\begin{table}%t3
\caption{\label{tab3}Established spectral type, literature photometry, estimated distance, radial and projected rotational velocity, observed~H$\alpha$ and forbidden line emission.}\vspace*{2mm}
\par
%\centering
\par
\begin{tabular}{l	c	c		c	c	c	c	c	c	c	c c c c c c }
\hline\hline  \noalign{\smallskip}               
       &          &                 $T_{\rm eff}$ &  $B$   &  $V$   & $E(B-V)$ & $A_V$ & $d_{\rm phot}$ &   $v ~{\rm sin}(i)$  & $v_r$  &     \\
Star  &   Sp.Type  &     [K]            & [mag] & [mag] & [mag]    & [mag]  & [kpc]                 &  [km~s$^{-1}$]                   &  [km~s$^{-1}$]  & H$\alpha$  & F.L.       \\
(1)   &  (2)   &  (3)           &     (4)            &   (5)    &    (6)  &  (7)       & (8)           &  (9)      &   (10)                & (11) & (12) \\ 
\hline
\multicolumn{12}{c}{\it Confirmed Herbig Ae/Be and T Tauri stars}\\
Hen 3-1121S &   B0Ve     &  30~000  &  11.6 $\pm$ $0.1$  & 11.1 $\pm$ $0.1$ & 0.85 $\pm$ $0.14$  &  2.7 $\pm$ $0.5$  &  3.1$^{\rm +1.0}_{-0.8}$ 
& 240 $\pm$ $20$ & --28 $\pm$ $5$ &    I & [\ion{O}{i}]\\
Hen 3-1121N &   B0.5Ve &  27~500  &     ...                  & 13.0 $\pm$ $0.4$ & 1.3 $\pm$ $0.7^\star$  &  4.1 $\pm$ $2.3$  &  3.2$^{\rm +6.3}_{-2.1}$  
& 245 $\pm$ $20$ & --58 $\pm$ $5$ &    I & [\ion{O}{i}] [\ion{N}{ii}] \\
MWC 878 &   B1Ve &  25~400  &        11.2 $\pm$ $0.1$  & 10.8 $\pm$ $0.1$  & 0.74 $\pm$ $0.15$  &  2.3 $\pm$ $0.5$  &  2.1$^{\rm +0.9}_{-0.6}$   
&  ... & --11 $\pm$ $3^*$ &  I &     [\ion{O}{i}] [\ion{N}{ii}]\\
WRAY 15-1435 &   B1Ve &  25~400  &        12.8 $\pm$ $0.5$  & 12.0 $\pm$ $0.5$  & 1.0 $\pm$ $0.7$  &  3.2 $\pm$ $2.2$  &  2.6$^{\rm +5}_{-1.7}$  
& 230 $\pm$ $20$ & --30 $\pm$ $10$ &  I & [\ion{O}{i}] \\
MWC 953 &   B2Ve &  22~000  &        12.0 $\pm$ $0.2$  & 10.9 $\pm$ $0.1$  & 1.3 $\pm$ $0.2$ &  4.0 $\pm$ $0.7$  & 0.8$^{\rm +0.5}_{-0.3}$  
& ${<}7$         &  23 $\pm$ $2$ &  II &    [\ion{O}{i}] \\
HD 313571 &  B3Ve &  18~700  & 10.3 $\pm$ $0.1$  & 9.9 $\pm$ $0.1$   &  0.57 $\pm$ $0.15$  &  1.8 $\pm$ $0.5$  &  0.9$^{\rm +0.4}_{-0.3}$  
& 380 $\pm$ $20$ &  --50 $\pm$ $20$ & I &      [\ion{O}{i}] \\
Hen 3-823 &   B3Ve &  18~700  & 10.5 $\pm$ $0.1$  & 10.4 $\pm$ $0.1$  & 0.33 $\pm$ $0.15$  &  1.0 $\pm$ $0.5$  &  1.6$^{\rm +0.8}_{-0.5}$   
& 310 $\pm$ $20$ & --10 $\pm$ $10$ &   II &   [\ion{O}{i}] \\
MWC 593 &   B4Ve &  17~000  & 10.5 $\pm$ $0.1$  & 10.0 $\pm$ $0.1$ & 0.65 $\pm$ $0.15$  &  2.1 $\pm$ $0.5$  &  0.7$^{\rm +0.2}_{-0.2}$  
& 330 $\pm$ $30$ & --20 $\pm$ $10$ &   I &      [\ion{O}{i}] \\
