Table 1:

Classical T Tauri stars that belong to NGC 2264 and were observed by CoRoT.

RA	Dec	V	CoRoT ID	H EW	UV1	UV2	H10%	SpT	LC group	Period
(deg)	(deg)	(mag)		(Å)	(mag)	(mag)				(days)
99.89338	9.91424	16.64	223957455	22.1	...	...	x	...	NP	...	...
99.92281	9.77214	14.64	223959618	28.4	...	...	x	...	PII	3.87	...
99.99684	9.45681	16.34	223964667	42.2	...	...	x	...	PII	6.45	-1.87
100.04666	9.63501	16.67	223968039	52.9	-1.15	...	x	K6	NP	...	-1.35
100.05673	9.41375	13.02	223968688	0.60	...	...	x	K0	PI	1.11	-2.81
100.05710	9.94183	17.02	400007614	130.2	...	...	x	M2	NP	...	0.0149
100.09620	9.46176	16.04	223971231	49.5	-1.62	...	x	K5	NP	...	-1.73
100.09889	9.92330	17.55	223971383	80.6	...	...	x	...	PI	4.66	-1.22
100.12006	9.51718	15.20	223972652	39.1	-0.89	...	...	K4	NP	...	-0.56
100.12186	9.73542	17.69	400007809	31.3	-1.36	...	x	M2	NP	...	...
100.12859	9.57794	16.03	223973200	22.2	...	...	x	K1	NP	...	-1.29
100.13013	9.51864	15.43	223973292	1.7	-0.91	...	...	K6	PI	1.96	...
100.15217	9.84601	16.67	400007538	21.1	-2.11	-1.687	...	M2	NP	...	-1.29
100.15262	9.80638	15.62	500007298	4.9	-1.43	-0.606	...	K5	PI	15.70	-4.19
100.15781	9.58167	16.64	400007528	23.4	...	...	x	M3	NP	...	-1.87
100.16297	9.84961	15.43	500007252	46.5	-1.89	...	x	K4	PII	7.06	-1.55
100.16840	9.84735	15.50	500007272	58.3	...	...	...	K7	PI	3.76	-2.42
100.17086	9.46509	16.53	500007505	13.2	...	...	...	...	NP	...	-1.97
100.17095	9.79936	16.01	500007379	7.5	-1.22	-0.984	...	K7	PI	14.15	-1.97
100.17216	9.85066	15.70	500007315	24.5	-2.13	...	...	K7	PII	7.80	-1.19
100.17233	9.90385	13.57	223975844	12.2	0.02	...	x	G3	PI	3.31	...
100.17435	9.86237	15.49	500007269	23.4	...	...	...	K5	PI	3.75	-1.53
100.17576	9.56040	12.09	223976028	7.3	...	...	x	G0	NP	...	-1.12
100.18006	9.78535	16.33	500007460	27.1	...	...	x	K6	NP	...	...
100.18580	9.54061	18.13	500007930	60.0	...	...	...	M3	NP	...	-2.61
100.18819	9.47901	14.55	223976747	7.2	-0.16	...	x	K2	PII	3.16	...
100.19793	9.82471	14.14	500007120	12.8	...	-0.806	x	K1	PII	4.23	-1.41
100.19968	9.55087	18.24	500007963	...	...	-0.917	...	...	PI	2.56	...
100.20505	9.96077	17.46	500007730	50.8	...	...	...	M1	PI	11.85	-2.67
100.20789	9.61375	15.37	223977953	66.3	-1.79	-1.906	...	K4	PII	4.96	-1.43
100.21081	9.91593	15.13	500007209	11.2	...	...	x	K2	PII	2.51	-2.14
100.21326	9.74615	12.05	223978308	3.5	...	...	x	G0	PII	5.40	-1.69
100.22346	9.55686	14.70	223978921	18.2	...	-0.643	x	K1	NP	...	-2.29
100.22607	9.82232	16.39	500007473	161.1	-2.11	...	x	M0	NP	...	-0.38
100.22990	9.84718	15.89	500007354	2.8	-0.64	-0.774	...	K5.5	PI	1.17	-9.15
100.23215	9.85385	15.54	500007283	8.00	...	...	...	K5.5	PI	3.23	-0.29
100.23663	9.63029	15.09	223979728	113.2	...	-1.353	x	M1	NP	...	-1.17
100.24208	9.61483	18.05	223980048	34.0	...	...	...	...	PII	4.06	-1.41
100.24447	9.60368	17.40	223980233	22.2	...	...	...	M4	NP	...	...
100.24510	9.65522	17.02	223980258	27.9	...	...	x	M0	PI	7.05	-1.39
100.24516	9.51592	14.04	223980264	14.3	...	...	x	K2.5	PII	3.46	-1.51
100.24770	9.99596	15.34	223980412	7.41	-0.53	...	...	K5	PI	3.23	...
100.24792	9.49770	17.00	500007610	26.2	...	...	...	M3	PII	4.66	-1.16
100.24811	9.58636	15.58	223980447	6.4	-1.01	-0.427	x	K6	PI	1.67	-1.14
100.25209	9.75088	15.39	223980688	15.0	-0.59	-0.723	x	K3	PII	4.16	-2.10
100.25214	9.48776	14.56	223980693	16.6	...	...	x	K4	PII	5.35	-1.72
