Table 4: List of known secondaries to the T Tauri stars in our sample.
Star
EW(H $\alpha$ )^a T^a $A_{\rm {V}}$ ^a L_*^b $L_{\rm exc.}$ ^c IR $_{\rm exc.}$ ^c d^d

[Å] [K] [ $L_{\odot }$ ] [ $L_{\odot }$ ] [L_*] [ $\hbox{$^{\prime\prime}$ }$ ]

Sz 68-B - 4000 0.75 0.13 1.5 11.2 2.7

Sz 124SE - - - - - - 13.6

ROX 2-B - - - - - - 0.41

DoAr 24E-B - - - 1.40 - - 2.3

SR 12B - 2500 - 0.50 2.4 4.8 0.3

ROX 31-B - - - - - - 0.39

Wa Oph/4-B - - - - - - 8.7

B62-H $\alpha$ 2^e 19 3500 - 0.43 - - 30

HBC 666^f 14 - - - - - 3.5

V536 Aql-B - - - - - - 0.52

Notes to table:
^a References for the H $\alpha$ equivalent width, temperature and extinction can be found in the corresponding entry for each star in Sect. 3.
^b The stellar luminosities were obtained from the corresponding black body curves fitted to the available photometry for each star, except for DoAr24E-B, which is from Chelli et al. (1988). $A_{\rm {V}}$ was taken to be zero unless otherwise stated.
^c The infrared luminosity excess ( $L_{\rm exc.}$ ) and IR $_{\rm exc.}$ have been calculated over the same range as the main star.
^d d is the angular distance from the companion to the primary.
^e This star is not really a companion but a star near V1725 Oph, associated with the same globule Barnard 62 (Reipurth & Gee 1986; Weaver & Jones 1992).
^f Companion of CoKu Ser/G1, also known as CoKu Ser/G1/c (Cohen & Kuhi 1979).

**Table 4:** List of known secondaries to the T Tauri stars in our sample.
Star	EW(H $\alpha$ )^a	T^a	$A_{\rm {V}}$ ^a	L_*^b	$L_{\rm exc.}$ ^c	IR $_{\rm exc.}$ ^c	d^d
	[Å]	[K]		[ $L_{\odot }$ ]	[ $L_{\odot }$ ]	[L_*]	[ $\hbox{$^{\prime\prime}$ }$ ]
Sz 68-B	-	4000	0.75	0.13	1.5	11.2	2.7
Sz 124SE	-	-	-	-	-	-	13.6
ROX 2-B	-	-	-	-	-	-	0.41
DoAr 24E-B	-	-	-	1.40	-	-	2.3
SR 12B	-	2500	-	0.50	2.4	4.8	0.3
ROX 31-B	-	-	-	-	-	-	0.39
Wa Oph/4-B	-	-	-	-	-	-	8.7
B62-H $\alpha$ 2^e	19	3500	-	0.43	-	-	30
HBC 666^f	14	-	-	-	-	-	3.5
V536 Aql-B	-	-	-	-	-	-	0.52

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