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Fig. 11.


Proper motion diagram of the NGC 3532 field. Left panel: all stars common to the catalogues of C11 and Gaia DR2. In this plot no difference between the proper motions of the field and cluster stars is visible. Right panel: same as left but zooming in on the region outlined on the left, with the sample limited to the spectroscopically observed stars. Here the cluster (black dots) is distinguishable from the field (crosses and grey squares). We have separated the field into the background giant component (grey squares) and the foreground component (crosses). The histograms show the distribution of radial velocity members (black) and background giant stars (grey). The dashed lines give the centre of the distribution of the members (μα = −10.37 ± 0.16 mas yr−1, μδ = 5.18 ± 0.08 mas yr−1) and the circle defines the region of proper motion members.

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