**Table A.4:** Stellar parameters relevant for the Hertzsprung-Russell Diagram of all objects. The objects are grouped by type and sorted by right ascension. For the objects in Taurus, a distance of $140~{\rm pc}$ is assumed, for MBM12 $90~{\rm pc}$ . The color excess that was used to calculate the extinction A_V is given in the neighboring column. To get the real colors of the objects we used the spectral type - color conversion from Kenyon & Hartmann (1995) for early spectral types and Leggett (1992) for type M0 and later. The masses and ages are interpolated from pre main sequence models by D'Antona & Mazzitelli (1994). The apparent magnitudes in V for objects observed in Run I was determined by absolute photometry ourselves. For Run II objects we had to rely on VizieR (Ochsenbein et al. 2000) values - we averaged all available values. For more details see text.
Object name	$\log L_{{\rm bol}}$	$\log T_{{\rm eff}}$	$T_{{\rm eff}}$	$M_{{\rm bol}}$	V	A_V	Determination A_V	$M/M_{\odot}$	$\log {\rm Age}$
Classical TTS:
Lk ${\rm H}\alpha$ 263	-0.870	3.519	3300	6.91	14.90	0.62	E(V-R,I,J;R-I)	0.20	6.35
Lk ${\rm H}\alpha$ 262	-1.162	3.585	3850	7.65	14.83	1.16	E(V-R,I,J;R-I)	0.60	7.25
Lk ${\rm H}\alpha$ 264	-0.570	3.638	4350	6.17	13.74	2.08	E(V-I,J;R-I)	0.90	7.20
Weak-line TTS:
RX J0255.4+2005	-0.656	3.624	4205	6.38	12.23	0.26	E(V-I,J,H,K;R-I)	0.82	7.30
E0255.3+2018	-0.195	3.662	4590	5.23	11.84	1.29	E(V-J,H,K;R-I)	1.10	6.94
RX J0312.8-0414NW	0.054	3.780	6030	4.61	10.86	0.35	E(R-I)	1.12	7.60
RX J0312.8-0414SE	-0.176	3.742	5520	5.18	11.62	0.46	E(R-I)	0.95	7.60
RX J0324.4+0231	-0.788	3.638	4350	6.71	12.69	0.0	E(R-I)	0.71	7.65
RX J0333.1+1036	-0.410	3.675	4730	5.77	12.15	0.15	E(R-I)	0.90	7.40
RX J0344.8+0359	-0.539	3.675	4730	6.09	12.74	0.42	E(R-I)	0.80	7.60
RX J0351.4+0953W	-0.600	3.699	5000	6.24	12.64	0.30	E(R-I)	0.79	7.88
RX J0403.4+1725	0.000	3.675	4730	4.74	11.69	0.72	(Chavarría-K et al. 2000)	1.33	6.80
RX J0406.8+2541	0.518	3.597	3955	3.45	11.72	1.46	(Chavarría-K et al. 2000)	0.55	5.00⁹
RX J0407.3+0113S	-0.506	3.675	4730	5.97	13.85	1.73	E(R-I)	0.83	7.55
RX J0407.3+0113N	-0.157	3.763	5800	5.13	12.80	1.73	E(R-I)	1.00	7.70
RX J0409.3+1716	-0.336	3.571	3720	5.58	13.30	0.56	(Chavarría-K et al. 2000)	0.50	6.16
RX J0434.3+0226	-0.362	3.662	4590¹	5.64	12.46	0.54	E(R-I)	0.76	7.20
RX J0439.4+3332A	0.158	3.638	4350	4.34	11.31	0.52	E(V-I)	0.90	6.07
RX J0445.5+1207	-0.399	3.609	4060	5.74	13.03	0.64	E(R-I)	0.80	6.70
RX J0450.0+0151	-0.218	3.675	4730	5.28	11.96	0.02	E(R-I)	1.02	7.20
RX J0452.8+1621	-0.158	3.662	4590	5.14	11.57	0.16	E(B-V)	1.13	6.88
RX J0528.9+1046	-0.658	3.675	4730²	6.38	13.22	0.61	E(R-I)	0.74	7.80
RX J0529.3+1210	-0.602	3.597	3955³	6.25	13.26	0.20	E(J-K),E(V-I)	0.54	6.90
RX J0530.7-0434	-0.015	3.675	4730	4.78	11.62	0.60	E(V-J,R-I)	1.32	6.80
Ke stars:
RX J0408.2+1956	-0.307	3.690	4900	5.51	13.04	1.38	E(R-I)	0.93	7.38
RX J0457.1+3142	-0.066	3.690	4900	4.91	11.80	0.74	$\varnothing$ Tau-Aur (Chavarría-K et al. 2000)	1.18	7.02
Zero Age Main Sequence:
RX J0407.9+1750	-0.060	3.662	4590	4.89	11.27	0.1	(Chavarría-K et al. 2000)	1.19	6.75
RX J0422.9+0141	0.107	3.792	6200⁴	4.47	11.79	1.43	E(B-V)	1.11	7.60
RX J0444.7+0813	-0.318	3.675	4730	5.54	13.23	0.38	E(R-I)	0.96	7.25
RX J0447.9+2755	-0.445	3.720	5250	5.85	12.34	0.45	E(J-K)	0.85	7.80
RX J0455.8+1742	0.012	3.675	4730	4.71	11.29	0.35	E(V-J,V-H,V-K,V-R)	1.27	6.75
Unknown type:
GSC2.2 N3022313162	-0.848	3.829	6740	6.86	13.27	0.56	same as neighbor	-	-
1RXS J044534.0+120917	-0.763	3.720	5250	6.65	13.23	0.54	E(R-I), SpTy(K0) from V-K	-	-
IRAS 04451+2750	0.294	3.690	4900	4.00	11.70	1.55	E( all filters), SpTy(K2) by adjustment	1.53	6.50

¹ Torres et al. (2002): $T_{\rm eff}^{\rm A}=$ 5050; ² Torres et al. (2002) $T_{\rm eff}^{\rm A,B}=$ 4800, 4550; ³ Torres et al. (2002) $T_{\rm eff}^{\rm A}=$ 4350; ⁴ Torres et al. (2002) $T_{\rm eff}^{\rm A,B}=$ 4550, 6300.
⁹ Note that this age is not consistent with the Lithium-Test (classified as ZAMS). However, in lower resolution spectra by Martín & Magazzù (1999) the $W_{\lambda }({\rm Li})$ was given as 590 mÅ.

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