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. ...

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The summary plot shows the monthly time distribution of all predicted magnetic conjugations between four spacecraft considered. ... To show the time of conjugation, in frame of the corresponding day for each SC the corresponding colour and line are used: . for the first SC the red color and the first line are used, . ... On the plot the SC names are shown by the corresponding colours. The summary plot permit to find the simultaneous magnetic conjugations of 3 and even 4 satellites. ...

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• The plot of the magnetic conjugation's time distribution
• Nonequilibrium distributions

... Distribution of orbital elements for the RR Lyrae stars. Results for stars with [Fe/H ] > -0.95 (left column), [Fe/H ] < 0.95 and V res < 290 km/s (middle column), and [Fe/H] < -0.95 and V res > 290 km/s (right column) are shown separately. In the top row, we have plotted normal curves fitting the distributions. ... next figure | privious figure . ...

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• Population of Galactic globular clusters, figures
• Subsystems of the Galactic halo, figures
• Vertical Structure, figures

Next: Structure of the Galaxy Up: Model of the Galaxy Previous: Model of the Galaxy . As discussed above (Section  6 ), galactic binary systems are assumed to be distributed logarithmically along their semi-major axis A (Abt and Levy, 1976[ 2 ]), . ... Figure 40: Number of binary stars per frequency decade. ... As the observed distribution of binary periods is flat (equation ( 15.3.1 )), the normalization constant is the total number of galactic binaries per frequency decade: . ...

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• Initial Distributions of Binary Parameters
• Results of calculations
• Test of the Initial Mass-Ratio Distribution

... One of the most widely used tools of Fourier analysis is the Parseval theorem. It enables the experimentalist to view how the `energy' in the signal is distributed among frequencies. The Fast Fourier Transform (FFT) algorithms have made power spectra one of the obvious diagnostics tools during data acquisition, and energy maps are a versatile alternative. ... The result is an energy map (Fig. 9), showing the distribution of energy corresponding to the wavelet map (Fig. ...

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• Relationship Between Auto Chirplet FF Plane and Radon Transform

Broadband SED of Ser X-1 constructed with simultaneous data and upper limits from ISGRI (filled diamonds), PICsIT (filled pentagon), JEM-X (filled squares) and ASM data (open square) plus non-simultaneous optical measurements (filled dots), NIR and far-infrared upper limits (open circles and open triangles, respectively) and radio data (filled triangles). Error bars of data points are not reported as their size is comparable to, or smaller than, that of the symbols used in the figure. ...

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• The AstroStat Slog Blog Archive chi-square distribution [Eqn]
• The AstroStat Slog distribution
• The AstroStat Slog Blog Archive Redistribution

... Let be a random deviate which follows a Poissonian probability distribution about the expectation value . Although the Poisson distribution itself is only defined for integer , one can find the following continuous `envelope function' to the Poisson values: . ... where is the gamma function . ... The expectation value of is . ... Equation 5 is used both in the present program and in boxdetect to estimate the null-hypothesis probability distribution of the weighted sum of Poissonian images. ...

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• Distribution of colours

... The Network Time Protocol (NTP) is used to synchronize the time of a computer client or server to another server or reference time source, such as a radio or satellite receiver or modem. ... Information on the NTP architecture, protocol and algorithms can be found in the Further Information and Bibliography page. The Building and Installing the Distribution page presents an overview of the procedures for compiling the distribution and installing it on a typical client or server. ...

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• Building and Installing the Distribution
• All Supernovae Distribution.
• Distribution of Supernovae according to their parent galaxies' recession

... 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...

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• Description of algorithm
• Results scientific researchs LRS

FEATURES OF THE HYDROGEN DISTRIBUTION AROUND LUNAR CRATERS PROCLUS AND KEPLER. ... In result of analysis of the data Lawrence and Feldman constructed the hydrogen distribution on the lunar surface [1]. ... However, the authors shown, that EN flux data features may be explained by other element abundance in the lunar soils, namely: Si, Ca, Gadolinium (Gd), Samarium (Sm) and Fe. ... Using of the Feldman's interpretation of the Lunar Prospector data [8], we constructed hydrogen distribution map (Fig.1). ...

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• http://selena.sai.msu.ru/Pug/Publications/Pugacheva%20LPS%2041.pdf

Employing the maximum entropy method (MEM) algorithm, we fit interstellar extinction measurements that span the wavelength range 0.125-3 ЮМm. We present a uniform set of MEM model fits, all using the same grain materials, optical constants, and abundance constraints. ... Although such usage is only a first step, the results do provide interesting insight into the use of grain size as a diagnostic of dust environment. ... ADS ] . ADS Citation Query . ... citations vs. year [year,citations] . ...

