Pleiades member candidates via STARGO with Gaia EDR3

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.本数据集采用STARGO方法选取昴星团成员星，所用数据来自盖亚早期第三批数据发布（Gaia Early Data Release 3, EDR3；Gaia Collaboration et al. 2021），相关详细描述参见Li等人2021年的研究（已投往美国天文学会研究快报，待刊）。我们以日心笛卡尔坐标系（Heliocentric Cartesian coordinates）下的昴星团中心坐标$(X,Y,Z)=(-121.38, +29.17, -54.47)$ pc为基准，下载了距离该中心100 pc范围内的盖亚EDR3数据（Galli et al. 2017; Olivares et al. 2018）。在剔除伪影与低质量测光源（Lindegren et al. 2018）后，我们选取了距离昴星团平均自行（proper motion）中心$(mu_alpha cosdelta, mu_delta)=(+19.997, -45.548)$ mas yr⁻¹半径10.8 mas yr⁻¹范围内的恒星（Gaia Collaboration et al. 2018），并将5维参数$(X,Y,Z, mu_alpha cosdelta, mu_delta)$输入STARGO方法。本研究允许识别出的成员星中存在5%的场星污染率。我们采用Carrera等人（2019）与Pang等人（2020, 2021）提出的贝叶斯方法，校正了因视差误差（parallax error）产生的伪伸展效应对昴星团单颗恒星距离的影响。昴星团单颗成员星的质量通过k-D树方法计算：以年龄为125 Myr、$A_V=0.11$星等、$[ ext{Fe/H}]=0.08$的等龄线（isochrone，Lodieu et al. 2019; Gossage et al. 2018）中最近邻点的质量作为该恒星的质量估计值。其中，"x_c"、"y_c"、"z_c"为经距离校正后的日心笛卡尔坐标系下星团位置参数；"Mass"代表通过k-D树方法得到的每颗成员星的质量估计值（Millman & Aivazis 2011）。其余参数的详细说明可通过在TOPCAT软件中打开FITS文件查看。