... If you elect to model the sky, you will see some graphs showing the progress of the fitting procedure. First, if some bright stars were observed, you see a plot of sky data (for a given band and night) as a function of the adjacent star's brightness. ... Second, if there are enough dark-sky data to model, you will see a plot of the dark-sky data (corrected for star light) as a function of airmass, with the fitted term drawn in as + signs. ... Again, the fit is shown with + signs. ...

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• Edition of the Table Containing the Cloud Model
• Inter-stellar/galactic Absorption Line Modelling
• Extinction and transformation models

... 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. ...

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• Structure of the Spectral Package
• Spectral Analysis
• The AstroStat Slog Blog Archive [ArXiv] Post Model Selection, Nov. 7, 2007

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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• GHRS Data Handbook
• Models
• Subtracting models from unsaturated WFPC2 PSFs

... 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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• Flux density bootstrapping
• Input Parameters to the Self-Calibration Tasks
• selfcal

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
• http://selena.sai.msu.ru/Symposium/ir_luna_e.pdf

... SFIT is a general-purpose code designed to optimize theoretical stellar spectra to an observed spectrum. ... While the programme expects input from "stdio", it is more natural to save commands in a file (eg "sfit_input") and run the code simply by . ... If the spectra to be fitted have a filename "star_spectrum", then the best fit spectrum will be written out, together with the renormalized input spectrum, to a file called "star_spectrum.fit". ... sets up model spectrum grid (and for 2nd star) . ...

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• ffit help file
• SCL Sfit SLV Commands
• Sfit Control Language: Classified Listing

... 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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• Fitting and Modeling in the ASC Data Analysis Environment
• ETCs and Observations Simulation at the VLT
• Modeling Scattered Light in the HST Faint Object Spectrograph

... Bojan Nikolic web pages (r. 329) . ... Since version 0.12, libAIR comes with a simple command line interface to the routines which retrieve the water vapour and the phase correction coefficient. Currently only the very simplest model is supported, in which the all of pressure, temperature and water vapour column are free parameters, and they are inferred from the four observed water vapour radiometer readings. ... Command line interface to libAIR and water vapour column retrieval . ...

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• Bojan Nikolic -- Nested sampling modelling of Star-Formation History of the
• Inference of Coefficients for Use in Phase Correction Bojan Nikolic web pages
• An expanding plasmon model for the radio outbursts of Cir X-1

. 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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• Catalogue 5 of WDC-B

... Abstract: We present Monte Carlo radiative transfer simulations for spiral galaxies modelled as a stellar disk and a two-phase clumpy dust distribution. ... As a general result, clumpy models are less opaque than the corresponding homogeneous models. ... 0.00 0.15 0.50 0.1 0.5 1.0 2.0 5.0 10.0 0.25 X . ... We have also produced several homogeneous models, to compare to the clumpy models. ... Homogeneous and clumpy models with the same tauV have the same dust mass. ...

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• Atlas of Monte Carlo Models of Dust Extinction in Galaxies
• A Hubble diagram for Quasars
• CHIANTI atomic database

... Lightcurves of two satellites of Saturn, namely Hyperion (S7) and Phoebe (S9), were modeled using algorithms and programs developed for calculat­ ing the rotational dynamics and constructing theoretical lightcurves of planetary satellites. ... The problem of fitting an observed lightcurve with the model one is solved by varying the initial data and values of the parameters of the problem. ... The value of the MLCE calculated for the deduced initial data and values of the parameters is close to zero....

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• http://www.ipa.nw.ru/conference/2002/sovet/PS/CHERNE.PS
• http://www.ipa.nw.ru/conference/2002/sovet/PS/GAYAZOV.PS
• LAB Ephem. Astronomy-ERA

... CI ) - Cm (I )) ( = 2 (I) N 2 2 PKS0558-504 simultaneous fitting The Chi-Squared is the most common statistic in use to fit a function f to data {x, y} : = 2 N ( yi - f ( xi )) 2 2 i N = number of data points i2 = variance (related to the measurement error for yi ) y = independet variable x = dependet variable f = assumed relationship between x and y yi = observed mean f(x i ) = predicted mean Statistical concepts relevant to data ... 2 * < 1 { (I) OVERESTIMATED} BAD FITTING!! ...