Hen 2-80 &    B6Ve &  14~000  & 14.0 $\pm$ $0.1$  & 13.2 $\pm$ $0.1$  & 0.97 $\pm$ $0.15$  &  3.0 $\pm$ $0.5$   &  1.6$^{\rm +0.5}_{-0.4}$  & 
60 $\pm$ 10 &  --22 $\pm$ $3$ & II &    [\ion{O}{i}][\ion{S}{ii}] \\
WRAY 15-1372 &  B6Ve &  14~000  &  11.7 $\pm$ $0.1$  & 11.1 $\pm$ $0.1$  & 0.80 $\pm$ $0.15$  &  2.5 $\pm$ $0.5$  &  0.8$^{\rm +0.2}_{-0.17}$  
& 280 $\pm$ $20$& --30 $\pm$ 10 &  II &     ... \\
Th 17-35&    B8Ve &  11~900  &   13.9 $\pm$ $0.1$  & 13.5 $\pm$ $0.1$ & 0.58 $\pm$ $0.15$  &  1.8 $\pm$ $0.5$  &  2.4$^{\rm +0.8}_{-0.6}$  
& 210 $\pm$ $20$& --10 $\pm$ $5$ &  I &  [\ion{O}{i}] \\
HD 145718 &  A5Ve &  8200  & 9.3 $\pm$ $0.1$  &  8.9  $\pm$ $0.1$ &  0.24 $\pm$ $0.15$  &  0.8 $\pm$ $0.5$  &  0.17$^{\rm +0.05}_{-0.04}$ 
& 100 $\pm$ $10$ 		 & 0 $\pm$ $3$ &   IV & ... \\
CD-38 4380 &   F4Ve &  6590  & 10.4 $\pm$ $0.1$  & 10.0 $\pm$ $0.1$  & 0.0 $\pm$ $0.15$  &  0.0$^{\rm +0.5}_{-0.0}$  &  0.19$^{\rm +0.05}_{-0.04}$  
& 45 $\pm$ $4$ & 20 $\pm$ $2$ & I &     ... \\
Hen 3-1145 &  M1IVe &  3720  & 15.3 $\pm$ $0.1$  & 14.0 $\pm$ $0.1$ & --0.15 $\pm$ $0.15$  & 0.0$^{\rm +0.1}_{-0.0}$ &   0.16$^{\rm +0.05}_{-0.04}$  
& $<$7 & --2 $\pm$ $1$ &  I &    
[\ion{O}{i}] \\[2pt]
\hline
\multicolumn{12}{c}{\it Giant stars with emission lines that may be Herbig Ae/Be stars}\\
HD 152291 &  B1IIIe &  24~000  & 9.0 $\pm$ $0.1$   &  9.0 $\pm$ $0.1$   &  0.28 $\pm$ $0.15$  &  0.9 $\pm$ $0.5$  &  3.1$^{\rm +1.3}_{-0.9}$  
& 320 $\pm$ $20$ & --20 $\pm$ 10 &  II &     ... \\
Hen 3-416 &   A1IIIe &        9480  & 11.9 $\pm$ $0.2$   & 10.8 $\pm$ $0.1$   & 1.0 $\pm$ $0.2$  &  3.3 $\pm$ $0.7$  &  0.29$^{\rm +0.12}_{-0.08}$  
& 30 $\pm$ $5$ & 33 $\pm$ $4$ &  III, IV &   [\ion{O}{i}] \\
WRAY 15-488 	&  F2IIIe 	 &    6870  & 10.3 $\pm$ $0.1$  & ~9.8 $\pm$ $0.1$	  & 0.11 $\pm$ $0.15$  &	 0.3 $\pm$ $0.5$  &	 0.36$^{\rm +0.09}_{-0.07}$   
& 30 $\pm$ $5$ & --2 $\pm$ $2$ & IV &      ... \\[2pt]
\hline
\multicolumn{12}{c}{\it Giant and Supergiant stars with emission lines}\\
HD 323154 			&  B4IIe		 &  15~500  & 10.2 $\pm$ $0.1$  & ~9.3 $\pm$ $0.1$	&  1.10 $\pm$ $0.15$ &  3.4 $\pm$ $0.5$  &  1.1$^{\rm +0.3}_{-0.2}$  
& 55 $\pm$ $5$ & 75 $\pm$ 4 &  I &     ... \\
WRAY 15-1104 &  B1Iae	 &  20~800  & 11.0 $\pm$ $0.1$  & 10.8 $\pm$ $0.1$ & 0.40 $\pm$ $0.15$  &  1.2 $\pm$ $0.5$  & 20$^{\rm +7}_{-5}$  
& 50 $\pm$ $5$  & 60 $\pm$ $5$ & IV & [\ion{O}{i}] \\
Hen 3-1428 		&  B1Iae 	 &  20~800  & 11.3 $\pm$ $0.1$  & 10.9 $\pm$ $0.1$ & 0.61 $\pm$ $0.15$  &  1.9 $\pm$ $0.5$  &  15$^{\rm +6}_{-4}$  
