Rotation-disk connection for very low mass and substellar objects in the Orion Nebula Cluster

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Table 3:

Median values of rotational period for objects with ( $\Delta(I-K)~+)$ and without ( $\Delta(I-K)~-)$ IR excess.
	$R<R_{\rm cluster}$						$R>R_{\rm cluster}$						Whole WFI field
	$\Delta(I-K)+$			$\Delta(I-K)-$			$\Delta(I-K)+$			$\Delta(I-K)-$			$\Delta(I-K)+$			$\Delta(I-K)-$
Mass bins^a	A	B	C	A	B	C	A	B	C	A	B	C	A	B	C	A	B	C
N	13	56	8	49	120	8	14	65	25	36	204	40	27	121	33	85	324	48
$\langle P \rangle$ [days]	6.3	4.7	1.5	4.4	2.9	1.7	6.4	3.8	1.7	3.8	2.0	1.6	5.8	4.5	1.7	4.2	2.5	1.7

Notes. ^(a) Mass bins as defined in Sect. 3: A corresponds to the bright bin containing stars with $M\geq 0.4~M_\odot$ , B to the intermediate bin with $0.4<M <0.075~M_\odot$ , and C to the faint bin in which all objects have $\textit{M}<0.075~M_\odot$ .

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