100.25323	9.85620	14.63	500007157	1.6	...	-0.658	...	K1	PI	4.36	...
100.25408	9.54568	13.51	223980807	6.4	...	...	x	K1	NP	...	-1.56
100.25767	9.64475	14.70	223981023	1.5	...	...	x	K4	PII	7.05	-2.41
100.26266	9.62660	19.17	500008211	34.1	...	...	...	M1	NP	...	-1.22
100.26503	9.50806	17.67	400007803	20.4	...	...	...	...	PII	9.75	-1.12
100.26789	9.41449	15.79	500007335	101.8	-2.34	...	x	M0	PII	7.36	-0.97
100.26905	9.64190	17.88	500007857	108.	...	...	...	M3	NP	...	-0.78
100.27071	9.84613	14.36	223981811	36.5	-0.29	-0.816	x	K1	PII	3.73	-1.91
100.27124	9.86239	15.39	500007248	1.7	-0.75	-0.570	...	K5	PI	1.88	-3.06
100.27583	9.60638	13.52	223982136	10.0	...	...	x	G3	PI	3.01	-2.03
100.27595	9.41769	18.01	500007896	34.7	...	...	...	M5	PI	9.30	-1.58
100.27679	9.47745	17.30	400007686	56.1	...	...	x	M1.5	NP	...	-1.57
100.27808	9.57943	15.97	500007369	49.4	...	...	x	G6	NP	...	...
100.28734	9.56278	17.53	500007752	51.0	...	...	x	M3	PI	4.01	-0.88
100.29582	9.59881	17.44	500007727	61.5	...	-2.037	x	K7	NP	...	-0.93
100.30241	9.87533	14.07	500007115	35.3	...	...	x	G	PII	2.01	-1.72
100.30362	9.43746	13.76	500007089	85.6	...	...	x	K4	NP	...	-1.33
100.31035	9.62065	17.23	500007667	4.1	...	-0.697	...	...	PI	5.41	-2.96
100.32188	9.90899	15.64	223985009	58.3	-2.40	...	...	K7	NP	...	...
100.32467	9.48364	18.55	500008049	231.4	...	...	...	M2.5	NP	...	-0.68
100.32534	9.64038	18.58	500008061	32.5	...	...	...	M3	PI	0.98	-2.89
100.32613	9.56488	15.02	223985261	28.9	-0.97	...	x	K4	NP	...	-2.39
100.33752	9.56005	15.20	223985987	10.6	...	...	x	K6	PII	3.31	-1.44
100.34851	9.78788	17.93	500007872	5.2	...	-0.767	...	...	PI	8.20	-2.01
100.35227	9.62653	17.38	400007709	8.9	-0.99	...	...	M3	PI	0.76	...
100.35677	9.57861	16.15	223987178	15.9	-0.61	-1.233	...	M0	PII	4.96	-1.11
100.36250	9.50365	17.47	400007734	25.8	...	...	...	M1	NP	...	-1.88
100.37968	9.44951	14.19	500007122	25.9	...	...	x	...	PII	12.53	-1.44
100.38169	9.80912	14.63	223988742	5.16	-0.08	-0.409	...	K2	PI	5.03	-2.84
100.38331	10.0068	15.59	223988827	13.1	...	...	...	K5	PI	4.78	-2.69
100.38543	9.63540	14.66	223988965	1.3	-0.67	...	...	K6	PI	3.23	-2.83
100.39397	9.60904	17.16	223989567	4.5	-0.83	...	x	M1	NP	...	...
100.40536	9.75186	15.44	223990299	35.0	...	-0.826	x	K4	PI	4.51	-0.93
100.41155	9.53661	15.40	500007249	58.6	...	...	x	K4	NP	...	-1.55
100.41564	9.67443	13.86	223990964	52.5	...	-1.061	...	K4	NP	...	-1.46
100.42867	9.41900	16.65	223991832	75.8	...	...	x	...	PII	8.40	-1.38
100.47104	9.96747	14.99	223994721	9.5	...	...	x	K7	NP	...	-1.47

Notes. The H equivalent widths come from Rebull et al. (2002) and Dahm & Simon (2005), except for six stars (CID 223957455, 223959618, 223964667, 223968688, 223991832, 223994721) for which we measured the H equivalent width ourselves, using the high resolution hectoechelle spectra kindly provided by Gabor Furész. The U-V excesses were taken from Rebull et al. (2002) (UV1) and Fallscheer & Herbst (2006) (UV2, the U-V excess data table was provided by Cassandra Fallscheer). Stars that have an H width at 10% intensity larger than 270  km s^-1 are identified by a x sign in column eight, following the classification of Furész et al. (2006). The LC group and period values were determined in the present work. The index is described in Sect. 3.3 and comes from Teixeira (2008).