## 5 Conclusions  
Data from the Tully Nearby Galaxies Catalog were used to implement a new research method. It also made it possible to check the results of the method using research papers containing a detailed analysis of the orientation of galaxies belonging to the catalog. The obtained results seem to confirm the effectiveness of the new method. However, when calculating, one should also take into account catalog effects specific to the analyzed data. The obtained data show that the omission of the Holmberg effect in the case of data from galaxy catalogs, for which this effect is significant, does not lead to correct results. It should be noted, however, that the current dominant view is that for catalogs based on automatic galaxy measurements, the Holmberg effect should not be significant. In order to fully assess the effectiveness of the new method of investigation of the orientation of galaxies, trials on other observational data are planned. Additionally, we confirmed that in small groups and clusters of galaxies, such as Tully clusters, there is no galaxy alignment. This is consistent with previous observations,  
Figure 12: Maps of \(s\equiv\Delta_{11}/\sigma(\Delta_{11})\) versus the chosen cluster pole supergalactic co-ordinates (\(L\), \(B\)) for the Cluster 15, with results obtained with help of HHD and FP corrections. The maps are presented for all cluster galaxies (upper), as well as for spiral (middle) and non-spiral (bottom) sub-samples. In the map, we indicate the important directions, as seen from the center of the considered cluster: (1.) three cluster poles (full star, square and triangle), (2.) the direction to the Local Supercluster center (open circle), (3.) the direction of the Virgo A cluster center (open square) and (4.) the line of sight from the Earth (asterisk). in which the alignment of galaxies in the structures increases with their mass and is not observed in small groups and clusters of galaxies, in contrast to rich clusters of galaxies, where such ordering is observed. This result is important from the point of view of testing scenarios for the formation of galaxies and their structures. This is because, some models, such as the original hierarchical clustering model [65], do not predict the alignment of galaxies in the structures at all, and other models, such as primordial turbulence [66] or the new version of the Zeldovich pancake model [67], predict the ordering of the orientation of galaxies in clusters, but are unable to explain the dependence of this effect on the mass of the structure. Fortunately, there are also models that predict that the ordering of galaxies in clusters increases with their number [68; 69]. However, it should be remembered that the correct scenario for the formation of galaxies and their structures must take into account the existence of dark matter. This is the main problem with most such models, which have difficulty accounting for the existence of dark matter. Only models based on the idea of hierarchical clustering [65], including, in particular, its new version, taking into account tidal effects [68], explicitly takes into account the presence of dark matter, although also in the Li model [69] is the existence of dark matter as a background taken into account. This means that the observational picture discussed above favors galaxy formation and structure scenarios that predict such a relationship, and takes dark matter into account, as, for example, tidal torque scenarios in the hierarchical clustering model [68], however, the Li model [69] is also allowed. Moreover, our results (lack of alignment in [PERSON]'s group) suggest that small-scale, local environmental effects dominate over cosmic anisotropy. Finally, it should be noted that our method is of great importance for the future study of galaxy clusters. Recently, new surveys of galaxies have appeared, such as, for example, SDSS Sky Surveys [70; 71], DESI [72] and Euclid [73]. On the basis of these surveys, catalogs of galaxy clusters can be compiled.