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• Infrared Spectral Energy Distributions of Nearby Galaxies
• Installing Compiled Executables for use with the IDL Runtime GPI Data Pipeline
• Introduction

Next: Power of test Up: Basic principles of Previous: Test statistics . In principle, it is possible to compute a value of the statistic for a single frequency and to test its consistency with a random signal ( ). ... The factor N means that there is an increased probability of accepting a given value of the statistic as consistent with a random signal. ... In the command individual descriptions, we often refer to probability distributions of specific statistics. ...

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• Some statistical trends and distributions
• Noise distributions
• Introduction

ON-LINE STATIC EIT RECONSTRUCTION SERVER . ... Static image reconstruction from the data measured in vivo is still intriguing problem in EIT. ... dipole (adjacent) current injection and voltage measurements on pairs of adjacent electrodes (like in Sheffield systems) . ... You can view examples of the text files for polar , dipole and trigonometric injection, use them for testing the server and find more details on HOW TO PREPARE INPUT FILE FOR THE ON-LINE EIT RECONSTRUCTION SERVER page. ...

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• Electromagnetic Tomography
• Electric field tomography
• MIT images

... Each DFS Department official document has to be issued according to the following internal procedure. Documents to be distributed outside DMD division must also be issued according to the Technical Archive procedure . ... Several documents are also available as complete templates defined internally for DFS Department documentation (e.g. template for Test Plan, for Test Report, .. ... Define the internal document number as: dfs-volxx-yyy-zzzz . ... Document title, . ... Issue number (e.g. 1). ...

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• the Technical Archive procedure for issue of documentation
• Redshift Distribution
• ESO - ESO-MIDAS Releases and Distribution

... Positive iterative deconvolution is an algorithm that applies non-linear constraints, conserves energy, and delivers stable results at high noise-levels. This is also true for Richardson-Lucy like algorithms which follow a statistical approach to the deconvolution problem. ... All algorithms resolve the objects, as shown by the reconstructions by Richardson-Lucy in Figure 2 on the right, the algorithm by M?ller in Figure 3 on the left and positive iterative deconvolution in Figure 3 on the right. ...

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• The ISOPHOT Interactive Analysis PIA, a Calibration and Scientific Analysis...
• Mapping the Jagiellonian Field of Galaxies
• Synthetic Images of the Solar Corona from Octree Representation of 3-D Electron

... 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). ...

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Figure 1: The ux density distribution of confusing sources in the IDV sample for 1.4 GHz. ... N corresponds to the number of confusing sources detected in 101 images of the IDV sample target sources (no beam shape correction applied). 1 (a) 2.4 GHz (b) 4.8 GHz Figure 2: The number distribution of modulation indices,  of the total ux den- sity calculated over the duration of each observing run: May 1994 and August 1994. The distributions of  are shown for (a) 2.4 GHz and (b) 4.8 GHz. ...

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• casacore: casa::Poisson Class Reference
• casacore: casa::HyperGeometric Class Reference
• casacore: casa::NegativeExpntl Class Reference

. An outline of how the dark matter distribution (right) was reconstructed from optical images (left) taken by the Subaru Telescope. A precise measurement of the shapes of background galaxies in observed images enabled the team to investigate the distortion pattern (center) and then reconstruct the distribution of dark matter in the galaxy clusters. // NAOJ/ASIAA/School of Physics and Astronomy, University of Birmingham/Kavli IPMU/Astronomical Institute, Tohoku University

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• http://www.astronomy.com/sitefiles/resources/image.aspx?item=%7B0E7AD457-B065-4951-A37B-700D97350B59%7D

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• http://zebu.uoregon.edu/~uochep/talks/talks05/trackrecon.pdf
• http://zebu.uoregon.edu/~uochep/talks/talks05/G050216-00.pdf
• http://zebu.uoregon.edu/~uochep/talks/talks04/S2S3GR~2.pdf

... Class . ... FRAMES NO FRAMES All Classes . ... FIELD | CONSTR | METHOD . DETAIL: FIELD | ... java.lang.Object ij.plugin.Distribution . ... public class Distribution . ... This plugin implements the Analyze/Distribution command. ... This method is called when the plugin is loaded. void . ... Constructor Detail public Distribution () . ... This method is called when the plugin is loaded. 'arg', which may be blank, is the argument specified for this plugin in IJ_Props.txt. ...

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• Uses of Class ij.plugin.Distribution (ImageJ API)