Table 3: H $\alpha$ equivalent widths, T Tauri classification, spectral types, effective temperatures and distances of the stars studied as found in the literature and used to calculate the stellar luminosities and infrared excesses.

Star
EW(H $\alpha$ ) TTS Ref. Sp. T. Ref. T $A_{\rm {V}}$ Ref. d Ref. L_* $\lambda$ $_{\rm IR}$ ^a $L_{\rm exc.}$ IR $_{\rm exc.}$ ^b co.^c

[Å] [K] [pc] [ $L_{\odot }$ ] [ $\mu$ m] [ $L_{\odot }$ ] o l

T Cha
- w 1 G8 1 5445 1.27 C 140 2 1.71 3.5 0.63 0.36 0.13 n

Sz 68
2-7 w 3 K2 3/4 4955 1.09 C 150 3 4.59 3.5 1.60 0.35 0.30 y

RU Lup
216.4 c 5 K7-M0 6 3963 0.20 6 127 7 1.27 3.5 0.68 0.53 0.48 n

EX Lup
43.3 c 5 M0.5 5 3802 ? 18 125 5 0.47 3.5 0.17 0.35 - n

Sz 124
1.6 w 5 M0 5 3917 0.22 C 125 5 0.21 3.5 0.17 0.81 - y

ROX 2
2.8 w 8 M0 8 3917 3.32 C 170 8 1.01 12.0 2.23 2.20 0.91 y

DoAr 24
20.0 c 8 K5 8 4395 3.15 C 170 8 1.58 4.8 3.42 2.17 0.05 n

DoAr 24E
5.0 w 8 K0 8 5236 5.84 C 170 8 8.50 3.5 3.97 0.47 0.08 y

SR 12
3.6 w 9 M2.5 10 3428 0.46 C 170 8 0.91 12.0 2.41 2.65 1.71^s y

ROX 31
3.3 w 8 K7 8 4000 4.20 C 170 8 0.48 4.8 0.55 1.15 0.33 y

Wa Oph/4
0.6 w 11 K4 11 4581 2.40 C 150 11 1.00 4.8 0.11 0.11 0.04 y

Wa Oph/6
35.0 c 11 K7 12 4000 1.24 C 150 11 0.67 4.8 0.64 0.96 0.23 n

IX Oph
1.3 w 9 G 13 5902 2.29 C 125 14 2.80 3.5 0.06 0.02 - n

V1725 Oph
6.5 w 15 M0.5 15 3802 1.08 15 225 15 0.63 4.8 0.86 1.37 - n?

CoKu Ser G1
3.3 w 9 K7 9 4000 3.48 9 350 16 0.60 4.8 2.21 3.70 2.24 y

CoKu Ser G7
5.5 w 9 M0 9 3917 3.72 9 350 16 0.82 4.8 20.09 24.52 0.65 n?

V536 Aql
51.8 c 9/3 K7 3 4000 1.43 C 200 3 0.72 4.8 1.79 2.48 0.47 y

MacC H3
11.4 c 9 K2 4 4955 0.53 C 845 17 1.83 7.7 3.03 1.66 0.85 n

Notes to Table 7: "C'' in the extinction's reference column indicates we have calculated it for this paper from the photometry and the spectral type. Otherwise the reference is given.
^a Wavelength (in $\mu$ m) from where the infrared luminosity excess was calculated (to infinite wavelength);
^b IR $_{\rm exc.}$ = ( $L_{\rm IR}$ - $L_{\rm bb}$ ) / L_*; (o) are the excesses calculated over the continuous line representing the star, seen in each graph (Figs. 1 to 6); (l) are the lower limits obtained for the excesses. "s'' indicates the infrared excess is over the luminosity of the binary system. Details on how each infrared excess for individual stars was obtained, can be found in Sect. 3;
^c If the star is believed to have a companion nearby (y) or not (n), according to the literature. "n?'' no companion has been reported but we believe there could be one.
References: (1) Alcalá et al. (1993), (2) Siebenmorgen et al. (2000), (3) Geoffray & Monin (2001), (4) Herbig-Bell Catalogue (HBC), (5) Appenzeller et al. (1983), (6) Stempels & Piskunov (2002), (7) Favata et al. (1998), (8) Bouvier & Appenzeller (1992), (9) Cohen & Kuhi (1979), (10) Rydgren et al. (1976), (11) Walter (1986), (12) Chavarría (2000), (13) Covino et al. (1992), (14) Reipurth et al. (1996), (15) Reipurth & Gee (1986), (16) Brown et al. (2000), (17) de Zeeuw et al. (1999), (18) Herbig et al. (2001).