& 38 $\pm$ $5$ & 30 $\pm$ $5$  & I &  [\ion{O}{i}] [\ion{N}{ii}] \\
MWC 314		&  B3Ibe 	 &  16~200  & 11.1 $\pm$ $0.1$  & ~9.8 $\pm$ $0.1$	& 1.45 $\pm$ $0.15$  &  4.5 $\pm$ $0.5$  &  1.5$^{\rm +0.4}_{-0.3}$  
& 40 $\pm$ $5$ & 65 $\pm$ $10$ & I & [\ion{O}{i}] [\ion{N}{ii}] \\
HD 320156		 &  B4Ibe	 &  14~900  & 10.5 $\pm$ $0.1$  & ~9.9 $\pm$ $0.1$	&  0.72 $\pm$ $0.15$ &  2.3 $\pm$ $0.5$  &  4.2$^{\rm +1.0}_{-0.8}$  
& 35 $\pm$ $5$  & 60 $\pm$ $3$ &  I & [\ion{O}{i}] [\ion{N}{ii}] \\
Hen 3-1347		&  B5Ibe &  13~600  & 11.9 $\pm$ $0.2$  & 11.5 $\pm$ $0.2$	& 0.56 $\pm$ $0.28$  &  1.8 $\pm$ $0.9$  &  10$^{\rm +6}_{-4}$  
& 30 $\pm$ $5$ & --15 $\pm$ $5$ & IV &    [\ion{O}{i}]  \\
AS 231				&  B9Iae &  10~300  & 12.6 $\pm$ $0.6$  & 10.2 $\pm$ $0.1$	& 2.4 $\pm$ $0.6$   &  7.5 $\pm$ $1.9$  &  0.9$^{\rm +1.3}_{-0.5}$ 
& 28 $\pm$ $5$ & --25 $\pm$ $5$& IV &    ... \\[2pt]
\hline
\multicolumn{12}{c}{\it Stars with strong emission line spectrum}\\
WRAY 15-1651 &   B1-B5 &  ...  &  17.0 $\pm$ $0.2$  & 15.8 $\pm$ $0.2$  & ...  &  ...  &  ...  & ... &  ... & I &     [\ion{O}{i}] \\
MWC 930        &   B5-B9 &  ... &   14.6 $\pm$ $0.5$  & 12.8 $\pm$ $0.5$  & ...  &  ...  &  ...  & 70 $\pm$ $10$ &  10 $\pm$ $10$ & IV &    [\ion{O}{i}] \\[2pt]
\hline
\multicolumn{12}{c}{\it Dwarf stars without H$\alpha$ in emission}\\
AS 321				&   A5V &   8200 & 12.0 $\pm$ $0.1$  & 11.3 $\pm$ $0.1$   & 0.60 $\pm$ $0.23$  &  1.9 $\pm$ $0.7$   &  0.31$^{\rm +0.13}_{-0.09}$  
& 150 $\pm$ $10$ & --30 $\pm$ $5$ & abs. &  [\ion{O}{i}] \\[2pt]
\hline
\multicolumn{12}{c}{\it Giant and Supergiant stars without H$\alpha$ in emission}\\
WRAY 15-522 &   G9III & 4820  & 14.3 $\pm$ $0.6$    & 13.4 $\pm$ $0.6$     & --0.03 $\pm$ $0.8$  &  0.0$^{\rm +2.6}_{-0.0}$ &   3.3$^{\rm +7.7}_{-2.3}$  
& ${<}7$ & --9 $\pm$ $2$ & abs. &  [\ion{O}{i}] \\
Th 35-41           &  M1III & 3720  & 14.5 $\pm$ $0.1$    & 13.1 $\pm$ $0.6$  & --0.17  $\pm$ $0.6$ & 0.0$^{\rm +1.5}_{-0.0}$ &   5.1$^{\rm +5}_{-2.6}$  
& 13 $\pm$ $4$ &  15 $\pm$ $2$ & abs. &  ... \\
WRAY 15-566  &   M6III & 3240  & 16.0 $\pm$ $0.4$    & 14.2 $\pm$ $0.8$   & 0.31 $\pm$ $0.90$  &  1.0 $\pm$ $2.8$   &  4.6$^{\rm +13}_{-3.5}$  
& $<$7 &  29 $\pm$ $2$ & abs. &  ... \\ 
WRAY 15-1650 &    M6III & 3240  & 13.5 $\pm$ $0.5$    & 11.9 $\pm$ $0.2$    & 0.13 $\pm$ $0.54$  & 0.4 $\pm$ $1.7$ &   2.1$^{\rm +2.5}_{-1.1}$  
& $<$7 & --22 $\pm$ $2$ &  abs. &  ... \\
WRAY 15-1702 &    M6III & 3240  & 13.9 $\pm$ $0.2$    & 12.6 $\pm$ $0.2$    & --0.24 $\pm$ $0.29$  & 0.0$^{\rm +0.1}_{-0.0}$ &   3.4$^{\rm +0.4}_{-0.4}$  
