Table 3:

Established spectral type, literature photometry, estimated distance, radial and projected rotational velocity, observed H and forbidden line emission.

			B	V	E(B-V)	AV			vr
Star	Sp.Type	[K]	[mag]	[mag]	[mag]	[mag]	[kpc]	[km s-1]	[km s-1]	H	F.L.
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)
Confirmed Herbig Ae/Be and T Tauri stars
Hen 3-1121S	B0Ve	30 000	11.6 0.1	11.1 0.1	0.85 0.14	2.7 0.5	3.1	240 20	-28 5	I	[O I]
Hen 3-1121N	B0.5Ve	27 500	...	13.0 0.4	1.3	4.1 2.3	3.2	245 20	-58 5	I	[O I] [N II]
MWC 878	B1Ve	25 400	11.2 0.1	10.8 0.1	0.74 0.15	2.3 0.5	2.1	...	-11 3*	I	[O I] [N II]
WRAY 15-1435	B1Ve	25 400	12.8 0.5	12.0 0.5	1.0 0.7	3.2 2.2	2.6	230 20	-30 10	I	[O I]
MWC 953	B2Ve	22 000	12.0 0.2	10.9 0.1	1.3 0.2	4.0 0.7	0.8	<7	23 2	II	[O I]
HD 313571	B3Ve	18 700	10.3 0.1	9.9 0.1	0.57 0.15	1.8 0.5	0.9	380 20	-50 20	I	[O I]
Hen 3-823	B3Ve	18 700	10.5 0.1	10.4 0.1	0.33 0.15	1.0 0.5	1.6	310 20	-10 10	II	[O I]
MWC 593	B4Ve	17 000	10.5 0.1	10.0 0.1	0.65 0.15	2.1 0.5	0.7	330 30	-20 10	I	[O I]
Hen 2-80	B6Ve	14 000	14.0 0.1	13.2 0.1	0.97 0.15	3.0 0.5	1.6	60 10	-22 3	II	[O I][S II]
WRAY 15-1372	B6Ve	14 000	11.7 0.1	11.1 0.1	0.80 0.15	2.5 0.5	0.8	280 20	-30 10	II	...
Th 17-35	B8Ve	11 900	13.9 0.1	13.5 0.1	0.58 0.15	1.8 0.5	2.4	210 20	-10 5	I	[O I]
HD 145718	A5Ve	8200	9.3 0.1	8.9 0.1	0.24 0.15	0.8 0.5	0.17	100 10	0 3	IV	...
CD-38 4380	F4Ve	6590	10.4 0.1	10.0 0.1	0.0 0.15	0.0	0.19	45 4	20 2	I	...
Hen 3-1145	M1IVe	3720	15.3 0.1	14.0 0.1	-0.15 0.15	0.0	0.16	<7	-2 1	I	[O I]
Giant stars with emission lines that may be Herbig Ae/Be stars
HD 152291	B1IIIe	24 000	9.0 0.1	9.0 0.1	0.28 0.15	0.9 0.5	3.1	320 20	-20 10	II	...
Hen 3-416	A1IIIe	9480	11.9 0.2	10.8 0.1	1.0 0.2	3.3 0.7	0.29	30 5	33 4	III, IV	[O I]
WRAY 15-488	F2IIIe	6870	10.3 0.1	9.8 0.1	0.11 0.15	0.3 0.5	0.36	30 5	-2 2	IV	...
Giant and Supergiant stars with emission lines
HD 323154	B4IIe	15 500	10.2 0.1	9.3 0.1	1.10 0.15	3.4 0.5	1.1	55 5	75 4	I	...
WRAY 15-1104	B1Iae	20 800	11.0 0.1	10.8 0.1	0.40 0.15	1.2 0.5	20	50 5	60 5	IV	[O I]
Hen 3-1428	B1Iae	20 800	11.3 0.1	10.9 0.1	0.61 0.15	1.9 0.5	15	38 5	30 5	I	[O I] [N II]
MWC 314	B3Ibe	16 200	11.1 0.1	9.8 0.1	1.45 0.15	4.5 0.5	1.5	40 5	65 10	I	[O I] [N II]
HD 320156	B4Ibe	14 900	10.5 0.1	9.9 0.1	0.72 0.15	2.3 0.5	4.2	35 5	60 3	I	[O I] [N II]
Hen 3-1347	B5Ibe	13 600	11.9 0.2	11.5 0.2	0.56 0.28	1.8 0.9	10	30 5	-15 5	IV	[O I]
AS 231	B9Iae	10 300	12.6 0.6	10.2 0.1	2.4 0.6	7.5 1.9	0.9	28 5	-25 5	IV	...
Stars with strong emission line spectrum
WRAY 15-1651	B1-B5	...	17.0 0.2	15.8 0.2	...	...	...	...	...	I	[O I]
MWC 930	B5-B9	...	14.6 0.5	12.8 0.5	...	...	...	70 10	10 10	IV	[O I]
Dwarf stars without H in emission
AS 321	A5V	8200	12.0 0.1	11.3 0.1	0.60 0.23	1.9 0.7	0.31	150 10	-30 5	abs.	[O I]
Giant and Supergiant stars without H in emission
WRAY 15-522	G9III	4820	14.3 0.6	13.4 0.6	-0.03 0.8	0.0	3.3	<7	-9 2	abs.	[O I]
Th 35-41	M1III	3720	14.5 0.1	13.1 0.6	-0.17 0.6	0.0	5.1	13 4	15 2	abs.	...
WRAY 15-566	M6III	3240	16.0 0.4	14.2 0.8	0.31 0.90	1.0 2.8	4.6	<7	29 2	abs.	...
WRAY 15-1650	M6III	3240	13.5 0.5	11.9 0.2	0.13 0.54	0.4 1.7	2.1	<7	-22 2	abs.	...
WRAY 15-1702	M6III	3240	13.9 0.2	12.6 0.2	-0.24 0.29	0.0	3.4	<7	-26 2	abs.	...
WRAY 15-770	M7III	3150	16.5 1.0	15.2 1.0	-0.16 1.4	0	11	<7	23 3	abs.	...
HD 305773	B1Ib	20 800	9.2 0.1	9.1 0.1	0.27 0.15	0.8 0.5	6.6	27 5	-2 1	abs.	...

Notes. Column (3): from Lang et al. 1991 (adapted from Schmidt-Kaler 1982). 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. (2003) and Hen 3-1121N where they are from the GSC 2.3.2. Columns (6) and (7): Schmidt-Kaler (1982) 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 Schmidt-Kaler (1982) tables. We deduced them by linear extrapolation of the M_V of the M3III and M4III spectral types. Column (6): in the case of Hen 3-1121N the R = 12.1  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 is given and the v_r estimate is based on the averaged velocity shift of emission lines (principally He I). Column (11): the type of the H profile is given following the classification of Reipurth et al. (1996) and Vieira et al. (2003): 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. [O I] refers to the detection of [O I] lines at 6301, 6365, or 8446 Å; [S II] refers to the [S II] line at 6716 and 6731 Å; [N II] refers to the lines at 6549 and 6585 Å.