Table 4: The [O I]parameters for each sample source. The objects are listed according to their IR-SED classification. The distance to the source, the effective temperature, UV luminosity and bolometric (= integrated observed) luminosity are given. References for the first two values can be found in Table 6 of AV04, unless otherwise indicated: ^A de Zeeuw et al. (1999); ^B Finkenzeller (1985); ^C Gray & Corbally (1993); ^D Gray & Corbally (1998); ^E Houk (1978); ^F Mora et al. (2001); ^G Vieira et al. (2003); ^H van den Ancker et al. (1998). The type of [O I] 6300 Å emission profile observed in each object has been indicated; E: pure-emission profile, A: 6300 Å region rich in photospheric absorption lines, U: undetected feature (upper limit). n.s.: no spectrum available. The typical errors on the FWHM and centroid position are $\pm$ 8 and $\pm$ 15 ${\rm km}~{\rm s}^{-1}$ respectively. The thirth column contains the stellar radial velocity employed in this study. This value is estimated from the available spectra, unless otherwise indicated: ^a Arce & Goodman (2002); ^b Arellano Ferro & Giridhar (2003); ^c Barbier-Brossat & Figon (2000); ^d Dunkin et al. (1997a); ^e Piétu et al. (2003); ^f Reipurth et al. (1996); ^g Yonekura et al. (1997, based on CO lines). $^\dagger$ Based on Ca II lines. $\circlearrowright$ Average of radial velocities of stars in the same field (radius $\sim$ 2 $^\prime$ ). The last two columns of the table give the type and EW of the observed H $\alpha$ profile; S: single-peaked; D: double-peaked; P: P Cygni-like; inv. P: inversed P Cyg-like. When no spectrum was available, literature values were used: ^h Arellano Ferro & Giridhar (2003); ⁱ de Winter & Thé (1990); ^j Dunkin et al. (1997a); ^k Dunkin et al. (1997b); ^l Finkenzeller & Mundt (1984); ^m Merín et al. (2004); ⁿ Pérez & Grady (1997).
[O I]6300 Å [O I]6363 Å H $\alpha$

Object Distance $\log T_{\rm eff}$ $\log L_{\rm uv}$ $\log L_{\rm bol}$ $v_{\rm rad}$ Profile EW L FWHM Centroid EW FWHM Profile EW

[pc] $\log$ [K] $\log\ [L_\odot]$ $\log\ [L_\odot]$ [ ${\rm km}~{\rm s}^{-1}$ ] [Å] [ $L_\odot$ ] [ ${\rm km}~{\rm s}^{-1}$ ] [ ${\rm km}~{\rm s}^{-1}$ ] [Å] [ ${\rm km}~{\rm s}^{-1}$ ] [Å]

Group I

V376 Cas 630 4.19 1.60 2.58 -28^g E -0.7 $\pm$ 0.2 $8.6 \times 10^{-4}$ 131 -28 | EW| < 0.7 D -29.7

AB Aur 144 3.98 1.56 1.71 9 E -0.16 $\pm$ 0.01 $6.4 \times 10^{-4}$ 20 15 -0.04 20 P -54.0

HD 34282 400 3.94 1.12 1.38 16^e U | EW| < 0.07 < $1.3 \times 10^{-4}$ n.s. n.s. D -4.7^m

HD 34700 336 3.77 0.91 1.42 -21^b A 0.25 $\pm$ 0.05 n.s. n.s. S -0.6^h

HD 36112 204^H 3.91^D 1.16 1.47 12 A 0.03 $\pm$ 0.01 | EW| < 0.02 P -19.7

HD 245185 336^A 3.95^D 0.93 1.29 24 E -0.20 $\pm$ 0.08 $2.2 \times 10^{-4}$ 26 8 | EW| < 0.1 D -29.5

HD 97048 180 4.00 1.54 1.42 21 E -0.16 $\pm$ 0.01 $5.3 \times 10^{-4}$ 24 2 -0.05 21 D -36.0

