... Method A simple radiative transfer model representing a HISA cloud with fore­ ground and background H i emission and background continuum emission is described by the expression T ON - T OFF =  T S - T C - p T OFF   1 - e -#  , (1) where T ON and T OFF are observed brightnesses on and o# the HISA feature, T S is the spin or excitation temperature of the HISA gas, # is its optical depth, T C is the continuum intensity, and p is the fraction of H i emission lying behind the HISA feature. ...

Еще в разделе: (Показать все результаты (>4614) - www.naic.edu/ )

• HISA Poster for the 199th Meeting of the AAS, January, 2002
• HISA Poster for the 195th Meeting of the AAS, January, 2000
• HISA Poster for the 33rd Annual Meeting of CASCA, May, 2002

... 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. ...

Еще в разделе: (Показать все результаты (>1107) - jet.sao.ru/ )

• Spectral energy distribution
• Structure and properties of IRC+10216

... 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. ...

Еще в разделе: (Показать все результаты (>3005) - www.sao.ru/ )

• Group IAG
• Improvement of selection criteria

SAI 175 anniversary . ... Moscow University . Search for in SAI Moscow University Search for in Russian astronomical resources . ... SAI Astronomical Databases . ... Browse SAI Software archive(ftp.sai.msu.su) . ASTRONET.RU - Russian Astronomical Network (available in translit also) . ... SAI Supernovae Research Group . ... Department of the Galaxy and Variable Stars (in Russian) . Sternberg Astronomical Institute Seminars . ... All-Russian Astronomical Olympiad (in Russian) . ...

Еще в разделе: (Показать все результаты (>8279) - www.sai.msu.su/ )

• SNe related preprints
• SAI SN RESEARCH GROUP

This is a tabulation of interstellar dust scattering properties dertermined from observations of various astrophysical objects (eg., ... Almost all studies in this field aim to determine the single scattering albedo (a) and scattering phase function asymmetry (g = <cos( )>) as different wavelengths. ... Plot Details . ... Plot details links to a page describing the studies included in the plot, the radiative transfer model used in each study, and an ascii listing of data plotted. ...

Еще в разделе: (Показать все результаты (>18830) - www.stsci.edu/ )

• Untangling the Nature of Spatial Variations of Cold Dust Properties in Star
• Modeling of the Blue Bump Emission in High Redshift Quasars.
• The mass-loss return from evolved stars to the Large Magellanic Cloud. III.

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 ( ). ...

Еще в разделе: (Показать все результаты (>418) - www.astro.spbu.ru/ )

• The 2175? feature
• Optical properties of cosmic dust analogs
• Extinction properties (transmitted radiation)

Old subtables of the extended ``HIPASS Bright Galaxy Catalog'' . ... Koribalski, Staveley-Smith, Kilborn, + HIPASS/ZOA teams 2004, AJ 128, 16 . The 1000 Brightest HIPASS Galaxies: HI Properties . ... The 1000 Brightest HIPASS Galaxies: The HI Mass Function . ... The 1000 Brightest HIPASS Galaxies: Newly Cataloged Galaxies . ... To download the gzipped ps-file click here . ... The Brightest Galaxies from HIPASS . Presented is the distribution of the 700 brightest HIPASS galaxies. ...

Еще в разделе: (Показать все результаты (>18062) - www.atnf.csiro.au/ )

• HIPASS Bright Galaxy Catalog
• ATNF Colloquium
• Evolutionary Paths in Galaxy Morphology

Next: Pulsations Up: PHYSICAL CHARACTERISTICS Previous: PHYSICAL CHARACTERISTICS . The fundamental properties of RCBs may be deduced from their spectra at maximum light. ... The properties of a stellar atmosphere may be measured from both the large-scale features - the broad-band flux distribution - and the detailed spectrum of absorption lines. ... They show that, in general, hydrogen makes up less than one part per thousand down to less than one part per million of the stellar atmosphere. ...

Еще в разделе: (Показать все результаты (>2918) - star.arm.ac.uk/ )

• BASIC PROPERTIES
• Basic Properties
• STELLAR PROPERTIES

FEATURES OF THE HYDROGEN DISTRIBUTION AROUND LUNAR CRATERS PROCLUS AND KEPLER. ... In result of analysis of the data Lawrence and Feldman constructed the hydrogen distribution on the lunar surface [1]. ... However, the authors shown, that EN flux data features may be explained by other element abundance in the lunar soils, namely: Si, Ca, Gadolinium (Gd), Samarium (Sm) and Fe. ... Using of the Feldman's interpretation of the Lunar Prospector data [8], we constructed hydrogen distribution map (Fig.1). ...

