\begin{table}%t3
\caption{\label{pcahexte}Results of spectral fits of PCA+HEXTE data taken outside of but within one day of bursts, i.e., representing persistent emission only.}
\par
%\centering
\par
\begin{tabular}{cccccccccccc}
\hline \hline \noalign{\smallskip}
\multicolumn{1}{c}{MJD} &
\multicolumn{1}{c}{$\Delta t$} & 
\multicolumn{1}{c}{$\chi^2_{\rm red}$/d.o.f.} &
\multicolumn{1}{c}{$kT_{\rm bb}$} &
\multicolumn{1}{c}{$R_{\rm bb}$} &
\multicolumn{1}{c}{$F_{\rm bb,bol}$ (10$^{-10}$} &
\multicolumn{1}{c}{$\gamma_{\rm pl}$} & 
\multicolumn{1}{c}{$N_{\rm pl}$} & 
\multicolumn{1}{c}{$E_{\rm Fe}$} & 
\multicolumn{1}{c}{$N_{\rm Fe}$ (10$^{-3}$} &
\multicolumn{1}{c}{$F_{\rm X}$} & 
\multicolumn{1}{c}{$F_{\rm X,bol}$} \\ 
\multicolumn{1}{c}{} &
\multicolumn{1}{c}{(days)} &
\multicolumn{1}{c}{} &
\multicolumn{1}{c}{(keV)} &
\multicolumn{1}{c}{(km)} &
\multicolumn{1}{c}{erg~s$^{-1}$~cm$^{-2}$)} &
\multicolumn{1}{c}{} &
\multicolumn{1}{c}{} &
\multicolumn{1}{c}{(keV)} &
\multicolumn{1}{c}{ph~s$^{-1}$~cm$^{-2}$)} &
\multicolumn{2}{c}{(10$^{-10}$~erg~s$^{-1}$~cm$^{-2}$)} \\
\hline
51~789 &  $<$0.27 & 1.81/108 & 0.93 $\pm$ 0.01 & 1.45  $\pm$  0.01 & 1.92 $\pm$ 0.03 & 1.841 $\pm$ 0.003 & 0.206 $\pm$ 0.001 & 6.9 $\pm$ 0.1 & 0.52 $\pm$ 0.05 & 8.37 $\pm$ 0.04 & 35.9 $\pm$ 0.2 \\
51~944 &     0.09 & 1.17/108 & 1.02 $\pm$ 0.02 & 1.18 $\pm$ 0.01 & 1.75 $\pm$ 0.04 & 1.988 $\pm$ 0.004 & 0.289 $\pm$ 0.001 & 6.6 $\pm$ 0.1 & 0.58 $\pm$ 0.08 & 9.10 $\pm$ 0.06 & 37.7 $\pm$ 0.3 \\
53~040 &     1.05 & 1.14/108 & 1.09 $\pm$ 0.01 & 1.12 $\pm$ 0.01 & 2.19 $\pm$ 0.04 & 2.162 $\pm$ 0.004 & 0.269 $\pm$ 0.002 & 6.8 $\pm$ 0.2 & 0.34 $\pm$ 0.11 & 7.36 $\pm$ 0.06 & 29.7 $\pm$ 0.2 \\
54~188 &     1.02 & 1.35/79$^a$ & 0.90 $\pm$ 0.02 & 1.51 $\pm$ 0.02 & 1.86 $\pm$ 0.04 & 1.957 $\pm$ 0.003 & 0.256 $\pm$ 0.001 & 6.7 $\pm$ 0.1 & 0.68 $\pm$ 0.07 & 8.44 $\pm$ 0.05 & 35.3 $\pm$ 0.2 \\
\hline
\end{tabular}
\tablefoot {\tablefoottext{a}{No HEXTE Cluster A spectrum.}\\
Given are the day of the observation (MJD), the time to the closest burst~($\Delta t$), and the spectral parameter values. The latter are the goodness of fit degrees of freedom~($\chi^2_{\rm red}$/d.o.f.), the black-body parameters (temperature~$kT_{\rm bb}$, radius~$R_{\rm bb}$ at~3~kpc, bolometric black-body flux~$F_{\rm bb,bol}$), the power-law parameters (power-law index~$\gamma_{\rm pl}$, normalization at 1~keV $N_{\rm pl}$), the~Gaussian line (presumably~Fe~K) parameters (line energy~$E_{\rm Fe}$, line normalization~$N_{\rm Fe}$; line width was fixed at 0.1~keV), and the
unabsorbed fluxes in the 2$-$10~keV ($F_{\rm X}$) and 0.1$-$200~keV ($F_{\rm X,bol}$)~bands.}
\end{table}