Scale-heights of the Galactic disk subsytems with different ages and metallicities . V.Marsakov & Yu. ... It is based on the fact, that all stars cross the disk plane several times during their Galactic orbital period. ... We have used our representative sample of nearby disk F2-G2 stars Marsakov & Shevelev (1995) in which fundamental stellar parameters was determined on the basis of published date on uvby-photometry, proper motion and radial velocities. ... Marsakov V.A., Shevelev Yu.G. Bull. ...

... Briefly, the count rate at the detector from a source at a redshift z is . ... Another possible way that could lead to arising diverse peculiarities in the - distribution induced by the sources evolution is connected with a possible non-monotonic character of the star formation rate in galaxies. ... The most prominent feature of the obtained theoretical - is a notable sharp increase at low count rates due to evolutionary effects. ...

... 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. ...

... 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...

... 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. ...

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. ...

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. ...

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. ...

... 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 . ...

... 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. ...

... 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. ...

. 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.

... 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! ...

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. ...

... CentralProcessor 0.11 documentation . ... It can be run with the following command, where ?config.in? is a file containing the configuration parameters described in the next section. ... Parset parameters understood by ccontsubtract are given in the following table (all parameters must have CContSubtract prefix, i.e. CContSubtract.dataset ). ... A number of other parameters allowing the user to narrow down the data selection are understood. ... Parameter . ... Data set file name to work with. ...

... dust_AbsXSec . Absorption Cross section. typedef void . ... Calculates the equilibrium temperature given the absorption cross section and a radiation field. double . ... Calculates the absortion cross section of a species/size of dust grain . ... The grain absorption cross section . ... The absorption cross section of the grain . ... Calculates the equilibrium emission at wavelength lambda from a (large) grain at temperature T and with absorption cross section xsection. double dust_EquiT . ...

... 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). ...

... It is found that the correlation coefficients between these two parameters calculated separately inside and outside the sunspot formation zone ±30 have cyclic variation and occur in anti-phase. This suggests different mechanisms of formation of the corona in the fields of small, medium, and large scales. ... The relationship between the coronal green line brightness (CGLB) and the magnetic field strength (MFS) has been investigated by constructing the corresponding synoptic maps for the 1977-2001. ...

... 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. ...

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 . ...