& $<$7 &  --26 $\pm$ $2$ & abs. &  ... \\
WRAY 15-770 &   M7III & 3150  & 16.5 $\pm$ $1.0$    & 15.2 $\pm$ $1.0$    & --0.16 $\pm$ $1.4$  & 0$^{\rm +3.9}_{-0}$ &   11$^{\rm +62}_{-9.6}$         
& $<$7 & 23 $\pm$ $3$ & abs. &  ... \\
HD 305773 &  B1Ib &  20~800  &  ~9.2 $\pm$ $0.1$    & ~9.1 $\pm$ $0.1$    &  0.27 $\pm$ $0.15$  &  0.8 $\pm$ $0.5$   &  6.6$^{\rm +1.6}_{-1.3}$  
& 27 $\pm$ 5 &  --2 $\pm$ $1$ & abs. & ...\\[2pt]
\hline 
\end{tabular}
\tablefoot {Column~(3):  $T_{\rm eff}$ from Lang et~al. 1991 (adapted from \mbox{Schmidt-Kaler} \cite{Schm82}).  
Columns~(4) and~(5): photometry in the $B$ and $V$~bands taken from the NOMAD catalog,
except for Hen~2-80,  Th~17-35, and CD-38~4380 where they are from Vieira et~al. (\cite{Viei03}) and Hen~3-1121N where they are from the GSC~2.3.2.
Columns~(6) and~(7): \mbox{Schmidt-Kaler} (\cite{Schm82}) intrinsic colors and absolute magnitudes of were used to calculate $E(B-V)$ and the distance. The absolute magnitudes for the M6III and M7III~stars are absent from the \mbox{Schmidt-Kaler} (\cite{Schm82}) tables. We deduced them by linear extrapolation of the~$M_V$ of the M3III and M4III~spectral types. 
Column~(6): $^\star$ in the case of Hen~3-1121N the $R$~= 12.1~$\pm$ $0.4$ band magnitude was used to derive $E(B-V)$ using $E(B-V)= E(V-R)/0.78$.  
Column~(7): no~correction for extinction was applied to sources with $E(B-V) < 0$.
Columns~(9) and~(10): $^*$~when the spectra are dominated by emission lines and almost no absorption lines are observed no constrain for $v ~{\rm sin}(i)$ is given and the~$v_r$ estimate is based on the averaged velocity shift of emission lines (principally~\ion{He}{i}).
Column~(11): the~type of the H$\alpha$~profile is given following the classification of Reipurth et~al. (\cite{Reip96}) and Vieira et~al. (\cite{Viei03}): type~I profiles are symmetric without, or~with only very shallow absorption features; type~II profiles are double-peaked with the secondary peak having more than half of the strength of the primary; type~III profiles are double-peaked, 
with the secondary peak having less than half the strength of the primary; type~IV profiles have P~Cygni line characteristics.
Column~(12):  F.L.~means forbidden lines.  [\ion{O}{i}]~refers to the detection of [\ion{O}{i}]~lines at~6301, 6365, or 8446~\AA;  [\ion{S}{ii}] refers to the [\ion{S}{ii}]~line at~6716 and 6731~\AA; [\ion{N}{ii}]~refers to the lines at~6549 and 6585~\AA.} 
\vspace*{3mm}\end{table}