One possible way for spiral galaxies to internally evolve would be for gas to flow to the center and form stars in a central disk (pseudo-bulge). ... In this paper we present radial profiles of stellar and 8 ЮМm emission from polycyclic aromatic hydrocarbons (PAHs) for 11 spiral galaxies to investigate whether the interstellar medium in these galaxies contains a central concentration above that expected from the exponential disk. ...

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• The Spectral Energy Distribution of Dust Emission in the Edge-on Spiral Galaxy
• Infrared Spectral Energy Distributions of Nearby Galaxies
• COS Instrument Handbook

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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• Effect of sources evolution on
• Test of the Initial Mass-Ratio Distribution
• Results of calculations

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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• The spectral energy distribution of PKS 2004-447: a compact steep-spectrum
• An HI selected sample of galaxies -- The HI mass function and the surface
• Finding the Bivariate Brightness Distribution of galaxies from an HI selected

... 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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• Sample Properties

... 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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Model Selection Astro193, March 9 Steps in Hypothesis Testing 1/ Set up 2 possible exclusive hypotheses - two models : M0 ­ null hypothesis ­ formulated to be rejected M1 ­ an alternative hypothesis, research hypothesis 2/ Specify a priori the significance level 3/ Choose a test which: - has the required power - approximates the conditions - finds what is needed to obtain the sampling The model with the largest value provides the best description of the data. ...

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• The AstroStat Slog sampling distribution
• The AstroStat Slog distribution
• False Alarms and Aliasing

... 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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• Corrections to the probability distribution
• Some statistical trends and distributions
• EXAMINE/ROMAFOT

... According to the most popular cosmological paradigm, the greater part of the galaxy mass is accumulated in the dark matter halo. ... The polar ring galaxies (PRGs) reveal external rings or disks of gas, dust and stars rotating in a plane roughly perpendicular to the disk of the central galaxy. ... The shape of the dark halo in the model was chosen so as to achieve the best fit to the observed rotation of both galaxies themselves and their polar rings. ... The SPRC-7 galaxy. ...

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• Lack of Dwarf Galaxies in the Local Volume Compared to Conventional Cosmology
• Metagalaxy sector, archive 2002
• Hardware sector, archive 2006

. Pulkovo Observatory of Russian Academy of Sciences is situated . near Saint-Petersburg. It was founded in 1839. 196140, Saint-Petersburg, Pulkovskoye chaussee 65/1 . English version . Russian version . This page has been accessed times since May 1, 1999.

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• Pulkovo NEO Page: Ephemeris Support

... 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

... In the case of a single pixel of a single image, is the Poisson distribution about the expectation value of the counts due to background, . As described in section 3.2 , we say there is a source present in this pixel if is larger than a cutoff value . ... This value of , minus the expectation due to background , is defined here as the detection sensitivity. Note that this does not mean that a source with an expectation value of counts which is greater than will always be detected. ...

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• Input
• Null-hypothesis probability distribution for a weighted sum of Poissonian

... Bug fixes below are collected in /pub/misc/XFree86OS2/fixes at the same site. If you came here by a notice of this URL in some newsgroup article: Here is the toplevel of the XFree86/OS2 pages . ... The following is the list of recent file dates and sizes from the main archive at ftp.xfree86.org/pub/XFree86/3.3.1/binaries/OS2. ... XFree86/OS2 3.1.2D . ... This fix is recommended because of unrelated bug fixes, but is not required specifically for XFree86/OS2 if you don't have TCP/IP 4.1. ...

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• Bugs found so far in XFree86/OS2 3.3
• Bugs found so far in XFree86/OS2 3.3.3
• Bugs found so far in XFree86/OS2 3.3.6

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
• Zen: snap sai
• Sternberg Astronomical Institute

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
• MONTE-CARLO
• RR LYRAE VARIABLES SUBSYSTEMS IN THE GALAXY, figures

Numerical theory of rotation of the deformable Earth with the fluid core, and its fitting to VLBI data . ... Improved differential equations of the rotation of the deformable Earth with the two-layer fluid core are developed. ... Poincare's method of modeling the dynamical effects of the fluid core, and Sasao's approach for calculating the tidal interaction between the core and mantle in terms of the dynamical Love number are generalized for the case of the two-layer fluid core. ...

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• Keywords_262
• Keywords_120
• Keywords_152

... dust_AbsXSec . Absorption Cross section. typedef void . ... Calculates the equilibrium temperature given the absorption cross section and a radiation field. double . ... Calculates the absortion cross section of a species/size of dust grain . ... The grain absorption cross section . ... The absorption cross section of the grain . ... Calculates the equilibrium emission at wavelength lambda from a (large) grain at temperature T and with absorption cross section xsection. double dust_EquiT . ...

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• James Gordon - Latex
• Paper I: Method Bojan Nikolic web pages (r. 329)
• casata: CASA Tools for Analysis Bojan Nikolic web pages (r. 329)

In this gallery are many images of Low Surface Brightness Galaxies which have recently been discovered and analyzed. ... The central surface brightness of this galaxy is 24.28 . Malin 2 This galaxy is another huge disk galaxy with a scale length of 15 kpc and a redshift of 15000 km/a. The high surface brightness knot in one of its spiral arms actually has the same color, luminosity and H-alpha equivalent width as the entire Large Magellanic Cloud . ... Truly it is a Low Surface Brightness Galaxy. ...

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• Comparing Means and Deviations
• Evidence for Dark Matter

. Made using Google Earth 2007 . Above: The GMRT antennas of the central array from space. The white, blurry objects are the antennas dishes. Above: The GMRT antennas of the central array from space. The position of the antennas are maked by symbols. Above: The GMRT antennas of the outer array from space. The position of antennas are maked by symbols. Last modified: Tue Apr 24 18:19:47 EST 2007

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• Siding Spring Survey
• Lecture 19: Probability Distribution Functions
• Lesson 1: Using Uncertainties

Next: Identification and Analysis of Binary Star Systems using Probability Theory . ... We present a computing code for modelling energy flux distributions, photometric indices and spectral line profiles of (non-)radially pulsating Main-Sequence stars. ... In the case of slowly rotating stars one can use the zero-rotation approximation to describe stellar pulsations. Such a model was used already by Cugier, Dziembowski & Pamyatnykh (1994) to study nonadiabatic observables of Cephei stars. ...

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• Robust Data Analysis Methods for Spectroscopy
• A Distributed System for ``Phase II'' Proposal Preparation
• Indexing and Searching Distributed Astronomical Data Archives

. 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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• "STP Data" STP Data
• Catalogue 5 of WDC-B