Cluster membership selection based on PMs obtained from displacements from JWST observations from two epochs collected under programme GO-2559 over a period of just 7 months. (a)-(b) VPD and m_F150W2 versus m_F150W2 − m_F322W2 CMD, respectively, for sources with measurable PMs. (c) FOV zoomed in on the region of the overlap between the two epochs, represented in green. (d) m_F150W2 magnitude versus the one-dimensional PM (μ_R). The red line separates cluster members from SMC and field stars. (e)-(f) VPD and m_F150W2 versus m_F150W2 − m_F322W2 CMD for stars that passed the PM selection. (g)-(h) same diagrams for stars that did not pass the PM selection. In panels (d) through (h), sources that passed the PM selection are represented by blue dots, while those that did not pass are depicted as orange crosses. Candidate BDs that passed and did not pass the PM selection are represented as green triangles and red crosses, respectively. The green and red error bars illustrate uncertainties: PM errors in (a), (e), and (g); colour errors in (b), (f), and (h); and errors in μ_R in (d). The uncertainties are estimated as detailed in Sect. 4.