HD 100453 112 3.87 0.66 1.09 17 A 0.10 $\pm$ 0.01 | EW| < 0.02 D 1.5

HD 100546 103 4.02 1.42 1.62 18 E -0.19 $\pm$ 0.01 $4.2 \times 10^{-4}$ 25 3 -0.06 21 S -36.8

HD 135344 140 3.82 0.60 1.01 -1 A 0.07 $\pm$ 0.01 | EW| < 0.02 S -17.4

HD 139614 140 3.89 0.71 1.03 5 A 0.04 $\pm$ 0.01 | EW| < 0.02 S -9.8

HD 142527 145 3.80 0.83 1.34 $\circlearrowright{-9}$ A 0.26 $\pm$ 0.02 n.s. n.s. S -17.9ⁿ

CD-42 $^\circ$ 11721 400 4.47 3.93 3.03 -84^f E -1.77 $\pm$ 0.03 $9.8 \times 10^{-2}$ 42 65 n.s. n.s. S -199.5ⁱ

HD 169142 145 3.91 0.98 1.13 -3^d E -0.05 $\pm$ 0.02 $7.6 \times 10^{-5}$ 22 3 n.s. n.s. S -14.0^k

T Cra 130 3.86 -0.44 0.88 0^f E -0.21 $\pm$ 0.04 $1.6 \times 10^{-5}$ 25 0 n.s. n.s. D -10.7

HD 179218 240 4.02 1.91 1.88 -9 E -0.05 $\pm$ 0.01 $3.4 \times 10^{-4}$ 43 19 -0.03 29 S -18.2

BD+40 $^\circ$ 4124 980 4.34 3.77 2.50 14 E -0.86 $\pm$ 0.01 $6.1 \times 10^{-2}$ 46 -38 -0.26 41 D -119.9

HD 200775 440 4.29 3.80 2.84 8 E -0.09 $\pm$ 0.01 $9.3 \times 10^{-3}$ 95 -15 -0.04 107 D -74.6

MWC 1080 2200 4.48 5.25 3.76 -4 E -0.17 $\pm$ 0.02 $1.9 \times 10^{-1}$ 61 -70 -0.03 42 P -122.8

Group II

VX Cas 630 3.97 1.37 1.45 7 E -0.13 $\pm$ 0.02 $3.6 \times 10^{-4}$ 49 -25 -0.07 59 D -12.9

HD 31648 131 3.94 0.99 1.22 11 U | EW| < 0.02 < $2.7 \times 10^{-5}$ | EW| < 0.02 P -18.3

HD 35929 510^A 3.86^D 1.81 1.95 15 $^\dagger$ A 0.15 $\pm$ 0.03 n.s. n.s. S -4.8

HD 244604 336^A 3.98^D 1.36 1.35 21 U | EW| < 0.04 < $1.0 \times 10^{-4}$ | EW| < 0.03 D -15.0

V586 Ori 510^A 3.97^C 1.50 1.61 26^f E -0.06 $\pm$ 0.02 $2.3 \times 10^{-4}$ 61 -4 n.s. n.s. D -17.1

BF Ori 510 3.95 1.39 1.38 26^f U | EW| < 0.14 < $4.4 \times 10^{-4}$ n.s. n.s. D -9.3

HD 95881 118 3.95 0.70 0.99 36 $^\dagger$ E -0.12 $\pm$ 0.02 $7.6 \times 10^{-5}$ 76 -10 n.s. n.s. D -21.1

HD 98922 >540^H 4.02^E 2.86 2.95 -15 $^\dagger$ E -0.13 $\pm$ 0.01 $7.9 \times 10^{-3}$ 34 25 n.s. n.s. P -27.9

HD 101412 160^A 4.02^G 1.53 1.40 $\circlearrowright{-3}$ E -0.12 $\pm$ 0.03 $3.4 \times 10^{-4}$ 63 26 n.s. n.s. D -20.4

