law spectral model, (6) the higher spectral index, (7) the observed fluence and (8) the detector band considered for the estimate of the fluence, (9) the GCN reference for the GRB, where we took the spectral data.}\vspace{-2mm}
\tablebib{\citep{Sakamoto}, \citep{McBreen}, \citep{Golenetskii}, \citep{Sakamoto2}, \citep{Bissaldi}, \citep{Bissaldi2}, \citep{Briggs}, \citep{Rau}, \citep{Golenetskii2}, \citep{Golenetskii3}, \citep{Barthelmy}, \citep{Wilson}, \citep{McBreen2}.}
\end{table}