Next: Star Formation Rate and Up: No Title Previous: Calculation of Evolutionary Tracks . To start calculations, we choose the distributions of the initial binary parameters: the mass of the primary ZAMS component, , binary mass ratio, , orbital separation a . ... whereas the mass ratio distribution is not. ... The zero assumption often made is that the mass ratio distribution has a flat shape, that is binaries with a high mass ratio occur as frequently as those with equal masses. ...

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• Dependence on the Scenario Parameters and Initial Distributions
• Initial binary parameters
• Parameters of binary compact star evolution

... The obtained results lead to the following conclusions: a) the heavy element enrichment had taken place in the Galaxy in a few bursts of its activity rether than in a continuons manner; b) these bursts occured during the callapse of the early Galaxy; c) the star formation had been inhibited in the time of the bursts; d) the metal enrichment did not proceed in the periods of star formation, between these bursts of activity. ...

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• Vladimir Marsakov Publication List
• Population of Galactic globular clusters, tabl

Next: Simulations Up: Maximum Likelihood Estimation of Previous: Introduction . The properties of an ensemble of faint galaxies can be defined by the distribution of the parameters of the models that best fit each individual object. ... The model also includes instrumental parameters, such as the sky background (estimated locally) and amplitude of the noise. ... The probability of the observed value is then computed for each pixel using the adopted error distribution. ...

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• Fundamental Parameters, Integrated Red Giant Branch Mass Loss, and Dust
• New Approach: Space Variant Hyperparameter
• Starburst99 - Simulation Parameters

... In brief: the frequency-dependent radiative transfer equation is solved for a dust under assumption of spherically-symmetric geometry for its distribution taking into account particle size distribution and quantum heating effects for the very small dust particles. ... Table: Model parameters for IRAS04296+3429. ... parameter . ... hot dust shell) . ... The best fit to the spectral energy distribution of IRAS04296 is shown by heavy solid line (see Table2 for details concerning parameters of the model...

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• Determination of atmospheric parameters and calculation of chemical composition
• harak_e

To construct two-dimension distribution of minor planets user should specify elements/ parameters/ function that will be plotted as abscissas and ordinates. In three-dimension case one should add to them the element plotted on Z axis. ... Though you may choose elements plotted along different axes at will, often there is good reason to plot such elements as a, n, or n" along X axis (two-dimension distributions) and to plot them along Y axis in three-dimension case. ...

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• ENGAMPLE

Next: Generation from Ground Calibration Up: EMOS_REDIST Previous: EMOS_REDIST Contents . The redistribution parameters for the MOS cameras. ... Attributes: . None. Columns: . ... The central CCD of each MOS detector has developed a patch where the energy resolution is worse than the average. ... The energy bounds of PHA channels. ... The energy bounds of the PI channels, used to determine the equivalent energies of spectral channels in the redistribution matrix construction. ...

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• Index
• Parameters

... A number of different statistical methods are used for estimating parameters from a data set. The most commonly used one is the least squares method which estimates a parameter by minimizing the function : . where y is the dependent and x the independent variables while f is a given function. ... The most important assumptions are that the errors in the dependent variable are normal distributed, the variance is homogeneous, and the independent variables have no errors and are uncorrelated. ...

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• Documentation: LEDA: parameter: vrot
• HyperLEDA documentation: parameter: vmaxg
• References

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... Quasi-stationary electron distributions for the different values of the particle escape time. ... The electron-cyclotron maser instability is widespread in the Universe, producing, e.g., radio emission of the magnetized planets and cool substellar objects. ... The model used takes into account the radiation escape from the source region and the particle flow through this region. ...

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• Galactic distribution and absolute magnitudes
• ffit help file
• C. Refereed Journal Publications 2001

... We demonstrate through numerical simulations that model parameters estimated with our technique are essentially bias-free, even when the average number of counts per bin is 1. ... The IW technique avoids such biases by estimating through successive iterations, where for each iteration, j, , and the best-fit parameters are determined by minimization of . ... In our sample, we find that the minimum values and best-fit parameters converge after about 6 iterations. ...

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• Recent Advances in Parameter Estimation in Astronomy with Poisson-Distributed
• Indexing and Searching Distributed Astronomical Data Archives
• The IUE Archive at Villafranca

... St Petersburg 23, September 2014 1 Motivation · Origin of Martian moons? ... Considered error sources: ­ Phobos a priori ephemerides; ­ Phobos a priori GM value; ­ measurements noise; ­ different strategies; · Methods: ­ real data analysis; ­ simulations. ... St Petersburg 23, September 2014 8 Simulations: sensitivity of the measurements to the a priori GM value Simulations: zero noise+ IMCCE a priori ephemerides +GMPH = 7.16 * 105 m3/sec2. ... St Petersburg 23, September 2014 14 Thank you! ...

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• http://www.gao.spb.ru/english/as/j2014/presentations/guseva.pdf
• Страница Е.В.Милецкого / Page of Eugen Miletsky

... 18-Jan-2010 17:22 . ... Apache/2.2.3 (CentOS) Server at www.wdcb.ru Port 80 ...

