Various models of structure formation can account for various aspects of the galaxy formation process on different scales, as well as for various observational features of structures. Thus, the investigation of galaxies orientation constitute a standard test of galaxies formation scenarios since observed variations in angular momentum represent fundamental constraints for any model of galaxy formation.We have improved the method of analysis of the alignment of galaxies in clusters. Now, the method allows to analyze both position angles of galaxy major axes and two angles describing the spatial orientation of galaxies. The distributions of analyzed angles were tested for isotropy by applying different statistical tests.For sample of analyzed clusters we have computed the mean values of analyzed statistics, checking whether they are the same as expected ones in the case of random distribution of analyzed angles. The detailed discussion of this method has been performed. We have shown how to proceed in many particular cases in order to improve the statistical reasoning when analyzing the distribution of the angles in the observational data. Separately, we have compared these new results with those obtained from numerical simulations. We show how powerful is our method on the example of galaxy orientation analysis in 247 Abell rich galaxy clusters. We have found that the orientations of galaxies in analyzed clusters are not random. It means that we genuinely confirmed an existence of the alignment of galaxies in rich Abells' galaxy clusters. This result is independent from the clusters of Bautz-Morgan types.

The analysis of Tully's groups of galaxies belonging to the Local Supercluster (LSC) was performed. In the 1975 Hawley and Peebles [D. I. Hawley, P. J. E. Peebles, Astron. J. 80, 477 (1975)] presented the method for investigations of the galaxies orientation in the large structures. In our previous papers [W. God lowski, P. Piwowarska, E. Panko, P. Flin, Astron. J. 723, 985 (2010); W. God lowski, Astrophys. J. 747, 7 (2012)] the statistical test proposed by Hawley and Peebles for the investigation of this problem was analyzed in detail and some improvements were suggested. On this basis the new method of the analysis of galactic alignment in clusters was proposed. Using this method, God lowski [W. God lowski, Acta Phys. Polon. B 42, 2323Polon. B 42, (2011] analyzed the orientation of galaxies inside Tully's groups founding no significant deviations from isotropy both in orientation of position angles and δD and η angles as well, giving the spatial orientation of galaxy planes. In the present paper we examined carefully and methodically the dependence of alignment in Tully's groups on the morphological type of galaxies. Moreover, we discussed the consequences of different approximation of "true shape" of the galaxies for different morphological types, a possible influence of this problem for the investigation of spatial orientation of galaxies. In addition, we discussed the implications of the obtained results for the theory of galaxy formation as well.

Abstract. We present a new method of analyzing galaxy alignments in clusters originaly proposed by Godowski 2012 and now improved.

The analysis of Tully's groups of galaxies belonging to the Local Supercluster (LSC) was performed. In the 1975 Hawley and Peebles [1] presented the method for investigations of the galaxies orientation in the large structures. In our previous papers [2, 3] statistical test proposed by Hawley and Peebles for investigation of this problem was analyzed in details and some improvements were suggested. On this base the new method of the analysis of galactic alignment in clusters was proposed. Using this method, God lowski [4] analyzed the orientation of galaxies inside Tully's group founding no significant deviations from isotropy both in orientation of position angles and δ D and η angles as well, giving the spatial orientation of galaxy planes. In the present paper we examined carefully and methodically the dependence of alignment in Tully's groups on morphological type of galaxies. Moreover, we discussed the consequences of different approximation of "true shape" of the galaxies for different morphological types, possible influence of this problem for investigation of spatial orientation of galaxies. In addition, we discussed the implications of the obtained results for the theory of galaxy formation as well.