... The models provided are: . abs - absorption of x-rays by neutral gas with solar abundances. parameter 1 = . ... parameter 2 = . ... normalization - logarithmic value of the flux density at 1 keV in units of keV cm -2 s -1 keV -1 . ... normalization - logarithmic value of the normalization of the gaussian in units of keV cm -2 s -1 . ... absorption ( params )* model ( params ) . ... A single value for the normalization (i.e., fixed normalization) will force the program to use that value. ...

... spectrum . ... nsource <n> : choice of source function (def: 3=Feautrier) . noptype <n> : choice of continuous opacity (def: 1=Kiel) . nhedat <nhedat> : choice of HeI data (BCS or Mon treal) (def: 1=BCS) . ... read_model <filename>: read model atmosphere in QUB/STERNE2 format . ... wavmax <w_max> : distance from line centre to compute . ... nvturb <n vt > : number of points in -dependent v turb . ... tau_exp <n> : increase resolution of optical depth scale by adding additional points . ...

... CentralProcessor 0.11 documentation . Calibration and Imaging Documentation . The cmodel pipeline task is responsible for extracting a local sky model (LSM) from the global sky model (GSM) and building an image from the components and/or images resulting from the request. ... MPI wrapper> cmodel -c config.in . ... None . ... If Cmodel.gsm.database is set to asciitable then a row/column (space separated) file is used as the global sky model source. ... cmodel (Model Image Generator) . ...

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. ...

... 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...

Next: Stellar models Up: Introduction Previous: Photometry Contents . In a hierarchical stellar system, the separation between two neighboring stars is always much smaller than the separation of this pair from the next companion in the system, be it another pair or a single star. ... They are also numerically easier to handle than non-hierarchical systems, since each pair can be described with the standard orbital parameters, and each star with a small number of physical parameters. ... System . ...

... 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. ...

Next: Initial binary parameters Up: Population synthesis of Previous: Introduction . Monte-Carlo method for statistical simulation of binary evolution was originally proposed by Kornilov & Lipunov (1983a,b) for massive binaries and developed later by Lipunov & Postnov (1987) for low-massive binaries. ... Recently Leitherer & Heckman (1995) have modelled star formation for elliptical and spiral galaxies, taking into consideration only the single stars. ... Initial binary parameters . ...

ON THE IMPACT OF THE GALACTIC ABERRATION ON VLBI-DERIVED PRECESSION MODEL Z.M. MALKIN Pulkovo Observatory Pulkovskoe Ch. ... Corrections to adopted precession rate are usually computed from the linear trends in long-term time series of celestial pole offset (CPO), which are the differences between the measured and the theoretical coordinates of the celestial pole. ... CONCLUSIONS We have estimated the impact of GA on parameters of precession-nutation model derived from VLBI observations. ...

Russian SHAREABLE DATA CENTER Institute of Solar-Terrestial Physics SB RAS . ... Although their determination is based on the scattering process model, independent check-ups by rocket experiments have shown their correctness in experimental applications. ... Ionospheric data analysis, especially during strong disturbances, cannot be without some other kinds of diagnostic tools. ... The lack of data has always been a challange in this case. ...

... Summary of the parameters handled by the user: . ... Edition of the Table Containing the Atomic Parameters . Edition of the Table Containing the Cloud Model . Computation of the Output Absorption Spectrum . ... Format of the table for atomic parameters (ABSP.TBL). Format of the table for the emission line model (EMI.TBL) . Format of the table for the absorption line model (ABSC.TBL) . ...

... Bojan Nikolic web pages home . ... As an exercise to put through the new InMin library through its paces, I have looked recently at applying Nested Sampling ( Skilling2006 ) algorithm to the fitting of star-formation history as function of redshift. ... The data I used are from Figure 1 of Yuksel08 but I use only the grey data paints, which are just the data originally from Hopkins2006 . ... The next step is to define the function which is the model for the history of the SFR density. ...

Previous page: Measuring temperatures and composition in the ionoshere . If the actual spectra that the radar measures from the ionosphere consisted of continuous smooth curves, and if it was necessary to measure only two quantities, say the width and the total power, then one could use a ruler and get pretty good answers. ... There is no simple way to get from the data points to the best answers, but one would say that one spectrum is much better than the other. ...

XMM-Newton Science Analysis System Page: 1 rgsbkgmodel July 2, 2008 Abstract Compute a model background spectrum from RGS background templates 1 Instruments/Modes Instrument Mode RGS Spectroscopy 2 Use In the interactive environment. pipeline processing no interactive analysis yes 3 Description The aim of this package is to compute a model spectrum of the RGS background applicable to a given observation from a combination of observations of empty elds. ... Model background spectra (OGIP-compliant). ...

polimodel -- Produce model linear polarization and position angle images . ... Whether to apply random errors to output polarization and position angle values. seed = "" [integer] . ... This task produces a model linear polarization image and corresponding position angle image from an input image assumed to represent intensity (Stokes I parameter). ... A threshold for the input image can be defined such that polarization and position angle are not computed for input values less than this threshold. ...

... The perceptron structure, on the basis of which the database is built, is defined by a number of the input and output parameters and a required accuracy. ... The output perceptron data are the expansion coefficients of the scattering matrix elements in series of the generalized spherical functions. ... As the cluster structure depends on the generation conditions the expansion coefficients were averaged over 5--7 realizations of the clusters (for N . ... is the coefficient number. ...

... Chapter 15. 15.0 Introduction Modeling of Data Given a set of observations, one often wants to condense and summarize the data by fitting it to a "model" that depends on adjustable parameters. Sometimes the model is simply a convenient class of functions, such as polynomials or Gaussians, and the fit supplies the appropriate coefficients. ... The parameters of the model are then adjusted to achieve a minimum in the merit function, yielding best-fit parameters. ... Data are generally not exact. ...

... We find a transition of LBV star from the LBV instability strip to the region of classical WN for the first time. ... Numerical modeling of the atmospheres of these objects are very important for understanding the evolutionary relationship WR and LBV stars, as well as of the physical causes of LBVs variability. We studied spectra of two very luminous stars in the M33 galaxy - LBV V532 and late WN star FSZ35. ... Bottom: The spectrum of FSZ35 with the final model . ...

The Earth's magnetosphere global structure is conditioned by the interaction of the Solar wind and Earth's magnetic field. ... Many various magnetospheric models are available in the NSSDC . ... Fairfield D. H., Average and unusual location of the Earth's magnetopause and bow shock, J. Geophys. ... Stasiewicz K., Polar Cusp Topology and Position as a Function of Interplanetary Magnetic Field and Magnetic Activity: Comparison of a Model with Viking and other Observations, J. Geophys. ...

. 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.