\begin{table}%t
\par
  \caption {\label{tab:psfit_line}Best-fit parameters from the fits to the spectra of Elias~29, during 6~different time intervals (PN data only), using an
  absorbed 1T thermal model with an additional line at 6.4~keV (Fe
  fluorescent line).}
\par
    %\centerline
 {
     \begin{tabular}{lcccccccccc}
     \hline\hline\\[-3mm]
Time interval &  $N({\rm H})$ & $kT$ & $Z$ & $E\!M$ & $f_{\rm 6.4 keV}$ & $W_{\rm 6.4~keV}$ & $\chi^2$/d.o.f. & $P$ & $F_{\rm X}$ & $R_{\rm 6.4~ keV}$\ddag \\
\hline
~ & $N_{22}$ & keV &  $Z_{\odot}$ & $E\!M_{53}$ & $f_{-6}$ & eV & ~ & ~ & $F_{-13}$ & \% \\
\hline
seg1 & 5.5 $\pm$ 0.7 & 4.8 $\pm$ 1.0 & 1.1 $\pm$ 0.3 & 0.7 $\pm$ 0.3 &
0.1 $\pm$ 0.7 & 34.8 & 1.0 & 0.5 & 1.8 & 46\\
flare & 9.4 $\pm$ 2.0 & 3.9 $\pm$ 1.4 & 0.9 $\pm$ 0.3 & 4.5 $\pm$ 3.4
& 2.0 $\pm$ 5.9 & 162.0 & 0.9 & 0.6 & 7.5 & 22\\
seg2 & 8.2 $\pm$ 1.3 & 2.8 $\pm$ 0.6 & 1.1 $\pm$ 0.3 & 0.8 $\pm$ 0.4 &
1.1 $\pm$ 0.6 & 834.0 & 1.3 & 0.1 & 1.1 & 0.1\\
seg3 & 6.6 $\pm$ 0.8 & 3.3 $\pm$ 0.6 & 0.7 $\pm$ 0.2 & 0.9 $\pm$ 0.4 &
0.5 $\pm$ 0.5 & 270.0 & 0.9 & 0.6 & 1.3 & 4.0\\
seg4 & 7.6 $\pm$ 0.6 & 3.6 $\pm$ 0.4 & 0.7 $\pm$ 0.1 & 1.7 $\pm$ 0.5 &
0.7 $\pm$ 0.7 & 171.0 & 1.3 & 0.1 & 2.7 & 3.1 \\
seg5 & 4.9 $\pm$ 0.4 & 4.5 $\pm$ 0.8 & 0.6 $\pm$ 0.1 & 1.1 $\pm$ 0.3 &
1.1 $\pm$ 0.8 & 335.0 & 1.2 & 0.2 & 2.5 & 0.3\\
\hline
seg3$+$seg4$+$seg5$\diamondsuit$ & 6.4 $\pm$ 0.3 & 3.9 $\pm$ 0.3 & 0.6 $\pm$ 0.1 &
1.2 $\pm$ 0.2 & 1.0 $\pm$ 0.3 & 330.0  & 1.3 & 0.0 & 2.1 & 0.0\\
\hline
    \end{tabular}}
\par
\smallskip
\par
\ddag\ Probability that a line with a best-fit
value equal or greater than $W_{\rm 6.4~keV}$ could be due to a random
fluctuation in the data, as estimated via Monte Carlo simulations (see
Sects.~3 and~4).
\par
$\diamondsuit$ Results for the fit to the source's spectrum integrated over
time intervals ``seg3'', ``seg4'', and ``seg5''.
\par
Note: For the line, the total flux in the line ($f_{\rm 6.4 ~keV}$ in
units of $f_{-6} = 10^{-6}$~photons~cm$^{-2}$~s$^{-1}$) and the
equivalent width ($W_{\rm 6.4~keV}$) are given.
\par
\end{table}