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

... 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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• Polarization properties (transmitted radiation)
• Extinction properties (transmitted radiation)
• Database of Optical Properties -- Level: subpage

... 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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• Basic principles of time series analysis
• Time series analysis in the frequency domain
• Signal detection

... 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
• Introduction
• Absorption bands identified with DIBs

... CentralProcessor 0.11 documentation . ... The Central Processor Manager is the local monitoring and control agent for the Central Processor sub-system. ... At the moment the Central Processor Manager only controls the acquisition phase; that is, it only controls the ingest pipeline. ... In addition to the CP manager specific parameters, any parameters that begin with ice_properties are passed directly to the ICE Communicator during initialisation. ... string . ... Central Processor Manager . ...

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• Determining Gains and Polarimetric Properties - GPCAL
• ccontsubtract CentralProcessor 0.11 documentation
• cmodel (Model Image Generator) CentralProcessor 0.11 documentation

... The distribution of redshifts among the DXRBS FSRQs identified so far (Figure 3) is quite similar to that of the 1 Jy and S4 samples. ... A more thorough comparison will have to await completion of our survey and the convolution of the redshift distribution with the WGACAT sky coverage. As has already been mentioned by Hook et al. (1996), selecting flat-spectrum sources is an efficient way of finding high-redshift, radio-loud quasars. ...

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• Previously Identified Sources
• Introduction
• FSRQs

... 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
• Generalized Spherical Harmonics for All-Sky Polarization Studies
• Modern CCD Observations of Moving Celestial Objects: Algorithms and Software

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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• Ionization and Thermal Structures of the Absorption-Line Systems of Quasars
• Scattering Properties of the Dust in the Reflection Nebula IC 435
• Ultraviolet Extinction Properties in the Milky Way

. Next: Spectrum Up: R Coronae Borealis Stars Previous: Historical Background . Figure 1: 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 is shown in Figure 1 . Spectrum . Galactic distribution and absolute magnitudes . Numbers and distances . Simon Jeffery . 2000-03-16

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• BASIC PROPERTIES
• STELLAR PROPERTIES
• Spectrum

... A file upload element on an HTML form. ... JavaScript 1.1: added type property . ... The HTML INPUT tag, with "file" as the value of the TYPE attribute. For a given form, the JavaScript runtime engine creates appropriate FileUpload objects and puts these objects in the elements array of the corresponding Form object. ... form . ... For all FileUpload objects, the value of the type property is "file" . ... Use the value property to obtain the file name that the user typed into a FileUpload object. ...

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• http://www.arcetri.astro.it/irlab/doc/library/javascript/clientreference/boolean.htm
• http://www.arcetri.astro.it/irlab/doc/library/javascript/clientreference/javarray.htm
• http://www.arcetri.astro.it/irlab/doc/library/javascript/clientreference/history.htm

... Bojan Nikolic web pages (r. 329) . ... Analysis of (radio) spectra . I describe an approach to fitting and comparison of radio spectra based on Bayesian analysis and realised using a new implementation of the nested sampling algorithm. ... I this paper I cover the theoretical background, the algorithms used and the implementation details of the computer code. I also briefly illustrate the method with some previously published data for three near-by galaxies. ... Paper I: Method . ...

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• Inference of Coefficients for Use in Phase Correction Bojan Nikolic web pages
• casata: CASA Tools for Analysis Bojan Nikolic web pages (r. 329)
• Analysis of surface error distributions through Moon (or Sun) beam cuts Bojan

THE PARAMETERS INVOLVED IN HAPKE'S MODEL FOR ESTIMATION OF THE COMPOSITION OF THE EJECTA LUNAR TERRAINS. ... In the previous papers we were estimated the surface roughness of the ejecta lunar terrains by means comparison of the local phase function and the average integrated lunar indicatrix. ... The Hapke's theoretical model of the lunar surface reflection. ... For THE PARAMETERS INVOLVED IN HAPKE'S MODEL: S.G. Pugacheva, V.V. Shevchenko a low-albedo lunar surface parameter Bo = 1. ...

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• http://selena.sai.msu.ru/Pug/Publications/m44_70_pugacheva.pdf

... The x-ray spectral analysis consists of a comparison between the observed pulse height spectrum and a pulse height spectrum calculated using a given spectral model. ... To obtain the spectral parameters for an x-ray source, several steps need to be followed. For each source: . ... obtain the best fit parameters for a spectral model - repeated for each model of interest . obtain a 1-D or 2-D grid of values around the best fit values - this can be done for as many models as desired . ...

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• Model Spectra for Spectral-Fitting Program
• Structure of the Spectral Package
• *search_grid* - Grid of - default mode

... badpixfind searches for pixels identified as containing no useful data, and uses this information to produce an output file. ... A bad pixel map (or mask) can also be produced. An important point regarding the bad pixels is that there are essentially three separate (though not exclusive) sets of bad pixels that must be dealt with. ... The user is able to specify maximum and minimum allowed values (via the parameters lothresh and hithresh ) to screen for hot and dead pixels. ...

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• Input
• Procedure

... The Radon transform (also known as the Hough transform) is formulated as a family of line integrals through a two-dimensional function. ... The Radon transform provides us with a simple means of computing the FF plane of the autochirplet transform, by using the Wigner distribution, and arriving at a transform space that tells us basically the same information as the chirplet FF-plane, except that we benefit from the greater resolution of the Wigner distribution. ...

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• Gaussian Chirplet Transform (GCT)
• Appendix D: The grammar of CSS2
• RELATED WORK

Download Izmccd (~2.7 MB). Solution of problems at identification of star field. ... 2) Scale is not correct. ... In this case algorithm of identification will revise all values of scale from twice smaller up to twice greater. ... There should be more than value of the field "Number of stars in frame". ... The star field is considered identified if number of the identified stars more or equally to this value. It is necessary to set value from 4 up to value of field "Number of stars in frame". ...

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... Публикации и издания Публикации профессорско-преподавательского состава СГАУ Издания проф. Сосниной Т.Н. Biosphere: Analysis of Value Parameters . ... Besides, the ways of saving the use value and value properties of biosphere are analyzed. The expediency of transformation of two-criterion theory of value into the three- criterion theory of the balance of value, where the ecologic component performs the function of the key criterion has been founded. ... BIOSPHERE USE VALUE OF THE PRODUCT: MAIN . ...

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... In this talk, I will discuss a study of the effect of ionization on the low end of HI mass function. The existence of a large population of low mass galaxies follows from CDM theory. ... HIDEEP found no low HI column density galaxies. One possible explanation is that the disks are "frozen". ... We assume that galaxies are exposed to an ionizing background radiation, from a uniform quasar distribution. ... We find a gap in the average column densities around N H which drops to 10 17 cm -2 . ...

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• HISA Poster for the 197th Meeting of the AAS, January, 2001
• The Search for HVCs in Other Galaxies

Next: The Evolution of Stars Up: NICMOS Science Previous: A Coronagraphic Search for . ... The NICMOS Parallel program . ... The Stellar Population . ... NICMOS Camera 3 is being used in parallel mode to observe galactic fields at both high and low galactic latitudes. ... Most of the fields are at high galactic latitude; as Figure 1 shows, only 8 pointings are within |b| = 10 o , i.e. the galactic disk. Figure 1: NICMOS parallel fields distribution in galactic latitude. ... Figure 6 ). ...

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• NICMOS Data Calibration and Analysis
• Introduction
• NICMOS Observes the Galactic Center

... 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/skurikhina.pdf
• Страница Е.В.Милецкого / Page of Eugen Miletsky
• Pulkovo NEO Page: Ephemeris Support