\begin{table}%t4
\caption{Spectral parameters obtained from fit.\label{tab4}}
\tiny
%\centerline
{\begin{tabular}{ccccccccc}
\hline\hline
 \multicolumn{2}{l}{Class~I} &&&&&& \\ 
\hline 
ROXN  & Name & & $kT$  & $N_{\rm{H}}$          & Abundance & $E.M.$                 & $L_{\rm{X}}$             & $\chi^2$/d.o.f. \\
      &&&       & ($10^{22}$ cm$^{-2}$) &           &($10^{52}$ cm$^{-3}$) & ($10^{29}$ erg s$^{-1}$) & \\ 
(1) & (2) & (3) & (4) & (5) & (6) & (7) & (8) & (9) \\
\hline \\
 22 & EL29   & & 4.3(3.6$-$5.1) & 4.9(4.4$-$5.3) & 1.0(0.80$-$1.3) & 16.0(13.6$-$18.9) & 27.5&  90.0/ 63.0 \\ 
 43 & IRS43/YLW15 & & 3.9(3.0$-$5.3) & 3.3(2.9$-$3.8) & [0.30] & 13.1(10.2$-$17.3) & 17.3&  36.5/ 35.0 \\ % PN 
    &        &f& 3.2(2.7$-$3.9) & 4.0(3.5$-$4.5) & [0.30] & 29.1(22.8$-$37.0) & 34.8&  56.3/ 45.0 \\ % PN 
 46 & IRS44/YLW16A  & & 2.7(2.4$-$3.1) & 5.3(4.9$-$5.7) & 0.28(0.19$-$0.38) & 45.6(38.3$-$53.9) & 49.7&  77.0/ 72.0 \\ 
 66 & IRS51  & & 2.1(1.8$-$2.8) & 4.2(3.5$-$4.8) & 0.62(0.27$-$1.18) & 13.8(10.2$-$18.5) & 16.2&  51.7/ 48.0 \\ 
\hline  
 \multicolumn{2}{l}{Class~II}&&&&&& \\
\hline 
ROXN &  Name && $kT$  & $N_{\rm{H}}$          & Abundance & $E.M.$                 & $L_{\rm{X}}$             & $\chi^2$/d.o.f. \\
 ID    &&&       & ($10^{22}$ cm$^{-2}$) &           &($10^{52}$ cm$^{-3}$) & ($10^{29}$ erg s$^{-1}$) & \\ 
(1) & (2) & (3) & (4) & (5) & (6) & (7) & (8) & (9) \\
\hline \\
  1 & DoAr25& & 6.4(4.9$-$8.8) & 1.1(0.96$-$1.2) & 0.26(0.02$-$0.51) & 157(141$-$177) & 247 &  80.1/ 72.0 \\
 11 & SR24S & & 2.3(2.0$-$2.7) & 1.2(1.0$-$1.3)  & 0.24(0.07$-$0.43) & 16.3(13.4$-$19.4) & 15.9& 107.7/ 75.0 \\ 
 18 & WL17  & & 2.9(2.0$-$4.3) & 4.1(3.1$-$5.2)  & [0.30]         & 8.4(5.0$-$14.6) & ~9.6&  27.5/ 19.0 \\ % PN 
    &       &f& 3.2(2.5$-$4.2) & 4.5(3.8$-$5.4)  & 0.66(0.31$-$1.2) & 18.1(13.1$-$25.7) & 24.8&  35.4/ 25.0 \\ 
 29 & IRS34 & & 1.8(1.1$-$3.7) & 2.7(1.6$-$4.4)  & [0.30]         & 12.8($<$41.5)  & 11.7 &   4.7/  5.0 \\ 
 30 & WL20  & & 2.3(1.8$-$3.0) & 2.0(1.6$-$2.4)  & [0.30]         & 8.1(5.9$-$11.4) & ~8.1&  16.2/ 17.0 \\ % PN 
    &       &f& 3.4(2.7$-$4.5) & 2.0(1.7$-$2.3)  & 0.34(0.04$-$0.75) & 16.4(13.3$-$20.2) & 20.4&  34.7/ 29.0 \\ % PN
 33 & GY245 & & 2.1(1.3$-$5.0) & 7.7(5.2$-$11.0) & [0.30]         & 4.5(1.5$-$16.4) & 4.4&  10.9/  9.0 \\ % PN 
