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We use high-dispersion CCD spectrograms obtained in 1993 - 1998 to study parameter variations of the absorption and emission components Hα line of the star β Cephei. We show that radial velocity of the emission component does not depend on star pulsation and systematically differs from the star radial velocity. The star radial velocity measured on doublet CII lines and corrected for pulsation decreases quickly than ensues from orbital moving ephemeris. We suppose the envelope appears around the closer β Cep companion, and the changes of the radial velocity of the emission components Hα partially reflects the orbital moving of the closer companion. It is possible, the system periastron passage will come earlier than ensues from the present significance of the orbital period.

We present the results of analysis of 2D distribution of galaxies in galaxy cluster fields. The Catalogue of Galaxy Clusters and Groups PF (Panko & Flin) was used as input observational data set. We selected open rich PF galaxy clusters, containing 100 and more galaxies for our study. According to Panko classification scheme open galaxy clusters (O-type) have no concentration to the cluster center. The data set contains both pure O-type clusters and O-type clusters with overdence belts, namely OL and OF types. According to Rood & Sastry and Struble & Rood ideas, the open galaxy clusters are the beginning stage of cluster evolution. We found in the O-type clusters some types of statistically significant regular peculiarities, such as two crossed belts or curved strip. We suppose founded features connected with galaxy clusters evolution and the distribution of DM inside the clusters.

X-ray counterparts for 35 galaxy clusters contained in the PF catalogue of galaxy clusters and groups were found in XMM-Newton archive. 22 ones (all from ACO catalogue) have extended elliptic X-ray haloes appropriate for determination of orientation. Position angles and eccentricities were calculated and compared with cluster orientations optical band.

Wepresent the results of photometrical research of close binary system V859Cyg with possible period variations. The light curve of the star was constructed using V-band magnitudes, obtainedin 2007, 2009, 2014 years in Kalinenkov Astronomical Observatory of Nikolaev National University (Nikolaev,Ukraine). According our full light curve both eclipsesare partial ,the depths of primary and secondary minima in V–band are 0m,38 and 0m,32 respectively. We found 9 new time minima. However, the standard ephemeris of primary eclipse corresponds to our secondary minimum and vice versa during all observational seasons.We obtained the parameters of binary system from light curve using Binary Maker 3 package. The inclination of orbit of V859 Cyg system is 64,◦5. The temperatures of components are TeffI =7100K, TeffII =6850K and mass ratio is 0.35. Both components are deformed by mutual gravity and overfill own Roshe lobes, fillout factor is 0.875 for both stars. Mean radii of components are 0.51 and 0.33 of distance between stars. We attributed V859Cyg as overcontact system with stable period 0,d4050066.

The morphological types of galaxy clusters resulting from their out ward appearance is physically related to the clusters and their member galaxies. Presented here is an adopted system of morphological types of galaxy clusters based on the Zwicky, Boutz&Morgan, Rood&Sastry, and L´opez-Cruz systems. The adopted types are suitable for automated classification of galaxy clusters from The Catalogue of Galaxy Clusters and Groups (Panko& Flin 2006). Numerical criteria describing 6 main types were distinguished: Concentrated C, Intermediate I, Open O, Line L, Flat F, and cD. The types correspond to the base divisions from regular to irregular clusters, but also note the presence of preferential direction or plane in each cluster.

We present the results of research of scantily explored close binary system V841 Cyg with possible period variations. It was attributed as /3 Lyr and as near contact binary star. We obtained light curve of the star in July 2013 in V-band. Both eclipses are partial, the depths of primary and secondary min­ima are 0m.53 and 0m.20. Light curve has feature near primary minimum: practically horizontal parts in phases ±(0.1 — 0.16). We found new time minima: HJDI = 2456504.48122, BJDH = 2456493.44562. We obtained new parameters of binary system using Binary Maker 3 package. The system contains from A6 V+G5 V stars with mass ratio about 0.49. The components have temperatures TeffI = 8550°, TeffI = 5500° and estimated masses MI = 1.85, MII = 0.90; they fill own Roshe lobes on 95% and 92% correspondingly and both components are de­formed. The distance between components is about 5R©, the distance between component surfaces is about 1.4R©. We confirm the V841 Cyg classification as is NCB system, with not significant mass transfer.

