\begin{table}%T4
\caption{X-ray spectral parameters of the \cyg OB-type stars.}\label{OB}
%\centerline
 {\small
\begin{tabular}{l ll l l ll l l l l}
\hline \hline
Src. &\multicolumn{2}{l}{Optical Parameters} &$\chi_\nu^2$&Pile-up&\multicolumn{2}{l}{$N_{\rm H}$[$\times 10^{22}$] [cm$^{-2}$]}&$kT_1$ & $kT_2$ & Abundance   &  Flux [10$^{-13}$]\\
\cline{2-3} \cline{6-7}
\#   &Hanson\#&S.T.&&(\%)&{\sc wabs}&{\sc absori}&[keV]&[keV]&[$Z_\odot$]&[erg~s$^{-1}$~cm$^{-2}$]\\
\hline
60$^b$  &304&B5~Ie     	&1.4&$\sim$18	&2.15 $\pm$ 0.15	&0.87 $\pm$ 0.12	&0.63 $\pm$ 0.03&1.56 $\pm$ 0.11&0.43 $\pm$ 0.04&$\rm 235.4^{255.4}_{201.7}$\\[0.4mm]
133     &339&O8.5~V    	&1.1&no		&0.24 $\pm$ 0.18	&--		&1.53 $\pm$ 0.68&--        &(0.3)   	  &$\rm 0.11^{0.19}_{0.07}$\\[0.4mm]
253     &378&B0~V      	&1.0&no		&3.57 $\pm$ 0.09	&--		&0.43 $\pm$ 0.15&--        &(0.3)        &$\rm 2.00^{2.21}_{1.42}$\\[0.4mm]
315     &390&O8~V      	&0.8&no		&3.30 $\pm$ 0.08	&--		&0.44 $\pm$ 0.10&--        &0.15 $\pm$ 0.09&$\rm 0.64^{0.73}_{0.51}$\\[0.4mm]
433     &417&O4~III(f)    	&1.5&$\lesssim$2&2.30 $\pm$ 0.07	&--		&0.39 $\pm$ 0.06&1.94 $\pm$ 0.73&0.60 $\pm$ 0.34&$\rm 42.1^{45.3}_{34.6}$\\[0.4mm]
456     & 421 & O9.5~V 	&1.4&no		&1.45 $\pm$ 0.08	&-- 		&1.71 $\pm$ 1.02&-- 	    &(0.30) 	  & 1.06$^{0.88}_{1.09}$\\[0.4mm] 
488$^b$ &431&O5~If     	&1.3&$\sim$12	&2.09 $\pm$ 0.07	&--		&0.79 $\pm$ 0.05&2.82 $\pm$ 0.61&0.65 $\pm$ 0.10&$\rm 72.6^{75.5}_{67.5}$\\[0.4mm]
530     &448&O6~V      	&1.4&no  	&1.97 $\pm$ 0.34	&--		&0.65 $\pm$ 0.20&--        &(0.1)        &$\rm 1.18^{1.39}_{0.96}$\\[0.4mm]
537     &455&O8~V      	&1.1&no  	&2.19 $\pm$ 0.07	&--		&0.61 $\pm$ 0.17&--        &(0.1)        &$\rm 1.20^{1.28}_{1.07}$\\[0.4mm]
544     &457&O3~If     	&1.3&$\lesssim$2&2.12 $\pm$ 0.06	&0.56 $\pm$ 0.09	&0.39 $\pm$ 0.14&1.32 $\pm$ 0.19&0.97 $\pm$ 0.3 &$\rm 88.8^{98.6}_{77.5}$\\[0.4mm]
562     &462&O6.5~II   	&1.0&no  	&2.52 $\pm$ 0.48	&--		&0.40 $\pm$ 0.12&--        &0.14 $\pm$ 0.1 &$\rm 8.45^{9.1}_{6.4}$\\[0.4mm]
568$^a$ &465&O6If~+~O5.5III(f)&1.4&$\sim$15	&2.94 $\pm$ 1.25	&--		&0.91 $\pm$ 0.05&2.64 $\pm$ 0.07&0.52 $\pm$ 0.07&$\rm 61.3^{64.9}_{57.1}$\\[0.4mm]
584     &470&O9.5~V    	&0.8&no  	&1.85 $\pm$ 0.07	&--		&0.44 $\pm$ 0.18&--        &(0.3)  	  &$\rm 3.49^{3.98}_{2.89}$\\[0.4mm]
