The Gaia-ESO Survey: Structural and dynamical properties of the young cluster Chamaeleon I

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Volume 601 (May 2017)

A&A, 601 (2017) A97

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Table 1

Members of the cluster observed by the Gaia-ESO Survey.

n	Cname	RA	Dec	RV^a	T_eff	γ ^b	EW(Li)	Hα10%^c	Inst.^d	Known
		(J2000)	(J2000)	(km s^-1)	(K)		(mÅ)	(km s^-1)		members

1	10550964-7730540	163.79017	–77.51500	16.83 ± 0.90	–	–	725	128	G	Y
2	10555973-7724399	163.99887	–77.41108	–	3640	–	120	441	U	Y
3	10561638-7630530	164.06825	–76.51472	12.56 ± 2.01	–	–	–	215	G	Y
4	10563044-7711393	164.12683	–77.19425	15.69 ± 0.27	4351	0.97	300	390	G	Y
5	10563146-7618334	164.13108	–76.30928	15.41 ± 0.54	3319	–	597	142	G	N
6	10574219-7659356	164.42579	–76.99322	16.14 ± 0.26	3452	0.89	571	272	G	Y
7	10575376-7724495	164.47400	–77.41375	15.71 ± 0.32	3426	0.86	632	138	G	N
8	10590108-7722407	164.75450	–77.37797	15.64 ± 0.40	4135	–	375	375	U	Y
9	10590699-7701404	164.77912	–77.02789	17.93 ± 0.26	4981	–	390	440	G	Y
10	11004022-7619280	165.16758	–76.32444	15.73 ± 0.42	–	–	584	230	G	Y

Notes. A full version of the table is available at the CDS.

^(a)

For spectra with a signal-to-noise ratio lower than 3 we did not report any velocity.

^(b)

Empirical gravity indicator defined by Damiani et al. (2014).

^(c)

Width at 10% of the peak of the Hα line.

^(d)

The letters “G” and “U” indicate GIRAFFE and UVES, respectively.

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