Markers of Evolution in Rich Galaxy Clusters Elena Panko (panko.elena@gmail.com) and Sviatoslav Yemelianov, Anton Sirginava Department of Theoretical Physics and Astronomy, I. I. Mechnikov Odessa National University, Odessa, Ukraine Elena Panko The idea, formulation of the problem, input data, lgorithm, etc Sviatoslav Yemelianov soft, ~200 rich galaxy clusters data analysis, discussion Anton Sirginava Input data, ~200 rich galaxy clusters data analysis, discussion Abstract We detected statistically significant regular substructures in 2D distribution of galaxies in rich clusters with redshifts till to 0.15. Input data were extracted from “The Catalogue of Galaxy Clusters and Groups” (Panko & Flin, 2006). Main type of substructures is linear elongated overdence regions in the cluster field. The direction of the linear substructure points usually to the nearest neighbor. In additional we found X- or Y- type regular substructures as well as short and/or compact chains. Bright galaxies in clusters are located in the regular substructures mainly and galaxies in the chains also show significant alignment along the chain. Founded peculiarities can be considered as a result of the formation of galaxy cluster at the intersection of DM filaments or filament-wall interaction. Input data format: The real 4200"4200" field of PF 0381-1789 cluster from DSS-R (upper panel) and the CC map 4000"4000". The background stars are present on the real frame. Weak galaxies on the frame are not visible. The reasons for present study: According to CDM model computer simulations the distribution of galaxies in the clusters is the point index of the hot gas and DM distribution: Gas density tracing the cosmic web in a subvolume (12.5 Mpch-1 comoving horizontally, stacked over 25 Mpch-1 comoving along the line of sight) of the HORIZON- AGN simulation (Codis, Gavazzi, et al.,2015) Projected density map, nodes in filaments. GADGET-4 code (Wang et al., 2020) We supposed the ways of evolution in 2D distribution of galaxies are reflected as: O  I  C  cD (Struble & Rood,1982) or O  OL  IL  CL  C  cD (Panko, 2019) or O  O (X, Y, c)  I(X,Y, c)  IL  CL  C  cD (present study), were types of galaxy clusters: O  Open, I  Intermediate, C  Concentrated, cD  having cD galaxy, L  linear substructure, X,Y, c  other regular peculiarities (Panko, 2013, Panko et al., in prep.) Input Data: MRSS, the list of galaxies and PF Catalogue of galaxy clusters and groups The Muenster Red Sky Survey. It covers an area of about 5000 deg2 on the southern hemisphere. The catalogue includes 5.5 million galaxies and is complete till to rF=18m.3 (Ungruhe et al., 2003). It's a result of scanning of 217 plates of Southern Sky Atlas R (ESO) by PDS 2020GMplus and automated recognition of galaxies with careful control. White spot is the region around the SMC. PF Galaxy clusters (based in the MRSS (Panko & Flin, 2006). Our data set contains 460 rich galaxy clusters contain 100 and more members. MRSS Cluster data 0016-5711 0.1670739 -57.107367 940 2130600 88 31 48 907 617 0.32 117.4 13.02 13.72 15.05 97.4 0.41 22.8 Galaxies data 149-40043 59 2.75 5.30 3.85 0.31 24.0 16.56 16.53 0.136070 -57.054264 149-39501 21 2.15 4.26 2.51 0.49 178.0 17.98 17.95 0.139043 -57.081429 111-51504 394 6.14 12.73 7.33 0.51 16.5 14.81 14.77 0.140979 -57.240734 111-50854 111 4.09 7.88 4.37 0.54 19.1 16.35 16.32 0.143299 -57.250084 149-38602 36 3.27 7.23 2.99 0.72 34.9 17.53 17.50 0.143872 -56.993507 Cluster Cartography (CC) set allows to visualize the input data and to analyze the distribution of galaxies as well as to study the orientations of cluster members. CC allows automatically: to determine the level of the concentration to the cluster center; to detect linear substructures and other types of regular substructures, namely crosses, semicrosses. Curved chains and compact short dense stripes are need visual control. The shape of symbol corresponds to MRSS data, the size of symbols corresponds to