\begin{table}%t4
\caption{\label{tab4}Equivalent widths of H$\alpha$,  \ion{He}{i},  \ion{Ca}{ii}, %and \ion{He}{i},
 and forbidden emission lines observed in the spectra.} 
\par
%\centering
\par
\begin{tabular}{l	c	c	c	c	c c c c c c c c c}
\hline
\hline \noalign{\smallskip}
Star & H$\alpha$ & P(17) & \ion{He}{i} & \multicolumn{3}{c}{[\ion{O}{i}]} & \multicolumn{2}{c}{[\ion{S}{ii}]}  & \multicolumn{2}{c}{[\ion{N}{ii}]}
       & \multicolumn{2}{c}{\ion{Ca}{ii}} \\
       & (6563 \AA) & (8467 \AA) & (6548 \AA) & \multicolumn{3}{c}{(6301 \AA,~6365 \AA,~8446 \AA)}  & \multicolumn{2}{c}{(6716 \AA,~6731 \AA)} 
       & \multicolumn{2}{c}{(6549 \AA,~6585 \AA)}
       & \multicolumn{2}{c}{(8498 \AA,~8662 \AA)}\\
\hline 
\multicolumn{13}{c}{\it Confirmed Herbig Ae/Be and T Tauri stars}\\
Hen 3-1121S      & EIA$^{\rm +2.8}_{-0.1}$ 	& (0.1)	& +0.8 		& --0.02     & (0.01) & (0.05)	& (0.01) 	& (0.01) & +0.01 & (0.01) & (0.01) & (0.0) \\
Hen 3-1121N     & EIA$^{\rm +2.0}_{-0.4}$ 	& (0.1)	& +0.8 		& --0.03     & (0.02) & (0.08)	& (0.01) 	& (0.01) & --0.04 	& --0.13 	& (0.1) & (0.0) \\
MWC 878          &  --54								& --2.0	&  --3.5 		&  --0.12    & (0.01) & --8.3		& (0.01) 	& (0.01) & --0.5 	& --1.6 		& --7.1   & --8.1 \\
WRAY 15-1435  & --20   								& --1.7	& +0.6	 	& --0.02     & (0.02) & --4.1		& --0.01   	& (0.01) & (0.01)	 & (0.02) & --0.3   & --0.5 \\
MWC 953          & --32   								& --3.5	& +0.3 		& --0.01     & (0.02) & --2.2		& (0.01) 	& (0.01) & +0.03 & +0.1 	& --0.4 	& --0.7 \\
HD 313571          & --34   								& --2.1	& --0.3		& --0.01     & (0.02) & --4.8		& (0.02) 	& (0.01) & +0.01 & (0.01) 	&  --1.3 	 & --0.1 \\
Hen 3-823          & --25   								& --1.4	& +0.6		& (0.01)   & (0.03) & --1.4		& (0.01) 	& (0.01) & (0.01) & (0.01) & (0.1)  & (0.1) \\
MWC 593          & --35  								& --1.3	& --0.2		& --0.01     & (0.03) & --3.7		& (0.01) 	& (0.01) & (0.01) & (0.02) &  --0.6	 & (0.1) \\
Hen 2-80            & --150								& --1.8	& +0.6		& --9.9       & --3.4     & --16			& --0.1  		& --0.2	  &  --0.06  & --0.2	 	& --0.2 	 & --0.2 \\
WRAY 15-1372  & --15									& (0.2)	& (0.02)	& (0.1)     & (0.1)  	& (0.6)		& (0.01)  	& (0.03) & (0.01) & (0.1) 	& (0.3)  & (0.6) \\
Th 17-35            & --90									& (0.6)	& +0.2		& --0.3       & --0.4    	& --5.3		& --0.1      & --0.1	  & --0.07 	 & --0.2 		& --0.1    & --0.2 \\
HD 145718       & PC$^{\rm +2.4}_{-0.2}$	& (0.6)	& (0.1)		& (0.2)     & (0.1)   	& +0.5		& (0.01) 	& (0.01) & (0.3) 	 & (0.0) 	& +0.6	 & +1.4\\
CD-38 4380       & EIA$^{\rm +1.0}_{-3.0}$ 	& (0.6)	& (0.03)	& (0.1)     & (0.2)  	& +0.5		& (0.1)    & (0.02) & (0.01) & (0.3) 	& +0.7  & +1.4\\
Hen 3-1145       & --30   								& (0.1)	& --0.5		& --0.5       & (0.3)  	& (0.02)	& +0.2    & (0.04) & (0.02) & (0.05)  & --0.5 	 & --0.5 \\[2pt]
\hline
\multicolumn{12}{c}{\it Giant stars with emission lines that may be Herbig Ae/Be stars}\\
HD 152291      & --3.4								& --0.8	& +0.2				& (0.01) 	& (0.02)	& (0.05)	& (0.01) &  (0.01) 	& (0.01) & (0.01) 			& --0.5 & (0.1) \\
Hen 3-416        & PC$^{\rm +0.5}_{-27}$	& (1.0)	&+0.2				& --0.4     	& --0.2     	& (0.0)		& (0.1)   &  (0.02) 	& (0.01) & (1) 				 	& --5.3 & --9 \\
WRAY 15-488  & PC$^{\rm +7.2}_{-0.8}$& +1.0	& (0.06)			& (0.1)   	& (0.1)   	& +0.6		& +0.1   &  (0.1) 		& (0.01) & (0.3) 	 			& +1.2 & +2.0 \\[2pt]
\hline
\multicolumn{13}{c}{\it Giants and Supergiants with emission lines}\\
HD 323154        & --26           					& --0.9	& --2.0				& (0.01) 	& (0.01)  & (0.02)	& (0.05) &  (0.01)  & (0.01) & --0.07 				& --0.8 & --0.9\\
