Tracing the W3/W4/W5 and Perseus complex dynamical evolution with star clusters

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Table 1

Mean properties of clusters in the W345 complex.

Cluster	(α, δ) (degree)	〈μ_α〉 σ_μα (mas yr⁻¹)		〈μ_δ〉 σ_μδ (mas yr⁻¹)		〈ω〉 σ_ω (mas)		ρ_μαμ_δ*	ρ_μαω*	ρμ_δω
IC 1848	(42.851, 60.438)	−0.40	0.12	−0.43	0.09	0.456	0.007	0.19	0.43	0.12
IC 1805	(38.198, 61.510)	−0.75	0.11	−0.74	0.11	0.464	0.010	−0.13	−0.32	−0.09
Berkeley 65	(39.766, 60.408)	−0.69	0.10	−0.42	0.09	0.448	0.014	−0.03	−0.60	−0.19
UBC 420	(40.174, 60.864)	−0.60	0.25	−0.30	0.12	0.428	0.029	−0.39	−0.16	0.09
SAI 24	(44.732, 60.578)	−0.26	0.14	0.07	0.10	0.460	0.010	0.02	0.42	0.30

Notes. Cluster name, center celestial coordinates, mean PM along the right ascension and declination coordinates, mean parallax, along with the corresponding intrinsic distribution widths. The last three columns list the correlation coefficients.

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