HD 104237 116 3.92 1.36 1.53 13 A 0.06 $\pm$ 0.01 | EW| < 0.02 D -24.5

HD 141569 99 3.98 1.16 1.10 -2 E -0.18 $\pm$ 0.01 $2.9 \times 10^{-4}$ 154 10 -0.09 158 D -6.7

HD 142666 145 3.88 0.91 1.03 3^d A 0.07 $\pm$ 0.02 n.s. n.s. D -3.2^j

HD 144432 145 3.87 0.77 1.13 2^d U | EW| < 0.04 < $4.7 \times 10^{-5}$ n.s. n.s. P -9.0^j

HR 5999 210 3.90 1.74 1.98 16 $^\dagger$ U | EW| < 0.04 < $3.8 \times 10^{-4}$ n.s. n.s. D -11.0

HD 150193 150 3.95 1.23 1.19 -6^f U | EW| < 0.04 < $8.8 \times 10^{-5}$ n.s. n.s. P -5.0^l

AK Sco 150 3.81 0.63 0.89 0^f A 0.18 $\pm$ 0.03 n.s. n.s. D -9.4

HD 163296 122 3.94 1.22 1.52 -4^c U | EW| < 0.04 < $9.2 \times 10^{-5}$ n.s. n.s. D -14.5^l

VV Ser 330 3.95 1.13 1.37 -4 E -0.73 $\pm$ 0.04 $1.2 \times 10^{-3}$ 50 -25 -0.21 47 D -81.3

R CrA 130 3.86 -0.45 3.46 0^f E -0.5 $\pm$ 0.1 $3.8 \times 10^{-5}$ 32 -20 n.s. n.s. D -44.3

WW Vul 440 3.98 1.32 1.30 2 E -0.07 $\pm$ 0.02 $1.6 \times 10^{-4}$ 60 -42 | EW| < 0.05 D -24.0

HD 190073 >290^H 3.95^F 1.72 1.92 3 E -0.07 $\pm$ 0.02 $4.7 \times 10^{-4}$ 25 -12 -0.01 13 P -27.1

LkH $\alpha$ 224 980 3.89 1.86 2.32 6 U | EW| < 0.15 < $1.9 \times 10^{-3}$ | EW| < 0.2 P -17.6

BD+46 $^\circ$ 3471 1200 3.99 2.50 2.43 8 E -0.04 $\pm$ 0.01 $1.3 \times 10^{-3}$ 48 -36 | EW| < 0.04 P -21.7

SV Cep 440 3.97 1.02 1.39 4 E -0.12 $\pm$ 0.01 $1.5 \times 10^{-4}$ 63 -34 -0.05 46 inv. P -10.1

IL Cep 690^H 4.27^B 3.76 2.18 1 U | EW| < 0.02 < $2.1 \times 10^{-3}$ | EW| < 0.05 D -34.5

Group III

Z CMa 1050 4.48 5.13 3.71 36 E -4.3 $\pm$ 0.2 3.8 421 -249 -1.08 695 P -45.2

MWC 297 250 4.37 4.01 2.69 -16 E -6.91 $\pm$ 0.02 $7.1 \times 10^{-1}$ 22 5 -1.56 21 S -355.3

LkH $\alpha$ 225 980 3.86 2.37 3.26 6 E -0.3 $\pm$ 0.1 $1.4 \times 10^{-2}$ 65 -51 | EW| < 0.2 U

PV Cep 440 3.91 0.76 1.92 -18^a E -2.9 $\pm$ 0.1 $2.7 \times 10^{-3}$ 321 -164 | EW| < 0.9 P -49.9

V645 Cyg 3500 4.58 4.42 4.61 -14 E -5.4 $\pm$ 0.6 $6.5 \times 10^{-1}$ 423 -257 -1.44 390 D -121.7