 45 & VSSG25&f& 2.0(1.6$-$2.5) & 1.1(0.9$-$1.4)  & [0.30]         & 6.3(4.7$-$8.2) & ~5.9&  29.1/ 24.0 \\ % PN 
 50 & IRS47 &f& 2.9(1.7$-$7.4) & 2.3(1.5$-$3.3)  & [0.30]         &  7.5($<$15.5)  & ~8.5 &   1.2/  2.0 \\ 
 57 & GY292 & & 2.3(2.1$-$2.5) & 1.7(1.5$-$1.8)  & 0.23(0.14$-$0.36) & 31.2(28.6$-$35.8) & 30.8& 159.3/153.0 \\ % PN 
 61$^a$ & IRS49 & & 2.0(1.9$-$2.2) & 1.6(1.4$-$1.7)  & 0.18(0.08$-$0.29) & 27.1(23.9$-$30.7) & 24.1& 131.1/114.0 \\ % PN 
 62 & GY310 &f& 2.5(1.7$-$3.6) & 0.82(0.59$-$1.2)  & [0.30]         & 1.8(1.4$-$2.4) & ~1.9&  22.4/ 13.0 \\ % PN 
 63 & GY312 & & 2.3(1.7$-$3.3) & 7.6(6.0$-$8.7)  & [0.30]         & 11.4(6.4$-$22.5) & 11.6&  25.0/ 17.0 \\ % PN 
 65 & GY314 & & 2.1(2.0$-$2.3) & 1.5(1.4$-$1.6)  & 0.16(0.07$-$0.26) & 31.6(28.4$-$35.0) & 28.4& 113.2/113.0 \\ % PN 
\hline  
 \multicolumn{2}{l}{Class~III}&&&&&& \\
\hline 
ROXN  &  Name && $kT$  & $N_{\rm{H}}$          & Abundance & $E.M.$                 & $L_{\rm{X}}$             & $\chi^2$/d.o.f. \\
       &&&       & ($10^{22}$ cm$^{-2}$) &           &($10^{52}$ cm$^{-3}$) & ($10^{29}$ erg s$^{-1}$) & \\ 
(1) & (2) & (3) & (4) & (5) & (6) & (7) & (8) & (9) \\
\hline \\
5  &  GY112      & & 0.98(0.79$-$1.1) & 0.36(0.31$-$0.50) & 0.10(0.06$-$0.16) & 7.5(6.1$-$11.8) & 4.3&  40.9/ 37.0 \\ % PN 
14$^a$ &  GY193  & & 1.27(1.19$-$1.74) & 0.87(0.56$-$1.07) & [0.30] & 7.0(4.6$-$8.2) & 6.0&  29.4/ 38.0 \\ % PN
15 &  GY194      & & 1.5(1.2$-$1.9) & 0.79(0.6$-$1.1) & [0.30] & 3.2(2.6$-$3.9) & 2.8&  20.7/ 13.0 \\ % PN 
25 &  WL19       & & 2.5(1.5$-$4.6) & 8.62(6.0$-$12.8)  & [0.30] & 9.2(3.7$-$30.7) & 9.8&   8.4/ 10.0 \\ % PN 
27,28$^{a,b}$ & ROXs20A, ROXs20B & & & 0.13(0.06$-$0.18) & 0.42(0.23$-$1.21) &         & 4.6&  59.2/ 40.0 \\ 
      &          & & 0.66(0.56$-$0.77) &                &           & 1.7(0.8$-$2.2) & 1.9& \\ 
      &          & & 1.66(1.30$-$2.29) &                &           & 2.8(1.9$-$3.9) & 2.8& \\ 
32,34,35$^{b,c}$ & WL5,WL4,WL3 &           &2.5(2.2$-$3.0) & 4.7(4.2$-$5.2) & [0.30] & 60.4(47.4$-$76.9) & 64.2& 104.6/ 74.0 \\ % PN 
36 & SR12A$-$B & &                   & 0.11(0.08$-$0.13) & 0.12(0.08$-$0.17) &                   & 21.9& 248.6/205.0\\ 
   &           & & 0.25(0.23$-$0.27) &                   &                   & 18.2(11.1$-$30.2) & 4.4& \\ %PN
   &           & & 0.97(0.89$-$1.03) &                   &                   & 18.6(17.0$-$25.2) & 11.1& \\ %PN
