Brown dwarfs and very low mass stars in the Praesepe open cluster: a dynamically unevolved mass function?

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Volume 510 (February 2010)

A&A, 510 (2010) A27

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Table 5:

Same as Table 3, but only the BD candidates are given and we include the spectral type expected.
ID	$\alpha$	$\delta$	$I_{\rm c}$	J	$K_{\rm s}$	M	$T_{\rm eff}$	$J_{\rm model}$	SpT^a
	( $^{\rm h}$ $^{\rm m}$ $^{\rm s}$ )	( $^\circ$ ' '')	[mag]	[mag]	[mag]	[ $M_{\odot }$ ]	[K]	[mag]
055	08 41 04.5	+20 14 58.0	21.61	18.29	17.12	0.068	2250	17.97	L0
096	08 41 13.48	+18 59 05.1	21.06	17.85	16.82	0.072	2335	17.75	M9
099	08 41 45.16	+19 18 07.7	21.30	17.98	17.01	0.068	2249	17.98	L0
909	08 39 29.94	+20 11 40.3	20.11	17.63	16.67	0.069	2259	17.95	L0
910	08 40 34.00	+20 14 56.2	20.08	17.60	16.65	0.069	2261	17.94	L0
915	08 38 51.77	+19 00 21.6	20.28	17.67	16.68	0.068	2238	18.01	L0

^a Spectral type expected based on $T_{\rm eff}$ and the temperature scale of Kraus & Hillenbrand (2007), with L1 set to 2100 K. The error on this estimation is one subclass.

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