597     &473&O8.5~V    	&1.0&no  	&1.88 $\pm$ 0.09	&--		&0.30 $\pm$ 0.22&--        &1.07         &$\rm 3.00^{3.78}_{2.38}$\\[0.4mm]
615     &480&O7.5~V    	&1.0&no  	&2.73 $\pm$ 0.06	&--		&0.50 $\pm$ 0.17&--        &(0.1)        &$\rm 4.01^{4.43}_{3.42}$\\[0.4mm]
625     &483&O5~If     	&1.0&no  	&1.00 $\pm$ 0.08	&--		&0.55 $\pm$ 0.06&--	    &0.60 $\pm$ 0.21&$\rm 99.4^{107.3}_{86.4}$\\[0.4mm]
626     &485&O8~V     	 	&1.1&no  	&1.65 $\pm$ 0.04	&--		&0.88 $\pm$ 0.23&--        &(0.1)        &$\rm 0.38^{0.53}_{0.21}$\\[0.4mm]
686     &507&O8.5~V    	&1.1&no  	&2.39 $\pm$ 0.08	&--		&0.35 $\pm$ 0.11&--        &(0.3)        &$\rm 4.16^{5.04}_{3.28}$\\[0.4mm]
729$^a$ &516&O5.5~V(f)    	&1.1&$\lesssim$4&0.81 $\pm$ 0.05	&0.51 $\pm$ 0.32	&1.98 $\pm$ 0.12&--	    &0.38 $\pm$ 0.09&$\rm 11.7^{12.4}_{10.1}$\\[0.4mm]
779     &534&O7.5~V  		&1.2&no  	&1.16 $\pm$ 0.03	&--		&2.28 $\pm$ 0.55&--	    &(0.1)	  &$\rm 6.05^{7.74}_{4.91}$\\[0.4mm]
817     &556&B1~Ib     	&0.9&no  	&1.57 $\pm$ 0.08	&--		&0.18 $\pm$ 0.07&--        &(0.3) 	  &$\rm 1.20^{1.53}_{0.94}$\\[0.4mm]
881     &588&B0~V      	&0.9&no  	&1.84 $\pm$ 0.05	&--		&0.42 $\pm$ 0.20&--        &(0.3)        &$\rm 0.81^{1.02}_{0.71}$\\[0.4mm]
895     &601&O9.5~III 		&1.0&no  	&1.98 $\pm$ 0.07	&--		&0.38 $\pm$ 0.21&--        &(0.3)        &$\rm 0.72^{0.92}_{0.50}$\\[0.4mm]
971     &642&B1~III    	&0.9&no  	&1.73 $\pm$ 0.05	&--		&0.96 $\pm$ 0.45&--        &(0.3)        &$\rm 0.14^{0.30}_{0.09}$\\[0.4mm]
979     &646&B1.5~V~+?	&1.5&no  	&2.90 $\pm$ 1.24  &--		&1.92 $\pm$ 1.01&--	    &(0.3)        &$\rm 0.22^{0.63}_{0.29}$\\[0.4mm]
1001    &696&O9.5~V    	&0.8&no  	&0.71 $\pm$ 0.02	&--		&0.54 $\pm$ 0.17&--        &(0.3)        &$\rm 0.71^{0.83}_{0.42}$\\[0.4mm]
\hline
\end{tabular}}
\medskip
\par
Notes: (1) Abundance values in parenthesis indicate cases for which abundances
were fixed in the spectral fit (see text), (2) Absorption-corrected fluxes are
calculated in the 0.5$-$8.0~keV energy range (3) Three bright sources,  \#60,
\#488, and \#568, suffer pile-up, and we extracted the spectra from annular
rings (see Sect.~\ref{sect:extraction}) that exclude the central parts of the
PSFs. $^a$ The 6.4+6.7~keV FeK$_\alpha$ complex is observed; $^b$ The
Fe{\sc i} 6.4~keV line is not detected, but the 6.7~keV seems to be present.
\end{table}