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tokens: (Fabricius et al. 2021 ). Radial velocity measurements in Gaia EDR3 are nearly the same as in Gaia DR2. Further details on Gaia EDR3 are available at https://www.cosmos.esa.int/web/gaia/earlydr3 . The membership selection in NGC 752 from the Gaia EDR3 data set is carried out in a region of radius 5° around its centre. This sample is termed All sources . We use ML-MOC (Agarwal et al. 2021 ) to identify cluster members using the proper motion and parallax information. While details of the membership selection are described in Agarwal et al. ( 2021 ), we briefly state it here. ML-MOC is based on the k-nearest neighbour algorithm (kNN; Cover Hart 1967 ) and the Gaussian mixture model (GMM; Mclachlan Peel 2000 ). It identifies cluster members in the PM– parameter space, independent of the spatial density of the cluster, thereby allowing for the identification of faint extended spatial structures such as tidal tails. As a first step to the membership selection, kNN is utilized to remove the obvious field stars such that the remaining member candidates have more cluster members than field stars. This is done by applying kNN to those stars within the central region of radius 1° to calculate a broad range of PM and ω values for the cluster members. For NGC 752, we find the range of PM in RA, μ α* = 8.372–11.372 mas yr −1 , PM in Dec., μ δ* = −13.948–−10.348 mas yr −1 , and ω = 1.552–5.199. The stars in All sources which fall in the aforementioned parameter ranges are termed Sample sources . Their spatial, PM, and ω distributions are shown in Fig. 1 . For the second step, a three-dimensional GMM is used in the PM–ω parameter space of the Sample sources to distinguish between the cluster and field members, also assigning a membership probability ( p memb ). Those sources having p memb ≥ 0.6 are considered as high probability members, also including all the radial velocity members. A small number of stars having 0.2 ≤ p memb ≤ 0.6 are also considered as members if their values lie within the range of values specified by the members that have p memb ≥ 0.8. This results in the identification of 282 members in NGC 752 whose spatial, PM, and ω distributions are also shown in Fig. 1 . Note the extended tails are clearly identified in the spatial distribution. The identified members with their Gaia EDR3 IDs, astrometry, photometry, radial velocity (RV), and p memb have been tabulated in Table 1 . Figure 1. The spatial, proper-motion, and parallax distributions of the Sample sources and the member stars identified by ML-MOC. Table 1. Gaia EDR3 members identified in NGC 752 using ML-MOC. The full table will be available in the online version of the journal. In Fig. 2(a) , the marked p memb values show that the extended tails are present for the high probability members showing their identification as being robust. The mean distance to the cluster is found to be 443.8 pc (see Agarwal et al. 2021 ) consistent with literature values (Agüeros et al. 2018 ).