Investigating the rotational evolution of very low-mass stars and brown dwarfs in young clusters using Monte Carlo simulations

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Table 2

Observational disk fraction for BDs and low-mass stars.

Region	Age (Myr)	BD (%)	VLM (%)	Total (%)	Disk criteria	References

NGC 1333^a	1–2				SED spectral slope	1
ONC	1–3	33/81 = 41			near-IR excess	2
ONC	1–3	–	62/125 = 50± 4.4	62/125 = 50± 4.4	Spitzer colour-mag diagrams	3
Taurus^b	1–2	27/63 = 43	44/86 = 51	71/149 = 48	IR colour-colour diagrams and SED spectral slope	4
Cha I^b	1–3				SED spectral slope	5, 6
IC 348^a	2–6				SED spectral slope	1
σ Ori^c	3–6				Spitzer colour-mag diagrams	7
25 Ori^d	6–8.5				SED spectral slope and Hα EW	8
TW Hya^e	7.5–10	2/3 = 67	5/13 = 38		SED excess emission	9
Upper Sco^f	5–11	45/152 = 28	97/364 = 27		IR colour-colour diagrams	10

Notes. All the uncertainties were calculated according to Burgasser et al. (2003).

^(a)

VLM stars with spectral types ≥M3.75 and ≤M5.75. BDs with spectral types ≥M6.

^(b)

VLM stars between M3.5 and earlier than M6. BD spectral types ≥M6.

^(c)

Calculated from the combination of disk fractions of VLM stars with M_J between 4–6 and 6–8 and of BDs with M_J between 8–10 and 10–12. See Luhman et al. (2008b) for more details.

^(d)

The VLM regime contains stars from M0.5 to M5.5 with four stars with spectral types earlier than M3 out of 77.

^(e)

BDs with spectral types ≥M6. VLM stars with spectral types between M3.5 and M5.

^(f)

The BD (≥M6) and VLM (M3.5–M6) disk fractions were calculated based on the authors’ disk classification from the paper’s Table 1 and encompass full, transitional, and evolved disks.

Reference. (1) Luhman et al. (2016); (2) Rodríguez-Ledesma et al. (2010); (3) Davies et al. (2014); (4) Luhman et al. (2010); (5) Luhman et al. (2008a); (6) Luhman & Muench (2008); (7) Luhman et al. (2008b); (8) Downes et al. (2015); (9) Kastner et al. (2016); (10) Luhman & Mamajek (2012).

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