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http://www.stsci.edu/stsci/meetings/irw/proceedings/ratnatungak.dir/section3_3.html.

1. File Formats Required for Photometry
... Observatory data . ... Required stellar data . ... Comment column . ... UT date --- column label: DATE . MJD --- column label: MJD_OBS . ... Column label: TELESCOP . Column label: DIAM . Column label: LON . Column label: LAT . Column label: HEIGHT . ... Descriptor for the ``horizon'' table . ... Instrument configuration and run-specific information . Storage format . ... Column DET . ... Sample instrument files . ... CCD photometry . ... Required observational data . ...
[ Сохраненная копия ]  Ссылки http://www.sao.ru/precise/Midas_doc/doc/94NOV/vol2/node548.html -- 12.5 Кб -- 23.02.1996
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2. Model Fitting
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. ...
[ Сохраненная копия ]  Ссылки http://www.stsci.edu/stsci/meetings/irw/proceedings/ratnatungak.dir/section3_2.html -- 6.3 Кб -- 18.04.1994
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3. Dependence on the Scenario Parameters and Initial Distributions
... 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. ...
[ Сохраненная копия ]  Ссылки http://xray.sai.msu.ru/~mystery/articles/review/node35.html -- 4.5 Кб -- 22.02.1997
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4. Making a Fake Observation
... The Miriad task uvgen can be used to simulate a variety of observing modes. ... Simulating a telescope approximately, let alone in some detail, requires a good many parameters. uvgen takes an appreciable number of parameters and input files to describe the telescope, correlator and source. Fortunately keyword and set-up files for some common situations exist ( e.g. simulating the ATCA and VLA). ... For example, to load typical parameters for the ATCA, use miriad% source $MIRCAT/uvgen.def.atca . ...
[ Сохраненная копия ]  Ссылки http://www.atnf.csiro.au/computing/software/miriad/userguide/node56.html -- 12.7 Кб -- 10.04.2016
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5. Parameters
... Meta Index / Home Page This section documents the parameters recognized by this task (if any). ... Default . ... dataset . ... Name of the FITS file containing the time series. ... boolean . ... The name of a new output file if required. ... Name of the output FITS file. screen . ... Name of the FITS file containing the GTIs. ... Do you want to perform the Kolmogorov-Smirnov test? . ... Do you want to carry out a chi-squared (Pearsons) test? . ... Do you want to carry out a flare test? . ...
[ Сохраненная копия ]  Ссылки http://xmm.vilspa.esa.es/sas/7.1.0/doc/ekstest/node5.html -- 8.0 Кб -- 08.07.2007
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6. Bias-Free Parameter Estimation with Few Counts, by Iterative Chi-Squared
... 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. ...
[ Сохраненная копия ]  Ссылки http://www.adass.org/adass/proceedings/adass94/kearnsk.html -- 12.3 Кб -- 03.11.2000
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7. Fit a source with a small number of net counts
Next: Inspection of results Up: *fit* - Fit Data Previous: Verbose Mode . If the number of net counts for a source is less than it is impractical to fit the data in all 34 energy bits. However, if the flux is required, then a fit must be performed first. ... Fit will then calculate the normalization of the model and xflux can be used to determine the flux and luminosity of the source from the best fit model. xs> fit rebin=yes . ...
[ Сохраненная копия ]  Ссылки http://hea-www.harvard.edu/PROS/PUG/node153.html -- 3.9 Кб -- 01.10.2012
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8. COALA - Wolfgang Kerzendor
... Exploring the physics of Type Ia supernovae through spectral analysis . ... Their progenitor scenario as well as the details of the explosion mechanism remain a mystery. ... It produces a supernova spectrum for a given luminosity, photospheric velocity, time since explosion and several elemental abundances. Tweaking these parameters to produce a spectrum that fits an observed spectrum is a complex, as of yet, manual task. ... The search space is large and complex. ...
[ Сохраненная копия ]  Ссылки http://www.mso.anu.edu.au/coala/wolfgang.html -- 4.1 Кб -- 01.10.2012
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9. Stellarium: SphereParams Struct Reference
... SphereParams Struct Reference . ... SphereParams (const float radius) . ... Definition at line 50 of file StelGeometryBuilder.hpp . ... Definition at line 103 of file StelGeometryBuilder.hpp . ... Definition at line 120 of file StelGeometryBuilder.hpp . ... Definition at line 112 of file StelGeometryBuilder.hpp . ... Definition at line 118 of file StelGeometryBuilder.hpp . ... Definition at line 110 of file StelGeometryBuilder.hpp . ... Definition at line 114 of file StelGeometryBuilder.hpp . ...
[ Сохраненная копия ]  Ссылки http://astro.uni-altai.ru/~aw/stellarium/api/structSphereParams.html -- 23.3 Кб -- 28.02.2014
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