Authors: Yu.G. Shevelev , V.A. Marsakov , . ... We have constructed and investigated properties of metallicity function of disk stars with different ages, proceeding from the statistically restored real altitude distributions of stars at the solar galactocentric distance. It is shown that the metallicity distribution of stars in each age range is not of Gaussian form, but it may be considered as a superposition of two normal distributions centered at -0.2 and 0.0 dex. ...

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New lUE observations of the reflection nebula IC 435 are presented, and the scattering properties of the nebular dust grains are derived. ... The UV observations plus optical data from the literature determine the most likely star-nebula geometry, the nebular dust density distribution, and the values of the albedo and the phase function asymmetry for the dust grains. ... ADS Citation Query . citations = 51 . citations vs. year [year,citations] . ...

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• HERschel Observations of Edge-on Spirals (HEROES). I. Far-infrared morphology
• Determinations of Dust Scattering Properties
• Ionization and Thermal Structures of the Absorption-Line Systems of Quasars

... ATCA HI and radio continuum observations of the peculiar southern galaxy IC2554 and its surroundings reveal typical signatures of an interacting galaxy group. We detected a large HI cloud between IC2554 and the elliptical galaxy NGC3136B. The gas dynamics in IC2554 itself, which is sometimes described as a colliding pair, are surprisingly regular, whereas NGC3136B was not detected. ... The total HI mass of the IC2554 system is approx. 2 x 10 9 Msun, a third of which resides in the HI cloud. ...

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• PhD Thesis Abstract
• Programme - Abstract
• The HIPASS Bright Galaxy Catalog

... We are using Canadian Galactic Plane Survey l 74.2њ, -3.6њ < b This poster gives preliminary results for a full-fledged analysis of the gas properties and distribution of HISA features in the CGPS. ... where T ON and T OFF are observed brightnesses on and off the HISA feature, T S is the spin or excitation temperature of the HISA gas, tau is its optical depth, T C is the continuum intensity, and p is the fraction of H I emission lying behind the HISA feature. ... GIF | ...

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• HISA Poster for the 199th Meeting of the AAS, January, 2002
• Frontiers of Astronomy with the World's Largest Radio Telescope

. Next: Spectrum Up: R CORONAE BOREALIS STARS Previous: HISTORICAL BACKGROUND . Figure: The light curve of RCoronae Borealis during a fading event in 1859 . RCB stars were first identified by their characteristic light curves. A part of the light curve of RCrB itself, taken from over a century of observations compiled by Ludendorff (1906) is shown in Figure 1 . Spectrum . Galactic distribution and absolute magnitudes . Numbers and distances . Simon Jeffery . 2002-01-25

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• STELLAR PROPERTIES
• Basic Properties
• Armagh Observatory

... Observations of the Moon eclipse on 17.09.97 have shown the Moon details contrasts had decreased and the total radio brightness had fallen at all observed frequency range (from 10% at 1.38 sm down to 2.5% at 13 sm). The fall of the Moon radio brightness has been detected during the eclipse at decemeter waves for the first time. ... Radio emission of the Copernicus crater at 1.38 and 2.7 sm has been detected for the first time. ...

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• Structure and properties of IRC+10216
• Spectral energy distribution
• Results scientific researchs LRS

... The sky distribution of the BCGs from the HSS sample is shown in Fig. 6 together with BCGs from the SBS and Case surveys (Izotov et al. [ 1993b ]; Pustilnik et al. ... First, we compare the apparent magnitude distributions of the three samples. ... The similar behaviour of the faint end of the apparent magnitude distributions infers that the Northern BCG sample may have a similar completeness down to this limiting magnitude. ...

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• Signal detection
• The ROSAT AGN
• Corrections to the probability distribution

Next: Redshift Distribution Up: Sample Identification Previous: Previously Identified Sources . ... In Figure 3, we plot the redshift distribution of DXRBS FSRQs opposite that of the 1 Jy and S4 samples. In Figure 4, we plot the redshift distribution of DXRBS BL Lacs opposite the Slew and 1 Jy samples. ... The apparent deficit of objects at the very highest luminosities is a result of the smaller area of sky covered by DXRBS compared to, e.g., the Slew and 1 Jy samples. ...

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• ESO - Thesis Topic: Properties of kinematically decoupled structures in
• Redshift Distribution

Find Similar Abstracts . ... Large scale distribution of matter - Galaxies and their clustering properties . ... 17-21, 1986 (A87-52256 23-90). ... 00/1986 . ... The distribution of galaxies in space is characterized by the existence of large inhomogeneities - the Large Scale Structure of the universe (LSS). ... Use: Authors Title Abstract Text Text Query with Keywords Return: Query Results Query Form Database: Astronomy Instrumentation Physics and Geophysics ABSTRACT QUERY USER FEEDBACK HELP ...

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• Initial Distributions of Binary Parameters
• Be/X-ray binaries and candidates
• Contents

... Abstract: We present Monte Carlo radiative transfer simulations for spiral galaxies modelled as a stellar disk and a two-phase clumpy dust distribution. ... As a general result, clumpy models are less opaque than the corresponding homogeneous models. ... 0.00 0.15 0.50 0.1 0.5 1.0 2.0 5.0 10.0 0.25 X . ... We have also produced several homogeneous models, to compare to the clumpy models. ... Homogeneous and clumpy models with the same tauV have the same dust mass. ...

