**Table 1:** Results for all objects. We list all observed objects grouped by membership (MBM12, in-cloud (in TA), off-cloud Taurus-Auriga (off TA), or Orion) and sorted in order of ascending right ascension. The object name is the most common one used in literature - in one case the Guide Star Catalog number was used. The second column gives the observing run in which the object was observed. The calculated period together with the 1 $\sigma$ error is given in the next column followed by periods as determined by other groups. In the next five columns, $v \sin i$ values from literature, the spectral type, the classification of the object (w: wTTS,c: cTTS,Z: ZAMS, MS: main sequence, ?: unknown) together with the relevant quantities for the lithium-test ( $W_{\lambda }({\rm Li})$ , $W_{\lambda }({\rm H}\alpha )$ ) are given. Negative values stand for emission, f means the absorption lines are partially filled by emission. The last columns give comments on the nature of the object where relevant (SB1/2: single/double-lined spectroscopic binary). For all values, the sources are given as footnotes at the bottom of the table.
Group	Run	Period	other P.	$v \sin i$	SpTy	Type	$W_{\lambda }({\rm Li})$	$W_{\lambda }({\rm H}\alpha )$	Remark
Object name		[days]	[days]	[km s^-1]			[mÅ]	[Å]
MBM12
RX J0255.4+2005	I	3.36 $\pm$ .17	6.22^l	10.0^a	K6^a	w	440^a	-1.26^a	see text
Lk ${\rm H}\alpha$ 262	I	1.27 $\pm$ .02	3.13(?)^l	-	M1 IIIeⁱ	c	412^a	-32.10^a	see text
Lk ${\rm H}\alpha$ 263	I	6.6 $\pm$ .48		-	M4^a	c	543^a	-32.90^a	see text
Lk ${\rm H}\alpha$ 264	I	7.4 $\pm$ .2	2.603^l	24.3^a	K5^a	c	836^a	-58.90^a	see text
E0255.3+2018	I	n.P.	0.505(?)^l	-	K4^a	w	499^a	-1.6^a
off TA
RX J0312.8-0414NW	I	n.P.		33^f	G0^b	w	350^b	0.2^b
RX J0312.8-0414SE	I	n.P.		11^f	G8^b	w	300^b	2.5^b
RX J0324.4+0231	I	4.7 $\pm$ .1		12^f	K5^b	w	330^b	-0.40^b
RX J0333.1+1036	I	n.P.		20^f	K3^b	w	320^b	-0.8^b
RX J0344.8+0359	I	1.34 $\pm$ .09		27^f	K3^b	w	300^b	0.3f^b
RX J0351.4+0953W	I	3.65 $\pm$ .2		7^f	K1^b	w	300^b	0.5f^b
RX J0407.3+0113S	I	n.P.		13^f	K3^b	w	350^b	0.5f^b
RX J0407.3+0113N	I	n.P.		29^f	G4^b	w	200^b	3.3^b
RX J0422.9+0141	I	n.P.		37/14^k	F8^f	Z	no/60^k	1.5^f	SB2, $P_{\rm orb}=5.368$ d^k
RX J0434.3+0226	I	n.P.		7^k	K4^b	w	300^b, 200^k	-0.8^b	SB1, $P_{\rm orb}=603$ d^k
RX J0444.7+0813	I	2.93 $\pm$ .11		17^f	K3^b	Z	280^b	-0.8^b
1RXS J044534.0+120917	I	3.35 $\pm$ .15		-	-	?	-	-
RX J0445.5+1207	I	6.34 $\pm$ .05		83^f	K7^b	w	350^b	-2.0^b
RX J0450.0+0151	I	2.23 $\pm$ .03		67^f	K3^b	w	350^b	0.5f^b
RX J0528.9+1046	I	7.04 $\pm$ .36		10,9^k	K3^k	Z	270/150^k	0.1f^b	SB2, $P_{\rm orb}=7.672$ d^k
RX J0529.3+1210	I, II	2.14 $\pm$ .20		18^k	K7-M0^b	w	350^b, 270^k	-2.0^b	SB1, $P_{\rm orb}=462.8$ d^k
in TA
RX J0403.4+1725	II	0.574 $\pm$ .001		112^c	K3^c	w	487^c	-0.5^d	SB1
RX J0406.8+2541	II, III	1.70 $\pm$ .02	1.73^j	32/44^c	K7-M0^c	Z	0^c	-3.0^d	SB2, triple
RX J0407.9+1750	II	0.985 $\pm$ .005		27/24^c	K4^c	Z	257^c	-0.2^d	SB1
RX J0408.2+1956	I, II, III	3.0109 $\pm$ .0002	3.02^j	-	K2^j	MS	<40^z	0.5^d	Eclipse
RX J0409.3+1716	II, III	0.60 $\pm$ .01		73^c	M1^c	w	299^c	-5.1^e	SB2^c
GSC2.2 N3022313162	II, III	0.59075 $\pm$ .00020		-	F2^y	MS	-	11.0^y	Eclipse
RX J0439.4+3332A	II	2.42 $\pm$ .02		24^c	K5^c	w	495^c	-0.7^e	SB1^c
RX J0447.9+2755	II, III	1.27 $\pm$ .02		36/27^c	K0^c	Z	203^c	-	SB2^c
IRAS 04451+2750	II	20.0 $\pm$ 2.0		-	-	?	-	-
RX J0452.8+1621	II, III	3.6 $\pm$ .1		41/26^c	K6^c	w	583^c	-0.5^e	SB2, triple
RX J0455.8+1742	II, III	8.1 $\pm$ 0.5		19/20^c	K3^c	Z	247^c	-	SB2^c
RX J0457.1+3142	I	$\gg$ 9	>37.6^j	25/27^c	K2^c	MS	138^c	0.9^d	SB1^c
Orion
RX J0530.7-0434	I	9.4 $\pm$ .9		10^h	K3^b	w	530^g	-0.04^g	SB2^h

^a Hearty et al. (2000b); ^b Magazzù et al. (1997); ^c Wichmann et al. (2000); ^d Martín & Magazzù (1999); ^e Wichmann et al. (1996); ^f Neuhäuser et al. (1997); ^g Alcalá et al. (1996); ^h Alcalá et al. (2000); ⁱ Mora et al. (2001); ^j Bouvier et al. (1997); ^k Torres et al. (2002); ^l Herbst et al. (2004), (?): tentative period only; ^y from low. res. CAFOS spectrum; no Li found; ^z personal communication by Eike Guenther.

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