WRAY 15-1104 & PC$^{\rm +0.2}_{-10}$& +0.5	& PC$^{\rm +0.4}_{-0.4}$	& (0.2)    & --0.02   	& --0.7		& (0.01) &  (0.01) 	& (0.01) 	& (0.3) & (0.5) & (0.5) \\
Hen 3-1428      & --18   & PC$^{\rm +0.25}_{-0.04}$ &  --1.4	   & --0.8   	& --0.3   	& --4.0		& (0.02) &   --0.05  	& --0.15		     & PC$^{\rm +0.2}_{-0.9}$ & (0.1) & (0.1)  \\
MWC 314        &  --118       					& --2.4	& --6.1     			& --0.01    & (0.01) 	& --4.7		& --0.06   &  (0.03) 	& --0.04 	& --0.17 			& --13 & --19 \\
HD 320156      & --7.8     							& --0.7	& 0.3			      & (0.02)  & (0.03) 	& PC$^{\rm +0.2}_{-0.05}$ & (0.02) &  (0.02) 	& +0.1 		& PC$^{-0.15}_{+0.03}$ & --8 		& --14 \\
Hen 3-1347      &PC$^{\rm +0.8}_{-12}$  	& +0.1	& 0.2				 	& --0.3    	& --0.1	  	& --0.7		& (0.05) &  (0.04) 	& (0.01) 	& +0.2 				& +0.5 & EIA$^{\rm +0.7}_{-0.2}$ \\
\par
AS 231            & PC$^{\rm +1.4}_{-14}$  & +0.7 	& 0.2				   & (0.01)  & (0.02)  & +0.8		& +0.01  & +0.03 	& (0.03) 	& (0.01)			& +1.3 & +2.0 \\[2pt]
\hline
\multicolumn{13}{c}{\it Unclassified stars with strong emission line spectrum}\\
WRAY 15-1651 & --92 & --1.2	& (0.6)			 & --0.90   & --0.1       & --7.4		& --0.1			 & --0.12 	& (0.06) & (0.02) 			& --1.5 & --1.7 \\ 
MWC 930         & PC$^{\rm +0.1}_{-42}$& PC$^{\rm +0.7}_{-1.0}$	& +0.2			 & --0.02   & (0.01)   & PC$^{\rm +1.5}_{-1.5}$ & PC$^{\rm +0.2}_{-0.1}$& (0.04) & --0.04   & (0.01) & PC$^{\rm +1.7}_{-5.1}$	& PC$^{\rm +2.0}_{-6.6}$ \\[2pt]
\hline
\multicolumn{13}{c}{\it Dwarf stars without H$\alpha$ in emission}\\
AS 321             & +5.7 		& (0.1) 	& (0.03) 			& --0.02    & (0.01) 	& +0.6		& (0.01) 			&  (0.01) & (0.01) & (0.01) & +0.8 & +1.8\\[2pt]
\hline
\multicolumn{13}{c}{\it Giant and Supergiant stars without H$\alpha$ in emission}\\
WRAY 15-522   & +1.2 		& +0.2		& (0.03) 	 & --0.2     & (0.1)    & (0.1)	  &  +0.1   &  (0.2) & (0.01)  & (0.1) & +1.3  & +2.1\\
Th 35-41           & +1.2			& +1.4		& --0.15		 & (0.1)   & (0.1)    & (0.2)	  & (0.5)    &  (0.4) & (0.01)  & (0.2) & +2.2 & +2.7 \\
WRAY 15-566   & +0.4			& (0.06)	& --0.15  	 & (0.3)   & (0.1)    & (0.1)	  & (0.6)    &  (0.1) & (0.1) 		& (0.2) & +0.6 & +0.6 \\
WRAY 15-1650 & +1.0			& +0.6		& (0.01) 	 & (0.2)   & (0.1)    & (0.2)	  & (0.5)    &  (0.2) & (0.1) 		& (0.3) & +1.3 & +2.1 \\
WRAY 15-1702 & +0.8			& +0.8		& (0.02) 	 & (0.1)   & (0.1)    & (0.3)	  & (0.5)    &  (0.5) & (0.1) 		& (0.3) & +1.1 & +2.0 \\
WRAY 15-770   & +0.5			& (0.05)	& (0.04) 	 & (0.2)   & (0.1)    & (0.1)	  & (1.0)    &  (1.0) & (0.1) 		& (0.1) & EIA$^{\rm +0.4}_{-0.1}$  & PC$^{-0.3}_{+0.4}$  \\
HD 305773      & +2.0			& (0.07)	& +0.7	 	 & (0.05) & (0.01)  & (0.05) & (0.01)  &  (0.02) & (0.01)	& (0.05) & (0.1) & (0.1) \\[2pt]
\hline
\end{tabular} 
\tablefoot {In the cases where emission lines are observed inside a broad absorption line, we give the {\it EW} of the absorption and emission component and write EIA meaning ``Emission Inside Absorption''. In the case of P~Cygni and inverse P~Cygni profiles  are noted by PC and the equivalent width ({\it EW}) of the absorption and emission component are given.  For the stars displaying Paschen emission, the \ion{Ca}{ii}~lines at 8498 and 8662~\AA\ are blended with the Paschen(16) and Paschen(13) respectively. For these sources the {\it EW} of \ion{Ca}{ii}~line at~8498 and 8662~\AA, is the {\it EW} measured at the position of the \ion{Ca}{ii}~line minus the 
{\it EW} of the Paschen(17) and Paschen(14) lines respectively. Upper limits are displayed in parenthesis.}
\end{table}