Members of the Pleiades open cluster are selected by using the STARGO method (Yuan et al. 2018) with Gaia early data release 3 (EDR3; Gaia Collaboration et al. 2021) data. See Li et al. 2021 (in prep. for Research Note of the AAS) for a detailed description. We downloaded the Gaia EDR3 data 100 pc from the center of Pleiades (X, Y, Z) = (−121.38, +29.17, −54.47) pc in Heliocentric Cartesian coordinates (Galli et al. 2017; Olivares et al. 2018). After removing artifacts and poor quality photometric sources (Lindegren et al 2018), we select stars within a radius of 10.8 mas yr^−1 from the center of the mean proper motion (μα cos δ, μδ ) = (+19.997, −45.548) mas yr-1 of Pleiades (Gaia Collaboration et al. 2018) and input the 5D parameters (X, Y, Z, μα cosδ, μδ) into STARGO. We allow a 5% field star contamination rate in our identified members. We correct the distance of individual stars in Pleiades for the pseudo-elongation generated by parallax errors, via a Bayesian approach described in Carrera et al. (2019) and Pang et al. (2020, 2021). The mass of individual members in Pleiades is computed via the k-D tree method by taking the mass of the nearest point in the isochrone of 125 Myr (Lodieu et al. 2019) with AV = 0.11 mag and [Fe/H] = 0.08 (Gossage et al. 2018). "x_c", "y_c", "z_c" are the cluster position with distance correction in Heliocentric Cartesian coordinates. "Mass" represents the mass estimate of each star member via k-D tree method (Millman & Aivazis 2011). The descriptions of other parameters are found by opening the fits. file in TOPCAT.