**Table 4:** The [O I]parameters for each sample source. The objects are listed according to their IR-SED classification. The distance to the source, the effective temperature, UV luminosity and bolometric (= integrated *observed*) luminosity are given. References for the first two values can be found in Table 6 of AV04, unless otherwise indicated: ^A de Zeeuw et al. (1999); ^B Finkenzeller (1985); ^C Gray & Corbally (1993); ^D Gray & Corbally (1998); ^E Houk (1978); ^F Mora et al. (2001); ^G Vieira et al. (2003); ^H van den Ancker et al. (1998). The type of [O I] 6300 Å emission profile observed in each object has been indicated; E: pure-emission profile, A: 6300 Å region rich in photospheric absorption lines, U: undetected feature (upper limit). n.s.: no spectrum available. The typical errors on the *FWHM* and centroid position are $\pm$ 8 and $\pm$ 15 ${\rm km}~{\rm s}^{-1}$ respectively. The thirth column contains the stellar radial velocity employed in this study. This value is estimated from the available spectra, unless otherwise indicated: ^a Arce & Goodman (2002); ^b Arellano Ferro & Giridhar (2003); ^c Barbier-Brossat & Figon (2000); ^d Dunkin et al. (1997a); ^e Piétu et al. (2003); ^f Reipurth et al. (1996); ^g Yonekura et al. (1997, based on CO lines). $^\dagger$ Based on Ca II lines. $\circlearrowright$ Average of radial velocities of stars in the same field (radius $\sim$ 2 $^\prime$ ). The last two columns of the table give the type and EW of the observed H $\alpha$ profile; S: single-peaked; D: double-peaked; P: P Cygni-like; inv. P: inversed P Cyg-like. When no spectrum was available, literature values were used: ^h Arellano Ferro & Giridhar (2003); ⁱ de Winter & Thé (1990); ^j Dunkin et al. (1997a); ^k Dunkin et al. (1997b); ^l Finkenzeller & Mundt (1984); ^m Merín et al. (2004); ⁿ Pérez & Grady (1997).
	[O I]6300 Å	[O I]6363 Å	H $\alpha$
Object	Distance	$\log T_{\rm eff}$	$\log L_{\rm uv}$	$\log L_{\rm bol}$	$v_{\rm rad}$	Profile	EW	L	FWHM	Centroid	EW	FWHM	Profile	EW
	[pc]	$\log$ [K]	$\log\ [L_\odot]$	$\log\ [L_\odot]$	[ ${\rm km}~{\rm s}^{-1}$ ]		[Å]	[ $L_\odot$ ]	[ ${\rm km}~{\rm s}^{-1}$ ]	[ ${\rm km}~{\rm s}^{-1}$ ]	[Å]	[ ${\rm km}~{\rm s}^{-1}$ ]		[Å]
Group I
V376 Cas	630	4.19	1.60	2.58	-28^g	E	-0.7 $\pm$ 0.2	$8.6 \times 10^{-4}$	131	-28	\| EW\| < 0.7		D	-29.7
AB Aur	144	3.98	1.56	1.71	9	E	-0.16 $\pm$ 0.01	$6.4 \times 10^{-4}$	20	15	-0.04	20	P	-54.0
