... HST . ... Lensing Models . ... In order to interpret many of the properties of background lensed galaxies, reliable models of the lensing maps for each cluster are required. Preliminary models for each of the six Frontier Fields clusters have been provided by five independent groups prior to the HST Frontier Fields observing campaign in order to facilitate rapid analysis of the FF data by all members of the community. ... The various groups model the cluster mass distribution in different ways. ...

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• Fundamental Parameters, Integrated Red Giant Branch Mass Loss, and Dust
• Model Fitting
• Simulation Parameters

... Previous: Image Processing of Digitized Spectral Data . ... The analysis of sequences of light curves spanning a long time interval (at least one or two decades) allows us to detect activity cycles, analogous to the solar 11-year cycle, inferring the overall properties of the stellar dynamos. ... Our parallel procedure was written in standard FORTRAN using the PVM library version 3 and exploits a networked system to perform the analysis of a sequence of N L light curves. ...

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• Spatial Structure of NGC 6822: An Example for Statistical Modeling of
• A New Entropy Measure Based on Multiple Resolution and Noise Modeling
• Fitting and Modeling in the ASC Data Analysis Environment

... 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) . ...

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• Multi-Plane Models
• Input Parameters to the Self-Calibration Tasks
• Modifying Images by Models

. Documents latest versions (PS and Latex)

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• Model Spectra for Spectral-Fitting Program
• The AstroStat Slog Blog Archive A Quote on Model
• Jonathan's ASC/SDS documents

... The most powerful and widely used methods to calculate the scattering matrix of a fractal cluster are based on the coupled dipoles methods (e.g. the Discrete Dipole Approximation, DDA) and the theory of light scattering by a cluster of spherical particles [2-4]. ... At present the procedure of calculation of the scattering matrix is well developed for both an oriented cluster of spherical particles and for chaotically oriented clusters of such particles [4]. ...

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• Model realization and some results
• Neural network approach
• Introduction

Astronomical Data Analysis Software and Systems VII ASP Conference Series, Vol. ... A Parallel Procedure for the Analysis of Long­term Sequences of Light Curves A. F. Lanza, M. Rodon‘o 1 , U. Becciani and V. Antonuccio Delogu Osservatorio Astrofisico di Catania, Viale A. Doria, 6 ­ I 95125 Catania, Italy Abstract. ... 1995, Lanza et al. ... The minimization of the function Q for all the light curves of a given se­ quence, for fixed values of the system parameters, represents a cycle of the procedure. ...

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• http://www.stecf.org/conferences/adass/adassVII/reprints/does.ps.gz
• POLIMODEL (V1.00) --- April99 --- POLIMODEL (V1.00)

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. ...

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... To determine the parameters we want (stellar magnitudes and colors) from the observations we have, we fit the data to a model. The model should represent the circumstances of the observations as realistically as possible; otherwise, effects present in the data but not in the model will be distributed among the available adjustable parameters, such as stellar magnitudes, extinction coefficients, and transformation parameters. ... The bias problem . ...

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• Parameter estimation
• Fourier analysis: The sine model
• Using the sky model

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 . ...

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• Initial parameters of compact stars
• Initial binary parameters
• Conclusions

... THE SIMPLEST MODEL. ... 13, Moscow 119992, Russia E-mail: san@sai.msu.ru Abstract: The analysis of the simplest model shows that an asteroid ­ rubble pile evolves, depending on the parameter V2d (where V is the average velocity of fragments and d is the average distance between fragments), either as a conglomerate of "independent mutually gravitating clusters" (when V2d < fm, where f is the gravitational constant and m is the average mass of a fragment) or as a "receding cluster" (when V2d > fm). ...

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• http://selena.sai.msu.ru/Pug/Publications/ms42/m42_60.pdf
• http://selena.sai.msu.ru/Pug/Publications/m44_70_pugacheva.pdf
• Svetlana G. Pugacheva

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 . ...

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• ESO - Thesis Topic: Dynamical models of multiple globular cluster populations
• POLIMODEL (V2.00) --- November00 --- POLIMODEL (V2.00)
• Manipulation of a model