**Table 3:** H $\alpha$ equivalent widths, T Tauri classification, spectral types, effective temperatures and distances of the stars studied as found in the literature and used to calculate the stellar luminosities and infrared excesses.
Star	EW(H $\alpha$ )	TTS	Ref.	Sp. T.	Ref.	T	$A_{\rm {V}}$	Ref.	d	Ref.	L_*	$\lambda$ $_{\rm IR}$ ^a	$L_{\rm exc.}$	IR $_{\rm exc.}$ ^b	co.^c
	[Å]					[K]			[pc]		[ $L_{\odot }$ ]	[ $\mu$ m]	[ $L_{\odot }$ ]	o	l
T Cha	-	w	1	G8	1	5445	1.27	C	140	2	1.71	3.5	0.63	0.36	0.13	n
Sz 68	2-7	w	3	K2	3/4	4955	1.09	C	150	3	4.59	3.5	1.60	0.35	0.30	y
RU Lup	216.4	c	5	K7-M0	6	3963	0.20	6	127	7	1.27	3.5	0.68	0.53	0.48	n
EX Lup	43.3	c	5	M0.5	5	3802	?	18	125	5	0.47	3.5	0.17	0.35	-	n
Sz 124	1.6	w	5	M0	5	3917	0.22	C	125	5	0.21	3.5	0.17	0.81	-	y
ROX 2	2.8	w	8	M0	8	3917	3.32	C	170	8	1.01	12.0	2.23	2.20	0.91	y
DoAr 24	20.0	c	8	K5	8	4395	3.15	C	170	8	1.58	4.8	3.42	2.17	0.05	n
DoAr 24E	5.0	w	8	K0	8	5236	5.84	C	170	8	8.50	3.5	3.97	0.47	0.08	y
SR 12	3.6	w	9	M2.5	10	3428	0.46	C	170	8	0.91	12.0	2.41	2.65	1.71^s	y
ROX 31	3.3	w	8	K7	8	4000	4.20	C	170	8	0.48	4.8	0.55	1.15	0.33	y
Wa Oph/4	0.6	w	11	K4	11	4581	2.40	C	150	11	1.00	4.8	0.11	0.11	0.04	y
Wa Oph/6	35.0	c	11	K7	12	4000	1.24	C	150	11	0.67	4.8	0.64	0.96	0.23	n
IX Oph	1.3	w	9	G	13	5902	2.29	C	125	14	2.80	3.5	0.06	0.02	-	n
V1725 Oph	6.5	w	15	M0.5	15	3802	1.08	15	225	15	0.63	4.8	0.86	1.37	-	n?
CoKu Ser G1	3.3	w	9	K7	9	4000	3.48	9	350	16	0.60	4.8	2.21	3.70	2.24	y
CoKu Ser G7	5.5	w	9	M0	9	3917	3.72	9	350	16	0.82	4.8	20.09	24.52	0.65	n?
V536 Aql	51.8	c	9/3	K7	3	4000	1.43	C	200	3	0.72	4.8	1.79	2.48	0.47	y
MacC H3	11.4	c	9	K2	4	4955	0.53	C	845	17	1.83	7.7	3.03	1.66	0.85	n

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations
	3 Results
	4 Discussion
	5 Conclusions
	Appendix A: New photometry reduced for this paper
	Appendix B: Photometry used for the SEDs from previous papers
	References