HD 34282	400	3.94	1.12	1.38	16^e	U	\| EW\| < 0.07	< $1.3 \times 10^{-4}$			n.s.	n.s.	D	-4.7^m
HD 34700	336	3.77	0.91	1.42	-21^b	A	0.25 $\pm$ 0.05				n.s.	n.s.	S	-0.6^h
HD 36112	204^H	3.91^D	1.16	1.47	12	A	0.03 $\pm$ 0.01				\| EW\| < 0.02		P	-19.7
HD 245185	336^A	3.95^D	0.93	1.29	24	E	-0.20 $\pm$ 0.08	$2.2 \times 10^{-4}$	26	8	\| EW\| < 0.1		D	-29.5
HD 97048	180	4.00	1.54	1.42	21	E	-0.16 $\pm$ 0.01	$5.3 \times 10^{-4}$	24	2	-0.05	21	D	-36.0
HD 100453	112	3.87	0.66	1.09	17	A	0.10 $\pm$ 0.01				\| EW\| < 0.02		D	1.5
HD 100546	103	4.02	1.42	1.62	18	E	-0.19 $\pm$ 0.01	$4.2 \times 10^{-4}$	25	3	-0.06	21	S	-36.8
HD 135344	140	3.82	0.60	1.01	-1	A	0.07 $\pm$ 0.01				\| EW\| < 0.02		S	-17.4
HD 139614	140	3.89	0.71	1.03	5	A	0.04 $\pm$ 0.01				\| EW\| < 0.02		S	-9.8
HD 142527	145	3.80	0.83	1.34	$\circlearrowright{-9}$	A	0.26 $\pm$ 0.02				n.s.	n.s.	S	-17.9ⁿ
CD-42 $^\circ$ 11721	400	4.47	3.93	3.03	-84^f	E	-1.77 $\pm$ 0.03	$9.8 \times 10^{-2}$	42	65	n.s.	n.s.	S	-199.5ⁱ
HD 169142	145	3.91	0.98	1.13	-3^d	E	-0.05 $\pm$ 0.02	$7.6 \times 10^{-5}$	22	3	n.s.	n.s.	S	-14.0^k
T Cra	130	3.86	-0.44	0.88	0^f	E	-0.21 $\pm$ 0.04	$1.6 \times 10^{-5}$	25	0	n.s.	n.s.	D	-10.7
HD 179218	240	4.02	1.91	1.88	-9	E	-0.05 $\pm$ 0.01	$3.4 \times 10^{-4}$	43	19	-0.03	29	S	-18.2
BD+40 $^\circ$ 4124	980	4.34	3.77	2.50	14	E	-0.86 $\pm$ 0.01	$6.1 \times 10^{-2}$	46	-38	-0.26	41	D	-119.9
HD 200775	440	4.29	3.80	2.84	8	E	-0.09 $\pm$ 0.01	$9.3 \times 10^{-3}$	95	-15	-0.04	107	D	-74.6
MWC 1080	2200	4.48	5.25	3.76	-4	E	-0.17 $\pm$ 0.02	$1.9 \times 10^{-1}$	61	-70	-0.03	42	P	-122.8
Group II
VX Cas	630	3.97	1.37	1.45	7	E	-0.13 $\pm$ 0.02	$3.6 \times 10^{-4}$	49	-25	-0.07	59	D	-12.9
HD 31648	131	3.94	0.99	1.22	11	U	\| EW\| < 0.02	< $2.7 \times 10^{-5}$			\| EW\| < 0.02		P	-18.3
HD 35929	510^A	3.86^D	1.81	1.95	15 $^\dagger$	A	0.15 $\pm$ 0.03				n.s.	n.s.	S	-4.8
HD 244604	336^A	3.98^D	1.36	1.35	21	U	\| EW\| < 0.04	< $1.0 \times 10^{-4}$			\| EW\| < 0.03		D	-15.0
V586 Ori	510^A	3.97^C	1.50	1.61	26^f	E	-0.06 $\pm$ 0.02	$2.3 \times 10^{-4}$	61	-4	n.s.	n.s.	D	-17.1
BF Ori	510	3.95	1.39	1.38	26^f	U	\| EW\| < 0.14	< $4.4 \times 10^{-4}$			n.s.	n.s.	D	-9.3
HD 95881	118	3.95	0.70	0.99	36 $^\dagger$	E	-0.12 $\pm$ 0.02	$7.6 \times 10^{-5}$	76	-10	n.s.	n.s.	D	-21.1
HD 98922	>540^H	4.02^E	2.86	2.95	-15 $^\dagger$	E	-0.13 $\pm$ 0.01	$7.9 \times 10^{-3}$	34	25	n.s.	n.s.	P	-27.9
