\begin{table}%t9
\caption{The nature of lines having white dwarf wind profile in AG~Peg in symbiotic stars.\label{tab9}}
%\centerline
{\begin{tabular}{lcccccc} \hline\hline
Object     & He II $\lambda$1640 & C IV $\lambda$1548  & N IV $\lambda$1486 & N V $\lambda$1238 & Si IV $\lambda$1393 & Comment  \\ \hline
EG And     & (tcp)   & 52 (s, pc)  & 36    &      & 34   & B  \\
CH Cyg     & 42 (s)  & 730 (pc*)  &       & 321  & str  & B  \\
T CrB      & 573 (pc*)& 821 (pc*) & 320   & 788  &      & B  \\
PU Vul     &       & 166     &      &      & 982 (pc) & B \\    
V1329 Cyg  & 159     & 226        &       &      &      & b \\
Z And      & 113     & 64         & 67    & 114  & 69   & N* \\
RX Pup     & 68      & 128 (s)    & 118   & 111  & 112  & N* \\
HBV475     & 142     & 130        &       &      &      & N* \\
R Aqr      &         & 112        &       &      & 110  & N* \\
HM Sge     & 137     & 111        & 130   & 131  & 110  & N* \\
AG Dra     & 110     & 58         & 41    & 70 (pc) & 56   & N* \\
RW Hya     & 64      & 56         & 55    &      &      & N  \\
SY Mus     & 66      & 67         & 36    & 58   & 39   & N  \\
BF Cyg     & 38      & 65 (s, pc)  & 65    &      & 69   & N  \\ 
CI Cyg     & 68      & 44         & 53    & 55   & 50   & N  \\
V1016 Cyg  & 65      & 65         & 51    & 52   & 64   & N  \\
RR Tel     & 70      & 68         & 39    & 51   & 43   & N  \\       
AX Per     & 64      & 52         & 46    & 58   & 58   & N \\
KX Tra     & 69      & 50         & 36    & 58   & 54   & N \\
AG~Peg$^{a}$ & 770   & (tcp, pc)   & (tcp) & 800  & (tcp)& B \\
AG~Peg$^{b}$ & 66    & 45         &       & 56   & 36   & N \\ \hline
\end{tabular}  }
\par
\smallskip

N) All five lines have {\it FWHM} less than 70~km~s$^{-1}$. \\
N*) One, a few or all of the five lines have a {\it FWHM} between 120 and 150 km s$^{-1}$, which is
significantly broader than for the majority of lines in their spectra. \\
b) Two of the five lines are observable in $IUE$ spectra of V1329 Cyg, the widths of those lines are broader than for
the stars denoted N* but narrower than 400~km~s$^{-1}$. \\
B) Very broad lines ({\it FWHM}~$>$~400~km~s$^{-1}$) are observed as single lines or as narrow lines superimposed on broad 
sockets (str). \\
pc) P cygni profile. \\
pc*) Inverted P cygni profile. \\
 tcp = Two component profile as the spectral line has a narrow emission component superimposed on the broad 
white dwarf wind profile.
\end{table}