Еще в разделе: (Показать все результаты (>137) - selena.sai.msu.ru/ )

• http://selena.sai.msu.ru/Shev/Publications/ms38/ms083.pdf
• http://selena.sai.msu.ru/Shev/Publications/m44_75_shevchenko_etal.pdf
• Шевченко Владислав Владимирович

Subject, Problems and Objects of Theoretical Astrophysics. ... Stellar Photospheres, Their Features. ... Physics of Continuous Radiation Absorption in Stellar Photospheres. ... Continuous Radiation Absorption in Stellar Photospheres of Various Spectral Classes. Solar Type Photospheres. ... Characterisics of Absorption Lines. ... Interstellar Absorption Lines, Their Features. ... Physical and Dynamic Features of Interstellar Medium, Which Follows from Observations of Interstellar Absorption Lines. ...

Еще в разделе: (Показать все результаты (>78) - space.univ.kiev.ua/ )

• Practical Astrophysics
• Extragalactic Astronomy
• General Astrophysics

... 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. ...

Еще в разделе: (Показать все результаты (>9231) - www.arcetri.astro.it/ )

• Objects, Methods, and Properties
• Client-Side JavaScript Guide
• research field

... 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. ...

Еще в разделе: (Показать все результаты (>2327) - www.mrao.cam.ac.uk/ )

• Small scale distribution in Molecular Clouds
• Astrophysics Group Exploring the Cosmic Dawn

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. ...

Еще в разделе: (Показать все результаты (>52066) - www.eso.org/ )

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

... What are the fluxes of the stars? ... Volume sampled is no longer 4/3 pi r cubed due to curved space-time Want to derive population properties brightness, size, etc - as function of distance (therefore, cosmic time) But - biases in sample Biases NUMBER OF STARS VS MASS Eddington Bias: in astronomy, there are always more little faint things than big bright things. ... Suppose there are 10 stars of mass 0.5 and 100 stars of mass 0.4, and you have a 20 percent error on measuring the mass. ...

Еще в разделе: (Показать все результаты (>4936) - hea-www.harvard.edu/ )

• H/RCULES
• Martin Elvis - Home Page
• The AstroStat Slog Blog Archive chi-square distribution [Eqn]

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. ...

Еще в разделе: (Показать все результаты (>125) - ip.rsu.ru/ )

• Subsystems of the Galactic halo, figures

... Institute of Solid State Physics, Academy of Sciences of the USSR . Percolation theory is used for a comparative analysis of curves of the superconducting transition in ceramic YBa 2 Cu 3 O 7 - in a zero magnetic field found through measurements of the resistance, R ( T ), and the dynamic susceptibility, ( T ). When there is an oxygen deficiency ( > 0), the grains have a wide distribution with respect to the superconducting transition temperature T c . PACS: 74.70.Vy, 74.60.Mj ...

Еще в разделе: (Показать все результаты (>1509) - www.issp.ac.ru/ )

• Grants LSR ISSP RAS
• SPECIALITY 01.04.07 - CONDENSED MATTER PHYSICS ADMISSION EXAMINATION PROGRAM
• LHPP ISSP RAS

In this gallery are many images of Low Surface Brightness Galaxies which have recently been discovered and analyzed. ... The central surface brightness of this galaxy is 24.28 . Malin 2 This galaxy is another huge disk galaxy with a scale length of 15 kpc and a redshift of 15000 km/a. The high surface brightness knot in one of its spiral arms actually has the same color, luminosity and H-alpha equivalent width as the entire Large Magellanic Cloud . ... Truly it is a Low Surface Brightness Galaxy. ...

Еще в разделе: (Показать все результаты (>403) - zebu.uoregon.edu/ )

• Orbital Properties of the Solar System
• Astronomy HyperText Book

... 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. ...

Еще в разделе: (Показать все результаты (>51) - sn.sai.msu.ru/ )

Еще в разделе: (Показать все результаты (>4) - aberrator.astronomy.net/ )

... Galaxies 99 Cosmic background with model of cloudy interstellar medium Yu. ... Figure 1: Averaged spectrum of the cosmic background I f in frequency range 0.25 200 MHz for the Galactic poles. ... First interpretation of the cosmic noise background spectrum at broad band frequency range 0.25 200 MHz with a model of the cloudy interstellar medium ISM is presented here. ... Synthesized background spectra I f for regions of the Galactic poles at the frequency range 0.25 200 MHz is presented in Fig. ...

Еще в разделе: (Показать все результаты (>318) - www.gao.spb.ru/ )

• Страница Е.В.Милецкого / Page of Eugen Miletsky
• RADIOSUN Workshop 2014
• The XIII Russian-Finnish Symposium on Radio Astronomy