HD 101412	160^A	4.02^G	1.53	1.40	$\circlearrowright{-3}$	E	-0.12 $\pm$ 0.03	$3.4 \times 10^{-4}$	63	26	n.s.	n.s.	D	-20.4
HD 104237	116	3.92	1.36	1.53	13	A	0.06 $\pm$ 0.01				\| EW\| < 0.02		D	-24.5
HD 141569	99	3.98	1.16	1.10	-2	E	-0.18 $\pm$ 0.01	$2.9 \times 10^{-4}$	154	10	-0.09	158	D	-6.7
HD 142666	145	3.88	0.91	1.03	3^d	A	0.07 $\pm$ 0.02				n.s.	n.s.	D	-3.2^j
HD 144432	145	3.87	0.77	1.13	2^d	U	\| EW\| < 0.04	< $4.7 \times 10^{-5}$			n.s.	n.s.	P	-9.0^j
HR 5999	210	3.90	1.74	1.98	16 $^\dagger$	U	\| EW\| < 0.04	< $3.8 \times 10^{-4}$			n.s.	n.s.	D	-11.0
HD 150193	150	3.95	1.23	1.19	-6^f	U	\| EW\| < 0.04	< $8.8 \times 10^{-5}$			n.s.	n.s.	P	-5.0^l
AK Sco	150	3.81	0.63	0.89	0^f	A	0.18 $\pm$ 0.03				n.s.	n.s.	D	-9.4
HD 163296	122	3.94	1.22	1.52	-4^c	U	\| EW\| < 0.04	< $9.2 \times 10^{-5}$			n.s.	n.s.	D	-14.5^l
VV Ser	330	3.95	1.13	1.37	-4	E	-0.73 $\pm$ 0.04	$1.2 \times 10^{-3}$	50	-25	-0.21	47	D	-81.3
R CrA	130	3.86	-0.45	3.46	0^f	E	-0.5 $\pm$ 0.1	$3.8 \times 10^{-5}$	32	-20	n.s.	n.s.	D	-44.3
WW Vul	440	3.98	1.32	1.30	2	E	-0.07 $\pm$ 0.02	$1.6 \times 10^{-4}$	60	-42	\| EW\| < 0.05		D	-24.0
HD 190073	>290^H	3.95^F	1.72	1.92	3	E	-0.07 $\pm$ 0.02	$4.7 \times 10^{-4}$	25	-12	-0.01	13	P	-27.1
LkH $\alpha$ 224	980	3.89	1.86	2.32	6	U	\| EW\| < 0.15	< $1.9 \times 10^{-3}$			\| EW\| < 0.2		P	-17.6
BD+46 $^\circ$ 3471	1200	3.99	2.50	2.43	8	E	-0.04 $\pm$ 0.01	$1.3 \times 10^{-3}$	48	-36	\| EW\| < 0.04		P	-21.7
SV Cep	440	3.97	1.02	1.39	4	E	-0.12 $\pm$ 0.01	$1.5 \times 10^{-4}$	63	-34	-0.05	46	inv. P	-10.1
IL Cep	690^H	4.27^B	3.76	2.18	1	U	\| EW\| < 0.02	< $2.1 \times 10^{-3}$			\| EW\| < 0.05		D	-34.5
Group III
Z CMa	1050	4.48	5.13	3.71	36	E	-4.3 $\pm$ 0.2	3.8	421	-249	-1.08	695	P	-45.2
MWC 297	250	4.37	4.01	2.69	-16	E	-6.91 $\pm$ 0.02	$7.1 \times 10^{-1}$	22	5	-1.56	21	S	-355.3
LkH $\alpha$ 225	980	3.86	2.37	3.26	6	E	-0.3 $\pm$ 0.1	$1.4 \times 10^{-2}$	65	-51	\| EW\| < 0.2		U
PV Cep	440	3.91	0.76	1.92	-18^a	E	-2.9 $\pm$ 0.1	$2.7 \times 10^{-3}$	321	-164	\| EW\| < 0.9		P	-49.9
V645 Cyg	3500	4.58	4.42	4.61	-14	E	-5.4 $\pm$ 0.6	$6.5 \times 10^{-1}$	423	-257	-1.44	390	D	-121.7

Source LaTeX | All tables | In the text

	1 Introduction
	2 The data set
	3 Analysis of the emission lines
	4 Interpretation
	5 Modeling the [O I] emission region
	6 Comparison with the observations
	7 Conclusions and discussion
	Appendix
	References