We present the results of analysing of the light curve and O–C variations in the eclipsing system BM UMa, based on V-band observations which cover the period from JD 2454933 to 2454961 using two robotic remotely-controlled telescopes of Tzec Maun Observatory (USA) along with observations made with the RK-600 telescope of Odessa Astronomical Observatory. The full light curve displays a total primary eclipse with a duration 0.06 of the period, or 24 minutes, and a partial secondary eclipse, with both maxima of equal magnitude. For our obesrvations, we determined the statistically optimal values of the initial epoch of T0 = 2454944.2814 ± 0.0001 and orbital period of P = 0.d271226± 0.000002. The depths of primary and secondary minima are nearly equal, 0.m838 ± 0.006 and 0.m748 ± 0.006, respectively. The physical parameters of the system were calculated using the Wilson-Devinney code, appended with the Monte Carlo search algorithm. The result establishes BM UMa as a contact system (fillout factor 10.7%) with parameters: mass ratio 0.538 ± 0.001, inclination 86.°815 ± 0.005, and temperatures of components 4700 ± 20 K and 4510 ± 10 K. The more massive component is larger and cooler. The 72 archival and 11 newly-obtained times of light minimum cover the interval 1961-2010 and allowed us to exclude possible systematic period variations in BM UMa and to determine an initial epoch of HJD 2447927.382 and orbital period of P = 0.d2712209± 0.0000006.

The distribution of galaxy clusters is analyzed in regions of 6 galaxy superclusters with both measured and estimated redshifts. The positions of ACO and APM galaxy clusters in the regions are compared with the positions of galaxy clusters and groups from a new catalogue based on the Muenster Red Sky Survey. The locations of galaxy clusters and groups are shown on 10° x 10° maps of the fields. A comparison is made between maps that include all galaxy clusters and groups, rich and poor clusters, and only rich clusters. The resulting large-scale structure in the regions is described in detail on the basis of both rich and poor clusters, and a new catalogue is produced that is convenient for further study of galaxy superclusters.

We discuss the possibility of using the Cluster Cartography set for the determined the morphological types of galaxy clusters. The applied morphological scheme was proposed by Panko (2013). The morphological types are determined using numerical criteria based on three parameters: concentration to the cluster center, the signs of preferential direction or plane in the cluster (filamentary substructure), and the positions of the brightest galaxies. However, structures like galaxy clusters need visual preview for classification. The Cluster Cartography set constructs the individual cluster map in different forms and allows to estimate previously cluster type.

We determined the morphological types for 254 rich galaxy clusters from the PF Catalogue of Galaxy Clusters and Groups. The data set contains the PF galaxy clusters, which have no ACO coinciding ones. The applied morphological scheme was combined of the prevalent classifications, such as Bautz-Morgan, Rood-Sastry etc approaches. We assigned the morphological types using numerical criteria and taking into consideration concentration tothe cluster center, the signs of preferential direction or plane in the cluster, and the positions of the brightest galaxies. The features of the data set are discussed.

The distribution of galaxy ellipticities was analyzed for 207 rich PF galaxy clusters found in the Munster Red Sky Survey Galaxy Catalogue. Clusters with BM types from a comparison with the ACO catalogue were also classified on the new scheme. The new morphological types take into consideration concentration towards the cluster center, indicationsof a preferential direction or plane, and the role of the brightest cluster galaxies. Differences in the distribution of galaxy ellipticities for individual clusters are statistically significant, in contrast to the average distribution of ellipticities for galaxies belonging to clusters of different morphological type. Two types of galaxy ellipticity distribution were found: single-modeand bimodal. The distributions apparently reflect different contributions from spiral and elliptical galaxies. The shapes of galaxies in individual clusters appear to relate to local conditions.