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• http://xmm.vilspa.esa.es/sas/6.1.0/doc/epatplot/ChangeLog
• http://xmm.vilspa.esa.es/sas/7.0.0/doc/epatplot/ChangeLog
• http://xmm.vilspa.esa.es/sas/7.1.0/doc/epatplot/ChangeLog

... Begin by reading an already prepared model file for 1997-05-01. readmodel,'1997-05-01.model' . ... This model has already best-fit parameter values set, but feel free to change them. ... Click on "Fit" in the (large) model fit widget. ... After this fit completes, click on "A-B" in the model fit widget to obtain the following listing of the parameters of the binary component. ... COMPONENT=A-B . ... SEMIMAJORAXIS= 9.8400002 +/- 0.0000000 . ... APSIDALMOTION= 0.0000000 +/- 0.0000000 . ...

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• The Hierarchical Stellar Systems Model Format
• Manipulation of a model
• Stellar models

Next: Initial parameters of compact Up: The Model Previous: The Model . To start the calculations, we choose the distributions of initial binary parameters: mass of the primary ZAMS component, ; binary mass ratio, ; and orbital separation, a . ... As for the mass ratio distribution in binaries, the observational information is poor. Meanwhile, from the evolutionary point of view, it is particularly important how different are the initial masses of the components (see, e.g., Trimble 1983). ...

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• Structure of the Galaxy
• Conclusions
• The Model

Decomposition of Galaxy Images and Galaxy Rotation Curves Mosenkov A.V.*^, Savchenko S.S.*, Sotnikova N.Ya.* ... The DECA (DEComposition Analysis) code is designed to investigate images of galaxies in an automatic regime (using the simple 'bulge+disc' model) as well as in manual mode for more detailed images and/or for multicomponent structures. ... The GRCF package was created for performing the galaxies rotation curve decomposition using the models of the bulge, the disc, and the dark halo. ...

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• http://www.gao.spb.ru/english/as/j2014/presentations/suvorkin.pdf
• http://www.gao.spb.ru/english/as/j2014/presentations/perepelkin.pdf
• http://www.gao.spb.ru/english/personal/malkin/publ/zm12e.pdf

... 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 . ...

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• Measurement of the dark halo shape in polar ring galaxies
• Lack of Dwarf Galaxies in the Local Volume Compared to Conventional Cosmology
• The dust jets in the nucleus of comet 29P/Schwassmann-Wachmann 1

... Towards a Truly Unified Model of AGN . ... The Unified Model holds that the aspect-dependent effects primarily determine the nature of the active galactic nucleus that we observe. ... The full postscript file can be obtained here: . The PASA Latex file can be obtained here: . The postscript file of Fig 1 can be obtained here: . ...

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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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• East Siberian Center for the Earth's Ionosphere Research. SW radiosignal
• East Siberian Center for the Earth's Ionosphere Research. VS data on-line
• East Siberian Center for the Earth's Ionosphere Research. Ionospheric parameter

Note: These models for T-receiver are based on measurements for all of the 14 pipelines. download Trx polynomial fit parameters . ... any additional offset to be addded as a correction not incorporated in the model (e.g. the contribution to receiver temperature from beyond the pre-amplifier stages), . ... No. of coefficient pairs, n_harm, associated with the harmonic (Cos & Sin) part of the fit (where the final fit is a simple sum of the two parts).. ... cos(j*pi*X/2) & sin(j*pi*X/2), . ...

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• modelAerostatPeriods
• Modeling the Spectrum
• REU Science Area

... We cannot use for this purpose equivalent widths and profiles of HI lines (well known criteria of atmospheric conditions for normal supergiants), since these lines are strongly distorted in the spectrum of IRAS04296 as seen in Fig. ... Figure: Upper: iron abundance FeI (circles) and FeII (crosses) calculated for IRAS04296+3429 with model parameters , and using lines with different excitation potentials EP of a low level; bottom: the same as a function of the equivalent width W . ...

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• Spectral energy distribution
• Publications of Klochkova Valentina
• Search for distant radio galaxies in SAO