Spectroscopy of very low-mass stars and brown dwarfs in the Lambda Orionis star-forming region - II. Rotation, activity and other properties of spectroscopically confirmed members of Collinder 69

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Volume 547 (November 2012)

A&A, 547 (2012) A80

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Table 4

Parameters measured and calculated for those sources showing variations in Hα and no significant variability in alkali lines; or variations in Hα that causes them to oscillate between accreting and non-accreting (see text for details).

Name	EW(Hα)	EW(Hα) S08	Ins. Res	Mass(M_⊙)	Class	Disk	Li I	Li I S08	KI	NaI

LOri073	–10.91 ± 1.04		MIKE R ~ 11 250	0.34	III	Diskless	0.62 ± 0.03			2.5 ± 0.02^∗∗
LOri073	–4.54 ± 0.19		FLAMES R ~ 8600	0.34	III	Diskless	0.66 ± 0.05			2.5 ± 0.02^∗∗


DM048	–3.36 ± 0.11		CAFOS R ~ 600	0.25	II	Thick			0.29 ± 0.07	2.57 ± 0.43
DM048	–7.72 ± 0.19		TWIN R ~ 1100	0.25	II	Thick			0.49 ± 0.21	2.36 ± 0.18


LOri068	–6.82 ± 0.52	–7.9 ± 1.26	MIKE R ~ 11 250	0.35	III	Diskless	0.69 ± 0.09	0.698 ± 0.025
LOri068	–14.39 ± 0.74	–7.9 ± 1.26	LRIS R ~ 2650	0.35	III	Diskless	0.53 ± 0.05	0.698 ± 0.025


LOri075	–12.81 ± 0.86	–10.71 ± 0.98	MIKE R ~ 11 250	0.25	III	Diskless	0.94 ± 0.05	0.455 ± 0.044
LOri075	–10.20 ± 0.89	–10.71 ± 0.98	LRIS R ~ 950	0.25	III	Diskless		0.455 ± 0.044		2.82 ± 0.38


LOri080	–21.3 ± 1.00	–14.47 ± 1.25	BC R ~ 2600	0.15	III	Diskless		0.523 ± 0.020	1.66 ± 0.89
LOri080	–22.82 ± 0.62	–14.47 ± 1.25	TWIN R ~ 1100	0.15	III	Diskless		0.523 ± 0.020	1.77 ± 0.33	2.34 ± 0.46


LOri091^∗	–11.93 ± 1.12		LRIS R ~ 2650	0.13	III	Diskless	0.23 ± 0.07		2.17 ± 0.46
	–23.2 ± 12.3		TWIN R ~ 1100							2.05 ± 0.70
	–13.47 ± 1.11		FLAMES R ~ 8600				0.76 ± 0.06


LOri109	–19.62 ± 0.52		FLAMES R ~ 8600	0.16	III	Diskless	0.57 ± 0.11
LOri109	–8.70 ± 0.45		LRIS R ~ 2650	0.16	III	Diskless	0.50 ± 0.15		2.62 ± 0.57

Notes. Positive equivalent widths for Hα denote emission while for the alkali lines it means absorption. We also compile the values from Sacco et al. (2008) for Hα and Li I.

^(*)

The S/N of the TWIN spectrum of LOri091 is very low. This is clear in the very large error on the determination of the EW. Therefore this object is not considered variable.

^(**)

Value from Maxted et al. (2008).

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