\begin{table}%t2
\caption{Parameters of the spectral modeling.}
\label{tb:fit} 
%\tabcolsep=0.19cm
%\centerline
{
\begin{tabular}{lcc}
\hline
\hline
Parameter & GX~340+0 & 4U1608-52\\
\hline
$D$, kpc		& 8.5			& 4.0 				\\
NH, cm$^{-2}$	& $5\times 10^{22}$ 	& $1\times 10^{22}$		\\
$F_{\rm3-20~keV}$ $^1$ erg/s/cm$^2$ & $1.4\times 10^{-8}$ & $4.2\times 10^{-9}$\\
$F_{\rm 0.1-30~keV}$ $^2$ erg/s/cm$^2$ & $2.7\times 10^{-8}$ & $8.8\times10^{-9}$\\
$L_{\rm 0.1-30~keV}$ $^2$ erg/s & $2.3\times 10^{38}$	& $1.7\times 10^{37}$\\
$\dot{M}$ $^3$,  g/s	& $3.1\times 10^{18}$	& $2.0\times 10^{17}$	\\
\hline
\hline
\multicolumn{3}{c}{QPO frequency resolved spectra ($\approx$boundary layer)$^4$}\\
\hline
\multicolumn{3}{c}{power law with exponential cutoff (phabs$\times$cutoffpl)}\\
\hline
$\alpha$	&$-0.55\pm0.16$	&$-1.28\pm 0.13$\\
$E_{\rm f}$, keV	&$3.3\pm0.2$	&$2.4\pm 0.1$	\\
$\chi^2$/d.o.f.	& 13.9/16	& 4.8/9		\\
\hline
\multicolumn{3}{c}{Comptonization model (phabs$\times$comptt)}\\
\hline
$kT_{\rm bb}$, keV	& $1.3\pm0.2$	& $1.4\pm0.4$	\\
$kT_{\rm e}$, keV	& $3.1_{-0.3}^{+0.9}$	& $2.6_{-0.3}^{+\infty}$\\
$\tau$		& $6.0_{-2.1}^{+1.8}$	& $6.7_{-5.3}^{+5.7}$	\\
$\chi^2$/d.o.f.	& 11.3/15	& 4.0/8		\\
\hline
\hline
\multicolumn{3}{c}{average spectra$^4$}\\
\hline
\multicolumn{3}{c}{phabs$\times$(grad+pexrav+Gaussian)}\\
\hline
inclination$^5$	& $60\degr$	&	$70\degr$\\
$T_{\rm col}/T_{\rm eff}$ $^5$ & 1.7	& 1.8	\\
$\dot{M}$, $10^{18}$ g/s	& $3.0\pm 0.04$	& $0.34\pm 0.01$\\
$\dot{M}/\dot{M}_{\rm Edd}$ $^6$	& $\approx$0.9	& $\approx$0.1\\
$\Omega/2\pi$	& $0.27\pm0.07$		& $\la$0.1\\
$EW$ $^7$, eV	& $48\pm 10$ 	& $147\pm 17$\\
$L_{\rm BL}/L_{\rm tot}$, 3--20 keV	&	47\%	&	57\%	\\
\hline
\hline
\end{tabular}}
\par
\smallskip
$^1$  Observed. $^2$  Absorption corrected;
$^3$  Calculated from the total unabsorbed luminosity 
using the accretion efficiency for the neutron star spin frequency of
$\nu_{\rm NS}=500$ Hz  \citep[][ see Sect.~\ref{sec:disk_bl},
Eq.~(\ref{eq:mdot})]{sibg00}.   
$^4$  The details of spectral modeling are given in Sect.~\ref{sec:fit}.
$^5$  Fixed at fudicial value. 
$^6$  Assuming $\dot{M}_{\rm Edd}=2\times 10^{38}/c^2\eta_{\rm disk}
\approx 3.5\times 10^{18}$~g/s, where  $\eta_{\rm disk}=0.066$ --
accretion disk efficiency for $\nu_{\rm NS}=500$~Hz and
$M_{\rm NS}=1.4~M_{\odot}$. $^7$ - Line energy and width were fixed at $E_{\rm line}=6.7$~keV and
$\sigma_{\rm line}=0.5$ keV.
\end{table}