The struve dynasty in the history of astronomy in Ukraine

The impact of the Struve astronomical dynasty on the development of astronomy in Ukraine in the 19th–20th centuries is studied. First of all, the role of F.G.W. Struve and O.V. Struve in the formation of astronomical research programs at the observatories at the Kharkiv, Kyiv, Odesa, and Mykolayiv, in equipping the observatories with instruments, in practical training of astronomers as well as in the organization of astronomy-geodetic expeditions (19th century). Particular attention is paid to the activity of L.O. Struve as a director of the Astronomical observatory of Kharkiv University and his works conducted together with G.A. Shajn and B.P. Gerasimovich (20th century) as well as to the impact of his scientific and public activity, including one he made as a President of IAC, on the development of astronomy in the Soviet Union and Ukraine. A range of important documents from the archives of Russian Academy of Sciences, Institute of astronomy and State Archive of Ukraine are cited. The article was translated by the authors.     

The distant galaxy cluster XLSSJ022403.9-041328 on the L X –T X –M scaling relations using Chandra and XMM–Newton observations

We present a very detailed analysis of Chandra and XMM–Newton observations of XLSSJ022403.9-041328 galaxy cluster of z=1, which was detected during the XMM-Newton Large Scale Structure survey. To define the “luminosity-temperature-mass”, L _X –T _X –M, scaling relations we built temperature, surface brightness, density, and mass profiles. The total gravitational mass of this cluster was taken within the scaled radius, R ₅₀₀, was determined under the assumption of hydrostatic equilibrium for intercluster gas and spherical symmetry of a cluster. The temperature of XLSSJ022403.9-041328 was found to be 4.5±0.7 keV from the Chandra data, and 3.8±0.3 from the XMM–Newton data. The total gravitational mass is equal to 1.44±0.23×10¹⁴ M _⊙ at the corresponding radius, while the fraction of gas is equal to 15 % of a total mass. These values were used to define the XLSSJ022403.9-041328 galaxy cluster at the L _X –T _X –M _g scaling relations, and for all of these cases we got agreement which fitting well with self-similar model. This research permits us to use L _X –T _X –M relations for galaxy clusters at a highest redshift in the cosmological probes.     

Mass-to-light ratios for galaxy pairs and triplets in various environments

We have estimated the dark matter content in galaxy pairs and triplets selected from SDSS DR5 by a higher-order Voronoi tesseleration method. Specifically, the median mass-to-light ratios M _vir/L are 12 M _⊙/L _⊙ for isolated pairs, 44 M _⊙/L _⊙ for isolated triplets, and 7 (8) M _⊙/L _⊙ for compact pairs (triplets) with a characteristic distance between the galaxies of R < 50 (100) kpc. We show that the less isolated a system, the larger its mass-to-light ratio. This suggests that galaxy groups in a denser environment have a higher velocity dispersion.     

An observational study of the structure of the nocturnal boundary layer

In an effort to describe the basic vertical structure of the nocturnal boundary layer, observations from four experiments are analyzed. During the night, the depth of significant cooling appears to increase with time while the depth of the turbulence and height of the low level wind maximum tend to remain constant or decrease with time. Since the inversion layer extends above the low level wind maximum and shear is small in the region of the low level jet, the Richardson number reaches a maximum at the jet level and then decreases again with height. As a result, turbulence is observed to be a minimum at the height of the low level wind maximum and then increases again above this height.The National Center for Atmospheric Research is sponsored by the National Science Foundation.Part of this work was performed while a visiting scientist at Oregon State University.     

Distinguishing between lodgement till and flow till in Weichselian deposits

Lodgement till and flow till are depositcd in quite different environments. In Weichselian depmits, they can be distinguishcd by the setting of the sediments, the fabric, geotechnical characters, and the morphological appearance. These indications support each other. Of the outlined methods, the morphological is the most convenient in practice. Since flow till normally exists together with meltwater sediments it is suggested that systematic morphological mapping will be time-saving and most profitable for the prospecting of economically important clay, sand, and gravel deposits.     

Supposed area-wasting of the Weichselian ice sheet in Denmark

The deglaciation at the end of the Weichselian in the Danish area has previously been considered to occur as a frontal wastage. Since the glacier ice was assumed to be debris-free, the wasting should be characterized by outwash plains and successions of end-moraines. The almost complete lack of sandur plains in the eastern part of the area and indications from recent investigations of widespread occurrence of flow till justify a re-evaluation of the mentioned deglaciation model.
Two morphological features have a general occurrence: the plains and the 'tunnel' valleys. The plains appear stepwise in the landscapes, and are frequently limited by steep slopes. Topmost is a subcircular kame-like hill. Sedimentologically, the plains mainly consist of melt water deposits, and the scattered occurrences of till are interpreted as flow till. The plains continue from the open landscape into the 'tunnel' valleys where they appear as terraces.
These features are considered to have been formed during the deglaciation. The almost horizontal surface of the ice sheet over large areas caused a sensitivity to changes in the climate. The wasting of the ice may therefore be expected to affect large areas almost simultaneously. On the assumption that the ice contained debris, an increasing amount of clastic matter was released on the ice surface. This material was concentrated in the depressions. If such a depression perforated the ice, the content of sediments settled on the substratum and a plain was established. During continued wasting the thickness of the ice decreased and the depressions were enlarged. They assumed the character of sandur plains. As still larger areas of these supraglacial sandurs rested on the basement the successive lower situated plains were formed. The latest ice was preserved where the 'tunnel' valleys are situated to-day.     

Astroinformation resource of the Ukrainian virtual observatory: Joint observational data archive, scientific tasks, and software

This paper reviews the most important components of the national project of the Ukrainian Virtual Observatory (UkrVO). Among them, there is the establishment of a Joint Digital Archive (JDA) of observational data, which has been obtained at Ukrainian observatories since the 1890s, including an astronegative JDA (more than 200 thousand plates). Since this task requires VO-oriented software, such issues as content verification software, integrity and administration of the JDA, compliance of image formats with the IVOA standards, and photometric and astrometric calibration of images are considered as the most important directions of software development, which carried out by members of the UkrVO. The scientific projects using local data archives of the UkrVO are discussed, namely: an analysis of a long observational series of active galactic nuclei, the study of solar flares and solar active regions based on spectral observational archives, research and discovery of variable stars, and the study of stellar fields in the vicinity of gamma-ray bursts. Particular attention is devoted to the CoLiTec Program that permits us to increase a number of observed solar system bodies and allows us to discover new bodies; for example, the C/2010 (Elenin) and P/2011 N01 comets were discovered using this program at the ISON-NM Observatory. The paper notes the creation of the UkrVO JDA prototype that provides access to the databases of the Main Astronomical Observatory, National Academy of Sciences of Ukraine (MAO NAS of Ukraine); Nikolaev Astronomical Observatory (NAO); and Lvov Astronomical Observatory.