   &           & & 3.5(2.5$-$6.5)    &                   &                   & 5.6(3.1$-$8.3) & 6.5& \\ %PN
   &           &f&                   & 0.06(0.03$-$0.10) & 0.24(0.13$-$0.55) &                   & 24.0& 74.0/ 60.0 \\ 
   &           & & 0.32(0.28$-$0.38) &                   &                   & 7.8(4.3$-$17.1) & 4.2& \\ %PN
   &           & & 1.22(1.09$-$1.35) &                   &                   & 15.3(5.5$-$22.5) & 12.0& \\ %PN
   &           & & 12.0($>$3.1)      &                   &                   & 4.9(3.0$-$10.4) & 7.7& \\ %PN
39 & GY253     & & 1.6(1.4$-$2.0)    & 4.5(3.9$-$5.2)   & [0.30]         & 24.9(17.5$-$34.9) & 22.0&  57.7/ 52.0 \\ % PN 
52 & BKLT162730-244726 &  & 1.9(1.3$-$2.3) & 1.0(0.8$-$1.5) & [0.30] & 6.6(5.3$-$11.2) & 6.1&  44.1/ 43.0 \\ % PN 
72 & GY377     & & 1.8(1.1$-$2.7)    & 1.1(0.7$-$1.8)    & [0.30]         & 1.7(0.9$-$3.6) & 1.5&   7.1/ 11.0 \\ % PN 
73 & IRS55     & &                   & 1.1(1.0$-$1.2)   & 0.31(0.20$-$0.50) &                   & 62.3& 139.3/141.0 \\ 
   &           & & 0.64(0.60$-$0.68) &                   &                  & 46.9(28.0$-$67.2) & 45.7& \\ %PN  
   &           & & 2.5(2.2$-$3.0)    &                   &                  & 15.7(12.7$-$19.2) & 16.6& \\ %PN 
76 &  GY410    & & 1.8(1.3$-$2.4)    & 1.5(1.1$-$1.9)   & [0.30]         & 3.8(2.5$-$5.9) & 3.4&   8.9/ 23.0 \\ % PN 
\hline 
 \multicolumn{2}{l}{New Class~III candidates} &&&&&& \\
\hline 
ROXN  & Name && $kT$  & $N_{\rm{H}}$          & Abundance & $E.M.$             & $L_{\rm{X}}$         & $\chi^2$/d.o.f. \\
 ID    &&&       & ($10^{22}$ cm$^{-2}$) &           &($10^{52}$ cm$^{-3}$) & ($10^{29}$ erg s$^{-1}$) & \\ 
(1) & (2) & (3) & (4) & (5) & (6) & (7) & (8) & (9) \\
\hline
31 & 16271643-24311 && 4.2(2.2$-$15.1)  & 5.2(3.5$-$7.4)  & [0.30] & 6.1(3.2$-$14.3) & 8.3&  25.8/ 26.0 \\ % PN 
41 & GY259          && 3.4($>$1.3) & 2.2(1.1$-$4.5)  & [0.30] & 1.9(0.8$-$6.3) & 2.3&   0.5/  2.0 \\ % PN 
44 & GY266          && 2.3(1.1$-$6.1)   & 2.8(1.6$-$5.0)  & [0.30] & 2.4(1.0$-$8.2) & 2.5&   7.5/  6.0 \\ % PN 
53 & GY283          && 1.4(0.5$-$2.6)   & 0.47(0.2$-$1.5) & [0.30] & 0.5(0.3$-$3.0) & 0.5&   2.1/  4.0 \\ % PN 
58 & GY295          && 1.9(1.2$-$2.8)   & 0.34(0.2$-$0.6) & [0.30] & 0.7(0.5$-$0.8) & 0.6&  12.3/ 11.0 \\ % PN 
77 & BKLT162800-244819 && 0.5(0.4$-$0.7)   & 0.97(0.8$-$1.1) & [0.30] & 8.7(4.4$-$17.2) & 7.8&  24.2/ 25.0 \\ % PN 
