Monika Biernacka

Letter: Rotation of the Universe and the Angular Momenta of Celestial Bodies

We discuss the equation of motion of the rotating homogenous and isotropic model of the Universe. We show that the model predicts the presence of a minimum in the relation between the mass of an astronomical object and its angular momentum. We show that this relation appears to be universal, and we predict the masses of structures with minimal angular momenta in agreement with observations. In such a manner we suggest the possibility at acquirement of angular momenta of celestial bodies during their formation from the global rotation of the Universe.

The Binggeli effect

We found the alignement of elongated clusters of BM type I and III (the excess of small values of the \Delta\theta angles is observed), having range till about 60Mpc/h. The first one is probably connected with the origin of supergiant galaxy, while the second one with environmental effects in clusters, originated on the long filament or plane.

Construction of luminosity function for galaxy clusters

The luminosity function is an important quantity for analysis of large scale structure statistics, interpretation of galaxy counts (Lin & Kirshner 1996 ). We investigate the luminosity function of galaxy clusters. This is performed by counting the brightness of galaxies belonging to clusters in PF Catalogue. The obtained luminosity function is significantly different than that obtained both for optical and radiogalaxies (Machalski & Godowski 2000 ). The implications of this result for theories of galaxy formation are discussed as well.

SOME PROPERTIES OF GALAXY STRUCTURES

Abstract We analysed some properties of galaxies structures based on the PF catalog of galaxy structures (Panko & Flin 2006) and the Tully NBG catalog (Tully 1988). At first, we analyzed the orientation of galaxies in the 247 optically selected rich Abell clusters, having at least 100 members. The distribution of the position angles of galaxies as well as of two angles describing spatial orientation of the galaxy planes were tested for isotropy, applying three statistical tests. We found the relation between the anisotropy and the cluster richness. The relation between the galaxy alignment and the Bautz-Morgan morphological type of the parent cluster is not present. A statistically marginal relation between the velocity dispersion and cluster richness is observed. We also analyzed ellipticities for 6188 low redshift (z < 0.18) poor and rich galaxy structures which have been examined along with their evolution. Finally, we analyzed the Binggeli effect and found that the orientation of galaxy groups in the Local Supercluster (LSC), is strongly correlated with the distribution of neighbouring groups in the scale up to about 20 Mpc. Analysis of galaxy structures from the PF catalog shows quite different situation - the efect is observed only for more elongated structures (e ≤ 0.3). The effect is present in a distance range of about 60 h−1 Mpc.

The application of the Faint Object Classification and Analysis System (FOCAS) and Source Extractor (SExtractor) packages to the Digitized Sky Survey

In this paper the comparison between the Faint Object Classification and Analysis System (FOCAS) and Source Extractor (SExtractor) packages for automated star–galaxy classification is discussed. The analysis presented here uses a data set containing 43 Abell clusters of galaxies obtained from the Digitized Sky Survey. Comparison is based on four image parameters: the magnitude, area, ellipticity and position angle computed for each object. Statistical analysis shows that in the case of individual clusters, in general, there is good correlation between parameters obtained from both packages. The comparison of visual classification with automatic classification from FOCAS shows that the percentage of misclassified galaxies is about 20.

On the ellipticity of galaxy clusters

We analysed 246 scanned ACO clusters and we do not find any dependence of galaxy cluster ellipticity on redshift.