Pleiades member candidates via STARGO with Gaia EDR3

<p>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.&nbsp;</p> <p>We downloaded the Gaia EDR3 data 100 pc from the center of Pleiades (X, Y, Z) = (&minus;121.38, +29.17, &minus;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^&minus;1 from the center of the mean proper motion (&mu;&alpha; cos &delta;, &mu;&delta; ) = (+19.997,&nbsp;&minus;45.548) mas yr^-1&nbsp;of Pleiades (Gaia Collaboration et al. 2018) and input the 5D parameters (X,&nbsp;Y,&nbsp;Z, &mu;&alpha; cos&delta;, &mu;&delta;) into STARGO. We allow a 5% field star contamination rate in our identified members.</p> <p>We correct the distance of individual stars in Pleiades for the pseudo-elongation generated by parallax errors, via a Bayesian approach described in&nbsp;Carrera et al.&nbsp;(2019) and&nbsp;Pang et al.&nbsp;(2020,&nbsp;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&nbsp;AV&nbsp;= 0.11 mag and [Fe/H] = 0.08&nbsp;(Gossage et al. 2018).</p> <p>&quot;x_c&quot;, &quot;y_c&quot;, &quot;z_c&quot; are the cluster position with distance correction&nbsp;in Heliocentric Cartesian coordinates. &quot;Mass&quot; represents the mass estimate of each star member via k-D&nbsp;tree method&nbsp;(Millman &amp; Aivazis 2011). The descriptions of other parameters are found by&nbsp;opening the&nbsp;fits. file in TOPCAT.</p>