78 & GY463          && 1.6(1.2$-$2.1)   & 2.6(2.0$-$3.4)  & [0.30] & 11.0(6.8$-$20.2) & 9.6&  16.0/ 20.0 \\ % PN 
86 & BKLT162823-244140 && 4.3(2.2$-$13.2)  & 0.87(0.5$-$1.3) & [0.30] & 4.0(2.8$-$6.7)  & 5.5 &   9.7/  9.0 \\ 
\hline \\
\\
 \multicolumn{4}{l}{X-ray sources with no optical or IR counterpart} &&&& \\
\hline 
ROXN  & Name && $kT$  & $N_{\rm{H}}$          & Abundance & $E.M.$             & $L_{\rm{X}}$         & $\chi^2$/d.o.f. \\
 ID    &&&       & ($10^{22}$ cm$^{-2}$) &           &($10^{52}$ cm$^{-3}$) & ($10^{29}$ erg s$^{-1}$) & \\ 
(1) & (2) & (3) & (4) & (5) & (6) & (7) & (8) & (9) \\
\hline
51 & .................       && 10.5($>$3.9)& 0.92(0.6$-$1.4) & [0.30] & 2.5(2.0$-$3.8) & 4.4&  40.1/ 28.0 \\ % PN 
64 & .................       && 82.4($>$20.5) & 2.2(1.7$-$2.9)& [0.30] & 3.5(2.9$-$4.1) & 5.5&  64.5/ 43.0 \\ % PN 
67 & .................       && 3.6($>$1.4) & 9.5(4.8$-$18.0) & [0.30] & 6.7(2.4$-$46.9) & 8.6&  25.4/ 29.0 \\ 
\hline 
\end{tabular}}
\par
\smallskip
(1) {\it XMM-Newton} source ID number, "Rho Oph X-ray sources, Newton''.
(2) The source name from Col.~(15) in Table~2.
(3) "f'' means that the X-ray spectra are extracted during the flare phase.
(4$-$7) The~90\% confidence regions are given between parenthesis. 
(5) We use WABS for absorption model in XSPEC where standard solar metal abundances are used. The use of revised solar abundances (Holweger \cite{Holweger01}; Allende Prieto et~al. 
\cite{AllendePrieto01}, \cite{AllendePrieto01}) would increase~$N_{\rm H}$ by 20 $\sim$\% (Vuong et~al. \cite{Vuong03}).
(6) The abundance [0.30] is fixed.
(7), (8) The emission measure and X-ray luminosity are calculated from the best-fit PN parameters assuming a distance of 140 pc. Those from MOS1+MOS2 parameters are consistent within errors. The X-ray luminosity is corrected for absorption.\\
$^a$ These sources showed a small flare during the observation, but the X-ray counts in the flares are not sufficient to obtain their spectra.\\
$^b$ It is difficult to obtain an individual spectrum without contamination from neighbouring sources.
We extracted the X-ray spectrum from a circular region that contains all the sources.\\
$^c$ Since the X-ray counts from ROXN-32 is dominant, we put the spectral parameters in the table for Class~III.
\par
\label{spec_tab}
\end{table}