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 3:

All photometric cluster member candidates of our survey. Table 3 is published in its entirety in the electronic edition of *Astronomy & Astrophysics*. A fraction is shown here for guidance regarding its form and content.
ID	$\alpha$	$\delta$	$I_{\rm c}^a$	J ^a	$K_{\rm s} ^a$	M^a	$T_{\rm eff}^a$	$J_{\rm model}^a$
	( $^{\rm h}$ $^{\rm m}$ $^{\rm s}$ )	( $^\circ$ ' '')	[mag]	[mag]	[mag]	[ $M_{\odot }$ ]	[K]	[mag]
001	08 40 53.61	+19 40 58.6	19.19	16.81	15.61	0.089	2665	17.00
002	08 41 08.8	+19 43 27.5	16.14	14.95	13.97	0.219	3321	14.86
003	08 41 01.6	+19 52 02.5	16.67	15.35	14.38	0.162	3189	15.48
004	08 41 12.17	+19 52 48.6	18.43	16.39	15.46	0.099	2805	16.72
005	08 41 08.5	+19 54 02.0	19.02	16.58	15.39	0.088	2636	17.06
006	08 40 10.74	+19 40 49.8	16.97	15.47	14.36	0.132	3061	15.95
007	08 39 39.56	+19 47 54.3	17.95	16.10	15.07	0.104	2860	16.58
008	08 39 43.38	+19 48 45.7	16.89	15.56	14.68	0.161	3186	15.50
009	08 39 55.84	+19 53 14.3	20.29	17.50	16.54	0.081	2520	17.32
010	08 39 06.9	+19 47 08.0	16.51	15.14	14.20	0.155	3166	15.57

^a The 1 $\sigma$ uncertainty in the determination of magnitude, effective temperature and mass are the following: $\Delta$ mag = 0.002 mag, $\Delta T_{\rm eff} = 140$ K and $\Delta M=0.1~M_\odot$ for stars ( $M > 0.2~M_\odot$ ), $\Delta$ mag = 0.01 mag, $\Delta T_{\rm eff} = 230$ K and $\Delta M = 0.05~M_\odot$ for very low-mass stars (0.072 $M_\odot< M < 0.2~M_\odot$ ), $\Delta$ mag = 0.04 mag, $\Delta$ $T_{\rm eff} = 420$ K and $\Delta M = 0.02~M_\odot$ for BDs ( $M<~0.072~M_\odot$ ). The magnitude $J_{\rm model}$ is the predicted magnitude based on photometric determination of $T_{\rm eff}$ and mass.

Source LaTeX | All tables | In the text

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