We report the results of a study of the distribution of galaxies in the projection along the radius (\(R \leqslant 3{{R}_{{200{\text{c}}}}}\)) for 157 groups and clusters of galaxies in the local Universe (0.01 < \(z\) < 0.10) with line-of-sight velocity dispersions 200 < \(\sigma \) < 1100 km s^–1. We introduce a new observed boundary for the halos of clusters of galaxies, which we identify with the splashback radius \({{R}_{{{\text{sp}}}}}\). We also identified the core of groups/clusters of galaxies with the radius \({{R}_{{\text{c}}}}\). These radii are determined by the observed integrated distribution of the number of galaxies as a function of squared angular radius from the center of the group/cluster, which (usually) coincides with the brightest galaxy. We found for the entire sample that the boundary of dark matter \({{R}_{{{\text{sp}}}}}\) for groups/clusters of galaxies is proportional to the radius \({{R}_{{{\text{200}}}}}\) of the virialized region. We measured the mean radius \(\langle {{R}_{{{\text{sp}}}}}\rangle = 1.14 \pm 0.02\) Mpc for groups of galaxies (\(\sigma \leqslant 400\) km s^–1) and \(\langle {{R}_{{{\text{sp}}}}}\rangle = 2.00 \pm 0.07\) Mpc for clusters of galaxies (\(\sigma > 400\) km s^–1). The mean ratio of radii is \(\langle {{{{R}_{{{\text{sp}}}}}} \mathord{\left/ {\vphantom {{{{R}_{{{\text{sp}}}}}} {{{R}_{{{\text{200c}}}}}}}} \right. \kern-0em} {{{R}_{{{\text{200c}}}}}}}\rangle = 1.40 \pm 0.02\), or \(\langle {{{{R}_{{{\text{sp}}}}}} \mathord{\left/ {\vphantom {{{{R}_{{{\text{sp}}}}}} {{{R}_{{{\text{200m}}}}}}}} \right. \kern-0em} {{{R}_{{{\text{200m}}}}}}}\rangle = 0.88 \pm 0.02\).

我们报告了157 组星系在沿半径 ( \(R \leqslant 3{{R}_{{200{\text{c}}}}}\) 投影分布的研究结果，并且本地宇宙中的星系团 (0.01 < \(z\) < 0.10)，视线速度色散 200 < \(\sigma \) < 1100 km s ^–1。我们为星系团的光晕引入了一个新的观测边界，我们将其标识为溅射半径\({{R}_{{{\text{sp}}}}}\)。我们还确定了半径为\({{R}_{{\text{c}}}}\) 的星系群/星系团的核心. 这些半径由观察到的星系数量的综合分布确定，该分布是星系群/星系团中心角半径平方的函数，星系团（通常）与最亮的星系重合。我们发现对于整个样本，星系群/星系团的暗物质边界\({{R}_{{{\text{sp}}}}}\)与半径\({{R} _{{{\text{200}}}}}\)的维化区域。我们测量了星系群的平均半径\(\langle {{R}_{{{\text{sp}}}}}\rangle = 1.14 \pm 0.02\) Mpc ( \(\sigma \leqslant 400\) km s ^–1 ) 和\(\langle {{R}_{{{\text{sp}}}}}\rangle = 2.00 \pm 0.07\)星系团的 Mpc (\(\sigma > 400\) km s ^–1 )。半径的平均比率为\(\langle {{{{R}_{{{\text{sp}}}}}} \mathord{\left/ {\vphantom {{{{R}_{{{\ text{sp}}}}}} {{{R}_{{{\text{200c}}}}}}}} \right. \kern-0em} {{{R}_{{{\text{ 200c}}}}}}}\rangle = 1.40 \pm 0.02\)或\(\langle {{{{R}_{{{\text{sp}}}}}} \mathord{\left/ { \vphantom {{{{R}_{{{\text{sp}}}}}} {{{R}_{{{\text{200m}}}}}}}} \right. \kern-0em } {{{R}_{{{\text{200m}}}}}}}\rangle = 0.88 \pm 0.02\)。