A census of very-low-mass stars and brown dwarfs in the σ Orionis cluster

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Volume 505 / No 3 (October III 2009)

A&A, 505 3 (2009) 1115-1127

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Table 4:

Numbers for the luminosity and mass functions.
Jmag range	Mass range^a	dM^b	dN^c	d $N_{\rm CF}^{d}$	d $N_{\rm NW}^{e}$	d $N_{\rm corr}^{f}$	d $N^{g}_{\rm bol_{\rm corr}}$	d $N/{\rm d}M$
12.00-12.50	0.4910-0.3440	0.1470	44.0	1.0	3.0	43.0	36	292.52
12.50-13.00	0.3440-0.2460	0.0980	55.0	11.0	5.0	44.0	35	448.98
13.00-13.50	0.2460-0.1690	0.0770	47.0	8.0	3.0	39.0	50	506.49
13.50-14.00	0.1690-0.1100	0.0590	37.0	5.0	3.0	32.0	38	542.37
14.00-14.50	0.1100-0.0670	0.0430	20.0	5.0	1.0	15.0	16	348.84
14.50-15.00	0.0670-0.0470	0.0200	23.0	1.0	2.0	22.0	23	1100.00
15.00-15.50	0.0470-0.0360	0.0110	27.0	3.0	6.0	24.0	28	2181.82
15.50-16.00	0.0360-0.0285	0.0075	8.0	2.0	1.0	6.0	1	800.00
16.00-16.50	0.0285-0.0233	0.0052	5.0	2.0	0.0	3.0	5	576.92
16.50-17.00	0.0233-0.0182	0.0051	6.0	0.0	0.0	6.0	8	1176.47
17.00-17.50	0.0182-0.0141	0.0041	8.0	2.0	0.0	6.0	3	1463.41
17.50-18.00	0.0141-0.0114	0.0027	2.0	1.0	0.0	1.0	1	370.37
18.00-18.50	0.0114-0.0092	0.0022	3.0	2.0	0.0	1.0	2	454.55
18.50-19.00	0.0092-0.0075	0.0017	7.0	4.0	0.0	3.0	3	588.24

^a Mass range associated to the magnitude range given in the first column: we assumed an age of 3 Myr and a distance of 352 pc; ^b Difference between the masses, dM; ^c Numbers of candidate members identified in $\sigma$ Orionis; ^d Numbers of contaminants identified in the control field (CF) ^e Numbers of objects located beyond 10 arcmin towards the North-West of the cluster center, where the contamination by the old population is the highest; ^f Numbers of candidate members in $\sigma$ Orionis using method #1 and corrected for contamination; ^g Numbers of candidate members in $\sigma$ Orionis using method #2 after correction for contamination estimated from the control field; ^h Values for the mass function in linear scale (d $N/{\rm d}M$ ) using method #1.

Source LaTeX | All tables | In the text

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