Rotation period distribution of CoRoT and Kepler Sun-like stars

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Volume 582 (October 2015)

A&A, 582 (2015) A85

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Table 1

Best-fit solutions.

	Sample name
Parameter^a	DMS_⊙	MH_⊙^b	RH_⊙

P_I (d)	5.5 ± 0.6	12.3 ± 2.0	11.3 ± 0.8
σ_I (d)	2.7 ± 1.4	6.4 ± 2.3	5.4 ± 1.3
ρ_I (%)	84 ± 12	64 ± 12	72 ± 14
ρ_II (%)	16 ± 12	36 ± 12	28 ± 14
Det. par.	S/N	w	A (mmag)
thres	1.00 ± 0.65	0.25 ± 0.08	1.78 ± 0.61
D _KS	0.058	0.034	0.025
P_KS (%)	51^c	0.65	20

Notes.

^(a)

P_I and σ_I refer to the normal distribution peak and standard deviation for group I, ρ_I and ρ_II depict the proportion of stars in groups I and II with respect to the entire Sun-like sample, Det. par. and thres give the detectability parameter considered in the simulation and the corresponding threshold value obtained in the fit, and D_KS and P_KS are the resulting K-S distance and K-S probability.

^(b)

For the MH_⊙ sample, the detectability parameter w was simulated from a calibration with the amplitude A for an approximate solution.

^(c)

P_KS increases with decreasing D_KS and decreases with increasing the sample sizes. Hence, the relatively low number of DMS_⊙-sample targets produces a high probability even though the MH_⊙ and RH_⊙ samples have lower D_KS values.

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