Next: Star Formation Rate and Up: No Title Previous: Calculation of Evolutionary Tracks . To start calculations, we choose the distributions of the initial binary parameters: the mass of the primary ZAMS component, , binary mass ratio, , orbital separation a . ... whereas the mass ratio distribution is not. ... The zero assumption often made is that the mass ratio distribution has a flat shape, that is binaries with a high mass ratio occur as frequently as those with equal masses. ...

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• Test of the Initial Mass-Ratio Distribution
• Dependence on the Scenario Parameters and Initial Distributions
• Seminars

... Where we have just a single image we assume a probabilistic mode of source detection such that, at a given image pixel, if the probability that the observed value at that pixel could have arisen through statistical fluctuation of the background at that pixel lies below a certain limiting probability , the pixel is considered to contain a source. In XMM practice it is likelihood rather than itself which is employed; in this case the detection criterion is for to exceed the cutoff . ...

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• Detection sensitivity
• The detection threshold

... Using the central limit theorem, the total noise can be approximated by a Gaussian or normal distribution which has the frequency function : . ... where is the mean intensity of the source. ... In the statistical analysis of the probability distribution of data several estimators based on moments are used. ... For a normal distribution, these moments are and while for a Poisson distribution are and . Besides these moments other estimators are used to describe a distribution e.g. median and mode . ...

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... RJMCMC Similar to Richardson Green 1997 Knowledge of the PSF makes things easier Insensitive to e.g. posterior for ten sources with = 3: Number of Components 9 10 11 12 0.141 0.222 0.220 0.157 0.022 0.029 0.027 0.021 Mean SD 7 0.029 0.018 8 0.058 0.019 13 0.082 0.014 Simulated Data Source region (2 SD) is about 28% of the area and contains about 41% of the observations Positions (-2, 0), (0, 1), (1.5, 0) with intensities ... Approximate the number of sources (2 in this case) 2. ...

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• The AstroStat Slog background
• The AstroStat Slog Pareto distribution
• The AstroStat Slog Blog Archive [ArXiv] Pareto Distribution

Next: The FMAPE Algorithm Up: HST Image Restoration with Previous: Introduction . ... We shall work with the following model: an object emits light with intensity given by a spatial distribution . The light is focused by the optical system over a detector array consisting of individual discrete and independent detectors. ... We assume that the detection process is Poisson distributed. ... The imaging equation corresponding to this model is: . Equation ( 1 ) in discrete form becomes: . ...

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• Model Fitting
• Stellar Photometry
• The Hubble Deep Field - Cosmic Ray Rejection

Distribution of the analyzed SEPs with different >100 MeV proton fluxes ( J 100 ) at the microwave flux density plane ' S 9 vs. ... 1) General correspondence takes place between intensities of microwave bursts and proton fluxes - J 100 increases when S 9 and S 15 rise. ... 3) Powerful microwave bursts ( S 9 , S 15 >3000-10000 sfu ) with hard radio spectra ( S 9 < S 15 ) correspond to majority of powerful proton fluxes ( J 100 >10 pfu ). ...

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... PPTA timeline . ... List of projects . ... RedGW . ... One of the main goals of pulsar timing array projects is to limit the existence of a background of gravitational waves (GWs). Jenet et al. (2006) developed a method to determine such a limit if (and only if) the pulsar timing residuals were statistically white. In the paper we used data from six pulsars from the PPTA project to obtain a limit. The remaining pulsars were rejected because their timing residuals were not white. ...

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• The spectral energy distribution of PKS 2004-447: a compact steep-spectrum
• correlator:distribution [ATNF VLBI Wiki]
• Tools - Random numbers

... 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
• harak_e
• Determination of atmospheric parameters and calculation of chemical composition

Following are instructions to build and install the programs in this distribution. Make sure that you have all necessary tools for building executables. ... The automatic build process expects a configuration file called Config.local . ... The configuration file specifies the directory in which to install the binaries, as well as control over the generation of debugging code and reference clock support. ... Cleans out object files, programs and temporary files. make distclean . ...

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• The Network Time Protocol (NTP) Distribution
• APOD: 2011 June 29 - Abell 2744: Pandora's Cluster of Galaxies
• APOD: 2000 December 30 - A Year of Resolving Backgrounds

... The distribution of galactic RCB stars is controversial. Several authors have argued that they belong to a thick galactic disk, and are thus old Population I stars. However, they may alternatively belong to the even older galactic bulge (Population II). ... In either case, the populations are sufficiently old that RCB stars must have relatively low masses ( ). ... These are the only RCB stars for which a distance is known and hence for which an absolute magnitude can be deduced. ...

