Hubble Space Telescope proper motions of Large Magellanic Cloud star clusters - II. Kinematic structure of young and intermediate-age clusters

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Volume 705 (January 2026)

A&A, 705 (2026) A94

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Table B.2

Positions and velocities of the young and intermediate-age star clusters projected onto the reference frame of the LMC.

Cluster ID	R [kpc]	ϕ [deg]	Z [kpc]	V_ϕ [kms⁻¹]	V_R [km s⁻¹]	V_Z [km s⁻¹]
NGC 1651	2.55 ± 0.11	124.00	2.15 ± 0.18	64.2 ± 8.1	3.7 ± 7.5	33.3 ± 5.4
NGC 1718	2.94 ± 0.03	178.00	−0.02 ± 0.38	106.0 ± 7.8	−70.1 ± 9.6	22.2 ± 5.5
NGC 1751	1.61 ± 0.09	133.69	1.17 ± 0.18	53.9 ± 7.5	−5.9 ± 7.4	26.0 ± 4.7
NGC 1783	3.35 ± 0.04	200.24	−0.01 ± 0.19	78.3 ± 6.8	4.2 ± 7.8	12.5 ± 4.3
NGC 1805	3.53 ± 0.15	218.39	1.41 ± 0.37	105.1 ± 7.0	0.4 ± 7.2	−2.3 ± 5.2
NGC 1806	1.79 ± 0.02	179.80	0.13 ± 0.38	28.6 ± 7.1	−16.3 ± 8.6	43.9 ± 4.8
NGC 1818	2.90 ± 0.12	208.95	0.33 ± 0.38	112.8 ± 9.0	1.9 ± 9.8	−2.9 ± 6.4
NGC 1831	4.14 ± 0.71	218.15	0.19 ± 1.89	62.3 ± 13.3	−23.4 ± 14.1	15.5 ± 8.1
NGC 1846	1.83 ± 0.06	192.53	−0.41 ± 0.38	17.0 ± 10.8	20.8 ± 12.5	28.1 ± 6.9
NGC 1850	1.18 ± 0.08	218.89	1.48 ± 0.18	−11.1 ± 6.1	−22.7 ± 6.3	10.8 ± 3.8
NGC 1856	0.69 ± 0.10	187.14	0.85 ± 1.12	40.0 ± 9.7	2.2 ± 11.3	8.0 ± 6.7
NGC 1866	4.07 ± 0.45	233.84	1.22 ± 0.92	101.7 ± 9.0	−19.4 ± 8.7	6.6 ± 5.2
NGC 1868	5.07 ± 0.42	231.16	0.39 ± 0.94	56.1 ± 12.2	−50.8 ± 11.7	16.5 ± 6.4
NGC 1978	2.75 ± 0.74	247.00	−0.69 ± 1.35	24.4 ± 12.0	13.3 ± 12.0	−24.7 ± 7.2
NGC 2108	1.99 ± 0.85	314.47	0.00 ± 1.90	70.3 ± 14.0	−27.0 ± 14.0	14.8 ± 9.7
NGC 2173	3.88 ± 0.04	359.53	1.88 ± 0.36	68.4 ± 7.7	17.9 ± 8.9	3.3 ± 5.3
NGC 2203	5.27 ± 0.03	10.17	3.27 ± 0.18	42.5 ± 6.8	23.9 ± 7.8	2.2 ± 5.2
NGC 2209	4.73 ± 0.22	357.60	2.66 ± 1.78	47.7 ± 18.0	4.2 ± 17.2	2.5 ± 11.4
NGC 2213	4.15 ± 0.03	347.66	0.51 ± 0.19	77.9 ± 8.6	14.0 ± 10.4	3.2 ± 5.6

Notes. Here, ϕ denotes the position angle within the LMC disc, measured anti-clockwise from the positive X-axis. A positive tangential velocity, V_ϕ, follows the clockwise rotation pattern of the LMC. The cluster NGC 1850 is the only cluster with a retrograde orbit (negative V_ϕ) in our sample.

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