The substellar population in Corona Australis | Astronomy & Astrophysics (A&A)

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Table 3

Slope α of the power laws fitted to the IMF (Fig. 7) and star-to-BD number ratio for different regions.

	Slope of the IMF (α)		Star-to-BD ratio		Reference	Surface density^d	F_FUV,median

	<1 M_⊙	<0.2 M_⊙	0.03–1 M_⊙	0.02–1 M_⊙		(pc⁻²)	(G₀)
CrA	0.95 ± 0.06	0.63 ± 0.14	${2.0}_{- 1.0}^{+ 2.7}$ $2.0^{+2.7}_{-1.0}$	${1.4}_{- 0.7}^{+ 1.4}$ $1.4^{+1.4}_{-0.7}$	This work^a	120	13.0
Cha I	0.62 ± 0.13	0.67 ± 0.23	3.2–4.8	2.6–3.7	Mužic´ et al. (2015)^b	29	1.2
Lupus 3	0.98 ± 0.38	0.29 ± 0.22	2.1–4.5	2.0–4.0	Mužic´ et al. (2015)^b	24	0.6
NGC 1333	0.61 ± 0.08	0.48 ± 0.15	1.8–2.8	1.8–2.7	Scholz et al. (2012b)	200	27.1
NGC 2244	0.98 ± 0.04	1.09 ± 0.14	2.34 ± 0.25	1.74 ± 0.28	Mužic´ et al. (2019)^c	33	11569.8
RCW 38	0.91 ± 0.11	0.51 ± 0.15	2.0 ± 0.6		Mužic´ et al. (2017)	3620	266124.6

Notes. (a) the mean of the results from the three isochrones; (b) updated as described in Appendix C; (c) values for isochrone 1 and distance of 1400 pc; (d) values from Mužic´ et al. (2019) and Appendix D.

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