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• Index of /stp/data/Images_of_f-plots/TABL/Tables of different Parameters/f min
• Index of /stp/data/Images_of_f-plots/TABL/Tables of different Parameters/fo Es
• Index of /stp/data/Images_of_f-plots/TABL/Tables of different Parameters/M3000

Magellanic Clouds in interaction evolutionary search for good models Adam Rzicka1, Jan Palous1, Christian Theis2 1Astronomical Institute, Prague; 2Institut fЭr Astronomie, Wien Idea investigate the LMC-SMC-Milky Way (MW) interaction by modeling the distribution of HI related to the Magellanic System (BrЭns et al. ... How much does the HI distribution tell about the LMC/SMC motion? ... It's all about proper motion... select a high-quality model (FF 0.5) and look around Tidal models don't work.. ...

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• Input Parameters to the Self-Calibration Tasks
• Cosmological Parameter Survey Using the Gravitational Lensing Method
• casacore: casa::Weibull Class Reference

... Colours of stars and galaxies hold information on intrinsic and extrinsic parameters, such as stellar temperatures and galaxy populations, selective absorption and colour changes due different dust contents and inclination angles of galaxies, as well as galaxy redshifts and evolution. ... The colour magnitude diagram of 65000 galaxies to which all above-mentioned quantities and others contribute can only be explained by comparison with simulations. ... Colours are also of technical help. ...

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• Sample Properties
• FSRQs
• IAU Symp317 Scientific Program

http ://hea-www.harvard.edu/ AstroStat /slog/2008/eotw-chisq- distribution / Weaving together Astronomy+Statistics+Computer Science+Engineering+Intrumentation, far beyond the growing borders Fri, 01 Jun 2012 18:47:52 +0000 hourly 1 http ://wordpress.org/?v=3.4 http ://hea-www.harvard.edu/ AstroStat /slog/2008/eotw-chisq- distribution /comment-page-1/#comment-308 Alex Sun, 27 Jul 2008 01:52:08 +0000 http ://hea-www.harvard.edu/ ... Thanks, Aneta, very useful comment. ...

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• Parameters
• The AstroStat Slog Blog Archive tests of fit for the Poisson distribution
• The AstroStat Slog Blog Archive chi-square distribution [Eqn]

... FTP access the basic models is here . ... Below, we put short descriptions of the used SED models for the photometric redshifts providing by the current server . ... The uniqueness of this model consists in expanding to the near IR (NIR) of Rocca-Volmerange and Guiderdoni's (1988) atlas of synthetic spectra with a revised stellar library, which includes parameters of cool stars. ... Homepage of the GISSEL model). ... Another model used earlier is the model of synthetic spectra of Poggianti (1997). ...

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• Informational system "Evolution of RG"
• Radio Sources Parameters

... 05/09/2013 Galaxy Evolution over Five Decades - Cambridge 2013 Nuclear activity and environment Effect of environment on AGN is not completely clear yet. ... 05/09/2013 Galaxy Evolution over Five Decades - Cambridge 2013 Effect of the mass Mass slices ­ optical and radio AGN overall interaction one-on-one interaction relative location 05/09/2013 Galaxy Evolution over Five Decades - Cambridge 2013 Stratified study Stratifed study that considers several strata of mass. ...

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• http://www.mrao.cam.ac.uk/~bn204/mk2/publications/2005/IREvolvePasadenaConfPoster.pdf
• http://www.mrao.cam.ac.uk/~krause/Dogliani2003.pdf
• Bojan Nikolic -- Nested sampling modelling of Star-Formation History of the

... Fitting the observed dependence includes calculations of the polarization cross-sections averaged over particles orientation and size distribution, their normalization and the comparison of obtained dependencies with Serkowski's curve representing observational data for a chosen star. ... Variations of the polarization factors with wavelength are shown in Fig. 16 for homogeneous spheroidal particles with PF orientation. ... The distinction between prolate and oblate spheroids is also clearly seen. ...

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• Database of Optical Properties -- Level: subpage
• Database of Optical Properties -- Level: subsubpage
• Nebular Abundances For PNe of Different Central Star Masses

spaceweb@oulu.fi - last update: 1 July 1998, 1200 UT (RR) . ... Relates the wave number k to the wave frequency. ... From the equation of motion , m d v /dt = q( v x B ) one can calculate that, in a presence of magnetic field B , a charged particle is accelerated in direction perpendicular to both v (perp) and B . ... The angle a between magnetic field B and velocity vector of a charged particle, v ., i.e., sin a = v(perp) / v(total), where v(perp) refers to the velocity component perpendicular to B . ...

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• Dayside aurora [Oulu]
• ENERGETIC PARTICLE EXPERIMENT DOK-2
• List of currently available KP AZ.

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. ...

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• Cosmological Issues for Theorists
• Chapter 35
• Potential Energy

Atmospheric influence on the different radio-engineering system functioning . ESTIMATION OF ATMOSPHERIC OPTICAL CHARACTERISTICS AND REMOTELY SANSED IMAGE CORRECTION . ... Direct transmittance estimation results for 12 channels of the spectrometer CHRIS. ... We have managed to develop a direct method of estimating the discrete Normalized Atmospheric Point Spread Function (NAPSF) from available images alone, not using any external sources of information about the atmosphere. ... IRE RAS 1996-20 11 ...

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• Project 4 - RFBR - Stepantsov, Determination of the space anisotropy of order
• Getting Started in Actor Prolog. Oil Production.