Deep XMM-Newton observation of the η Chamaleontis cluster

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Table 1

Spectral type, binarity, and disk properties of η Chamaleontis members in the XMM-Newton field of view.

Source	RECX	Sp.T.^*	Binarity^**	Disk type^†	log L_bol^‡
					(erg s^-1)

η Cha	2	B8	?	debris	35.5
EH Cha	3	M3		TO	32.7
EI Cha	4	M1		TO	32.9
EK Cha	5	M4		TO	32.6
EL Cha	6	M3			32.7
EM Cha	7	K6	K6.9+M1.0		33.4
RS Cha	8	A7 + A8	eclipsing		34.9
EN Cha	9	M4	M4.4 + M4.7	TO	32.6
EO Cha	10	M0			33.2
EP Cha	11	K6		class II	33.4
EQ Cha	12	M3	M3.2+M3.2:		32.7
HD 75505	13	A1			35.1
ES Cha	14	M5		TO	32.1
ET Cha	15	M3		class II	32.7

Notes.

^(*)

Torres et al. (2008).

^(**)

Sicilia-Aguilar et al. (2009), determined from Lyo et al. (2004).

^(†)

Sicilia-Aguilar et al. (2009). TO are transitional disk objects.

^(‡)

Luminosities determined from the spectral type, assuming an age of 6 Myr and the Siess et al. (2000)’s pre-main-sequence model.

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