... Calculations of at least two runs with different values of a parameter are required in order to discover to what extent the results depend on the , if at all. ... In order to study how the final statistical distributions depend on the initial functions, the method of Green functions is used. ... Then we can restore any distribution on this parameter (with a certain accuracy) by summing the results for each interval with the appropriate weight. ...

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• Initial Distributions of Binary Parameters
• Initial binary parameters
• Parameters of binary compact star evolution

Russian SHAREABLE DATA CENTER Institute of Solar-Terrestial Physics SB RAS . ... Investigations of the ionospheric response to strong magnetics storms which are usual for our latitudes, are of great interest. ... In the figure, we present ionospheric parameter dynamics during three perturbed days in July 2000. ...

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• East Siberian Center for the Earth's Ionosphere Research. Modelling, secondary
• East Siberian Center for the Earth's Ionosphere Research. Capabilities and
• East Siberian Center for the Earth's Ionosphere Research. Specific character

... 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

... 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

... A list of spectrum files from a set of observations, referring to one RGS instrument and one spectral order. These spectra files must be produced using the attstyle=user and associated parameters from a call to rgsproc . ... A list of accompanying event list files, in the same order as the spectra files. ... If this parameter is set to yes, the spectra files of the input lists will be combined to produced a combined spectrum file each for both spectra and background spectra files. filermf . ...

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... ATNF Home . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Parkes radio telescope . ... Parkes | ... Australia Telescope 20GHz Survey . ... Visiting Parkes radio telescope . ... Parkes radio telescope webcam . ... Additionally, they provide insight into the gravitational lensing process and its complex relationship with the various cosmological parameters. Keywords: cosmology: large-scale structure - gravitational lensing . ... The Elements of Gravitational Lensing . ...

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• casacore: casa::Weibull Class Reference
• casacore: casa::Poisson Class Reference
• Pulsar Group Main/Psrfits

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
• MultiDrizzle parameter tables
• CCD Parameters table

... Nonparametric density estimation drops these restrictions 8 Nonparametric Density Estimation 12 density 0 0.0 2 4 6 8 10 0.1 0.2 0.3 redshift 0.4 0.5 Histogram of 1,425 galaxy redshifts. 9 Nonparametric Density Estimation 12 density 0 0.0 2 4 6 8 10 0.1 0.2 0.3 redshift 0.4 0.5 Compared with best fitting gamma distribution. ... 13 Nonparametric Density Estimation 12 density 0 0.0 2 4 6 8 10 0.1 0.2 0.3 redshift 0.4 0.5 Parametric versus nonparametric estimate (kernel density estimate). ...

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• The AstroStat Slog distribution
• The AstroStat Slog Blog Archive chi-square distribution [Eqn]
• Comments on: chi-square distribution [Eqn] By: Alex By: vlk By: aneta By: aneta

. This Directory contains Model of distribution of density, temperature and effective collision freguency of electrons. Yu.K.Chasovitin. 1998. This Directory contains The program RIM98 for calculating the parameters of the ionosphere to use the "Reference Ionospheric Model-98" (RIM-98).Yu.K.Chasovitin. 1998.

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• "STP Data" STP Data
• Index of /stp/data/Images_of_f-plots/TABL/Tables of different Parameters/M3000
• Index of /stp/data/Images_of_f-plots/TABL/Tables of different Parameters/fo E

... Fit Teff, theta and E(B-V) to IUE spectrum and uvby photometry using a grid of helium-rich model flux distributions. models{ . ... simon/models/01980001/19325he90L.s . simon/models/01980001/20325he90L.s . simon/models/01980001/21325he90L.s . simon/models/01980001/22325he90L.s . simon/models/01980001/23325he90L.s . simon/models/01980001/24325he90L.s . simon/models/01980001/25325he90L.s . simon/models/01980001/26325he90L.s . ... IUE data file in "spectrum format 2" . ...

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• Armagh Observatory
• lte-codes: sterne model atmospheres
• Refereed Journal Publications 2004

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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• Preparation of parameter file
• Stellar models
• DFS Department internal procedure for issue of documentation

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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• Keywords_262
• ENGAMPLE

... Future seminars . P a s t seminars . Seminar council . The emission time of Gamma-Ray Bursts" . A. Sanin (IKI) . ... The three new parameters of cosmic gamma-ray bursts are introduced: the emission time, the peak energy of the emission time spectrum and the cosmological invariant parameter. ... Using this distribution the "collective estimation" of the best fitting redshifts for the group of long bright gamma-ray bursts detected by BATSE experiment was found. ...

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• PLASMA EXPERIMENTS ON TAIL PROBE
• ENERGETIC PARTICLES EXPERIMENTS ON TAIL PROBE
• INTERBALL Auroral Results Page

... 3D structure rings , spots filaments · Application to Cygnus A and 3C 317 Radio cocoon and shaped Xray gas (contours) in Cygnus A Cygnus A (Chandra archive, courtesy P. Strub) large cocoon width elliptically shaped cluster gas marks bow shock axis ratio: 1.2 Outline · · · ­ Pretty data: Cygnus A Parameters of jet simulations in the history Extension to very low ... L g[ = -2 ] Parameter Study: Axis Ratio Small jets have spherical bow shocks! critical radius depends on . ...

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• DUST: dustiface.h File Reference
• B Bayesian value for
• Astrophysics Group MADCOW

... 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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• Corrections to the probability distribution
• EXAMINE/ROMAFOT
• The main observational parameters

... 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
• Бобылев Вадим Вадимович

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. ...

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• Introduction to Plasma Physics
• ION AND ELECTRON ENERGY DETECTOR PAN-2
• Optical static Fourier spectrometer

... 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
• Астрономия в Санкт-Петербургском университете |

Preliminary results of astroclimate parameters measurements at the Sternberg 2.5m telescope installation site V.Kornilov, N.Shatsky, S.Potanin, O.Voziakova, B.Safonov Moscow, 2008 Acknowledgements A.Belinskiy M.Kornilov A.Tokovinin M.Kuznetsov P.Kortunov E.Gorbovskoy SAI administration some SAI students Pulkovo solar station (KHSS) staff RFBR support MAVEG Gmbh Why to study optical turbulence and some other relevant ... Mean seeing by DIMM data for this night is 1''5. ...

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ENERGETIC PARTICLE EXPERIMENT DOK-2 . ... Due to much higher energy, angular and time resolution, better separation of electrons and ions it is expected that DOK-2 experiment will allow to re-examine in more details energetic particle population and related processes in magnetosphere regions covered by the spacecraft orbit. ... Thin foil in front of detector absorbes protons with energies E<400 keV so this detector measures electron spectrum in 20 - 420 keV range. ... Energy values, keV . ...

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• List of currently available KP AZ.
• THE LOW ENERGY PLASMA COMPOSITION EXPERIMENT AMEI-2
• Basic definitions [Oulu]