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• Armagh Observatory
• Armagh Observatory: Chris Winter [ lte-codes ]
• Background

Scale-heights of the Galactic disk subsytems with different ages and metallicities . V.Marsakov & Yu. ... It is based on the fact, that all stars cross the disk plane several times during their Galactic orbital period. ... We have used our representative sample of nearby disk F2-G2 stars Marsakov & Shevelev (1995) in which fundamental stellar parameters was determined on the basis of published date on uvby-photometry, proper motion and radial velocities. ... Marsakov V.A., Shevelev Yu.G. Bull. ...

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• Vladimir Marsakov Abstracts

Chair of solid state physics . ... The Physics of Phonons . ... In the first part of the course “The Physics of Phonons” the dynamics of atoms in one- and three- dimensional crystalline lattices is considered in detail. The quasiparticle conception in solids, taking phonons as an example, is discussed; creation and annihilation operators of phonons, main properties of acoustic and optical phonons dispersion laws, density of phonon states. ... Crystalline state. ... Acoustic and optical phonons. ...

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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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• ENGAMPLE

LOFAR Object Detection Nested Sampling LOFAR peculiarities.. Object detection for LOFAR Object detection for LOFAR LOFAR Object Detection Nested Sampling LOFAR peculiarities.. ... The Likelihood The Prior Ratio 2 3 4 Object detection for LOFAR LOFAR Object Detection Nested Sampling LOFAR peculiarities.. ... The Likelihood The Prior Ratio Outline 1 LOFAR Object Detection Bayesian Framework Nested Sampling LOFAR peculiarities.. ... The Likelihood The Prior Ratio For Instance (2).. ...

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• http://www.mrao.cam.ac.uk/~bn204/lecture/2008/bn-l3.pdf
• Small scale distribution in Molecular Clouds
• DUST: dustiface.h File Reference

... SiD workshop, Fermilab, April 9-11 2007 April 9, 2007 Nick Sinev, SiD design Workshop, Fermilab 1 Topics 1. ... What and how was simulated What and was One column clusters effects Accepted background density Hit reconstruction efficiency Hit efficiency How to improve efficiency Conclusions April 9, 2007 Nick Sinev, SiD design Workshop, Fermilab 2 What is this April 9, 2007 Nick Sinev, SiD design Workshop, Fermilab 3 Marty's idea Shift charge in neighboring columns in opposite directions. ...

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• http://zebu.uoregon.edu/2004/es399/chitable.html
• http://zebu.uoregon.edu/~uochep/talks/talks04/blount12-04.pdf
• http://zebu.uoregon.edu/~uochep/talks/talks05/G050216-00.pdf

These lesson introduces you to the use of uncertainties. ... It introduces probability distribution functions, the Gaussian Distribution, hypothesis testing and model fitting. This lesson introduces you to the different types of uncertainty, and how you can estimate them from the scatter in your measurements, or from knowledge of your experimental set-up. ... It also covers averaging and how that affects uncertainties. Back Main Lab-Skills Page . ...

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• Siding Spring Survey
• Lecture 19: Probability Distribution Functions
• Proposed Facility

... Up: Software Systems and Tools . ... The Starlink Software is a collection of astronomical packages and utilities comprising over 120 separate components. When built, the system needs between 500 and 650 MB disk space (without source) making it ideal for distribution on CD-ROM. Each component has been individually packaged into an easy-to-install bundle for users to obtain over the Internet via a ``point and click'' WWW interface from the Starlink Software Store. ...

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• Distributed Software for Observations in the Near Infrared
• Modelling Spectro-photometric Characteristics of Nonradially Pulsating Stars
• ADASS 2003 Conference Proceedings

... 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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• XFree86/OS2 Download Page
• Long description of example of cell background calculation
• Long description of example illustrating background calculation

... The distribution of redshifts among the DXRBS FSRQs identified so far (Figure 3) is quite similar to that of the 1 Jy and S4 samples. ... A more thorough comparison will have to await completion of our survey and the convolution of the redshift distribution with the WGACAT sky coverage. As has already been mentioned by Hook et al. (1996), selecting flat-spectrum sources is an efficient way of finding high-redshift, radio-loud quasars. ...

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• Stars and Galaxies
• Colours and magnitudes
• Sample Properties

The project of the informational system creation on the problem of evolution of radio galaxies, as a part of the "Big Trio" project aimed on studing of distant radio galaxies, is designed. This system allows a user to operate with simulated curves of spectral energy distributions (SED) to estimate ages and redshifts by photometry data. Authors use SEDs of several models for different types of galaxies. ... The HTTP and e-mail access is organized to this system. ...

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• Description of SED models