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Table 1

Mean astrometry of the LMC and SMC clean (after spatial and proper motion selection) samples and the evolutionary phase subsamples extracted from them.

σϖ
LMC –0.0040 0.3346 1.7608 0.4472 0.3038 0.6375
Young 1 −0.0049 0.0729 1.7005 0.2700 0.2073 0.4733
Young 2 0.0058 0.1154 1.7376 0.3260 0.2083 0.5067
Young 3 −0.0095 0.4245 1.7491 0.4814 0.2859 0.6586
RGB −0.0010 0.3239 1.7690 0.4372 0.3255 0.6344
AGB −0.0164 0.0414 1.8387 0.2686 0.3217 0.4486
RRL −0.0046 0.3201 1.7698 0.4818 0.2947 0.6742
BL 0.0047 0.1341 1.7103 0.3996 0.2852 0.6260
RC −0.0050 0.2314 1.7719 0.4167 0.3093 0.6113
SMC –0.0026 0.3273 0.7321 0.3728 –1.2256 0.2992
Young 1 −0.0099 0.0995 0.7754 0.2495 −1.2560 0.1195
Young 2 0.0036 0.1585 0.7708 0.2981 −1.2555 0.1951
Young 3 −0.0012 0.4382 0.7721 0.4224 −1.2336 0.3472
RGB −0.0034 0.3244 0.7106 0.3593 −1.2183 0.2883
AGB −0.0145 0.0545 0.7267 0.2247 −1.2432 0.1222
RRL −0.0028 0.4196 0.7372 0.4368 −1.2214 0.3637
BL −0.0080 0.1401 0.7647 0.2907 −1.2416 0.2070
RC −0.0050 0.2576 0.7130 0.3572 −1.2196 0.2890

Notes. Parallax is in mas and proper motions in mas yr−1. As discussed in the text, the negative mean parallaxes arise because zero-point parallax corrections were not applied.

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