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Based on high-latitude molecular clouds with highly accurate distance estimates taken from the literature, we have redetermined the parameters of their spatial orientation. This systemcan be approximated by a 350 × 235 × 140 pc ellipsoid inclined by the angle i = 17° ± 2° to the Galactic plane with the longitude of the ascending node l = 337° ± 1°. Based on the radial velocities of the clouds, we have found their group velocity relative to the Sun to be ( u , v , w ) = (10.6, 18.2, 6.8) ± (0.9, 1.7, 1.5) km s. The trajectory of the center of the molecular cloud system in the past in a time interval of ~60 Myr has been constructed. Using data on masers associated with low-mass protostars, we have calculated the space velocities of the molecular complexes in Orion, Taurus, Perseus, and Ophiuchus. Their motion in the past is shown to be not random. [ABSTRACT FROM AUTHOR]

We analyze the properties of galaxy clusters in the region of the Leo supercluster using observational data from the SDSS and 2MASS catalogs. We have selected 14 galaxy clusters with a total dynamical mass of 1.77 × 10 M in the supercluster region 130 by 60 Mpc in the plane of the sky ( z ≃ 0.037). The composite luminosity function of the supercluster is described by a Schechter function with parameters that, within the error limits, correspond to field galaxies and does not differ from the luminosity function of the richer Ursa Major (UMa) supercluster for the same luminosity range (the bright end). The luminosity functions of early-type and late-type galaxies in Leo at the faint end are characterized by a sharp decrease ( α = −0.60±0.08) and a steep increase ( α = −1.44± 0.10) in the number of galaxies, respectively. In the virialized cluster regions, the fraction of early-type galaxies selected by the u- r color, bulge contribution, and concentration index among the galaxies brighter than M + 1 is, on average, 62%. This fraction is smaller than that in the UMa supercluster at a 2-3 σ level. The near-infrared luminosities of galaxy clusters down to a fixed absolute magnitude correlate with their masses almost in the same way as for other samples of galaxy clusters ( L ∝ M)). [ABSTRACT FROM AUTHOR]