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• serplines (Abstract)
• research field
• Objects, Methods, and Properties

Next: Polarization efficiency: size/shape/orientation effects Up: Optical properties of cosmic Previous: The 2175? feature . To model the interstellar polarization one needs to calculate the forward-transmitted radiation for an ensemble of non-spherical aligned dust grains. ... Let non-polarized stellar radiation passes through a dusty cloud with a homogeneous magnetic field. ... The angle between the line of sight and the magnetic field is ( ). ... where the angle is connected with and ( ). ...

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• Extinction properties (transmitted radiation)
• Optical properties of cosmic dust analogs
• Database of Optical Properties -- Level: subpage

... Chandra Observation of DEEP2 Galaxy Groups and Clusters . ... Monday: 'Normal' Galaxies, Tuesday: Cluster Formation and Evolution . ... Statistics of galaxy groups in ultradeep XMM surveys. ... What can multiwavelength observations tell about cluster/group formation as well as galaxy evolution? ... I will present results from a Chandra study of eight low-redshift clusters that has systematically measured the AGN fraction in clusters and describe their spatial, kinematic, and host galaxy...

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• http://hea-www.harvard.edu/tanagra/etc/jpb_Hinode5_96.pdf
• Comments on: chi-square distribution [Eqn] By: Alex By: vlk By: aneta By: aneta
• Statistics 310 2005-2006

... ICND-96, Saratov, Russia. ... And though a number of efficient methods of digital sound compression is developed by far, there is still a need in new efficient methods. In this report we study a possibility of application of fractal methods to compression of speech signals. ... In this method, a speech frame is divided into larger pieces called domains, and smaller ones called regions, and an optimal set of affine transformations of domains into regions is calculated. ...

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... All the galaxies are divided into 4 groups depending on the environment type; every subsample contains more than 10 galaxies. ... An effect of environments is seen both for the nuclei and for the bulges: if we consider the clusters (Virgo and Ursa Ma jor) and group centers as dense environments and the field and group periphery as sparse environments, then in the dense environments the stellar populations of S0s are in average older by 4­5 Gyr than in the sparse ones. ...

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... NGC 1530 is one of the largest barred spiral galaxies in the northern sky, with bright CO emission. ... To trace molecular gas, we observed the line, with the IRAM Interferometer. ... Properties of NGC 1530 and observational results . ... Then in a frame rotating with the potential, the periodic orbits are ellipses either parallel to the bar ( ) or perpendicular ( ), depending on the radius of the orbit. ... We observed the molecular gas in the bar of NGC 1530, a barred SBb spiral in the line. ...

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• Small scale distribution in Molecular Clouds
• Bojan Nikolic -- Phase Correction for ALMA with 183 GHz Water Vapour
• Abstract

... Empirical and theoretical modeling of 3-D structures in the solar corona is confronted by the tremendous amount of data needed to represent phenomena with a large dynamic range both in size and magnitude, and with a rapid temporal evolution. Octree representation of the 3-D coronal electron distribution offers the right compromise between resolution and size, allowing computation of synthetic images of the solar corona. ... The time interval between images is one day. ...

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• MKRMF: Multi-Dimensional Redistribution Matrices
• Time Series Analysis of Unequally Spaced Data: Intercomparison Between
• Using Massively Parallel Processing of a NLTE Spectrum Synthetic Code and an

... G.K.Strukova, D.V.Shovkun, V.N.Zverev, I.E.Batov, S.A.Zver'kov and S.S.Khasanov. ... Conductivity of YBa 2 Cu 3 O 7 - x single crystals with reduced oxygen content: anisotropy of resistivity and metal - insulator transition. ... A.M. Neminsky and D.V. Shovkun. ... Pis'ma v ZhETF, v. 65 , pp.834-839 (1997) (in english) . ... Phys. - JETP Lett., v. 65 , pp.870-876 (1997). Abstract Full Text: [ PDF (102 kB) GZipped PS (143 kB) ] . ... An English translation in : JETP Lett., v. 65 , pp.332-337 (1998). ...

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• LPCBC: Abstract, 1_5
• Physical Properties of Crystals
• Department of Solid State Physics MIPT

A comparative study of type I and type II supernovae . ... Sternberg State Astronomical Institute, Moscow, U.S.S.R. (Received 26 November, 1985) . ... No significant difference between SNe I and SNe II has been found in their radial distribution and frequency of outbursts in spiral galaxies. ... The radial distribution of type Ia SNe in spiral galaxies is only slightly steeper than the one for SNe II, while SNe Ib/c are more concentrated towards the central regions. ...

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• Zen: CASDB

... V.V.Shevchenko, Sternberg State Astronomical Institute, Moscow University, Universitetsky 13, Moscow 119899, Russia, shev@sai.msu.ru . ... 1.Sternberg State Astronomical Institute, 119899, Moscow, Russia. shev@sai.msu.ru . ... V.V.Shevchenko, Sternberg State Astronomical Institute, Moscow University, Moscow 119992, Russia, shev@sai.msu.ru . ... 119992 Moscow, Russia; . ... 2Sternberg Astronomical Institute, Moscow University, Moscow, 119992, Russia, . ... Moscow, 119992, Russia shev@sai.msu.ru . ...

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• Ekaterina A. Kozlova
• Козлова Екатерина Анатольевна

Download Izmccd (~2.7 MB). ... a) a choice of the best mode of measurements of stars and objects ("Properties/Measurement"), . b) a choice of reference stars. ... 1) necessity of presence on an image of a plenty of stars (we recommend to apply this mode, if on the frame of reference stars is more 100) . ... Sx and Sy depend from residuals at all reference stars (reference stars are marked by blue color). ... These residuals are the image of the star a minus function of a profile for each pixel. ...

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