... 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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• Recent Advances in Parameter Estimation in Astronomy with Poisson-Distributed

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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• Initial binary parameters
• Dependence on the Scenario Parameters and Initial Distributions
• Restrictions on the Scenario Parameters

... Posts tagged ?BEHR? ... A great advantage of Bayesian analysis, they say, is the ability to propagate the posterior. That is, if we derive a posterior probability distribution function for a parameter using one dataset, we can apply that as the prior when a new dataset comes along, and thereby improve our estimates of the parameter and shrink the error bars. ... Suppose you have two data sets, D1 and D2, hypotheses H, and background info (model, etc.) ... Comment . ... 7 Comments . ...

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• Comments on: chi-square distribution [Eqn] By: Alex By: vlk By: aneta By: aneta
• Structure of the Spectral Package
• The AstroStat Slog Blog Archive chi-square distribution [Eqn]

... Fitting the observed dependence includes calculations of the polarization cross-sections averaged over particles orientation and size distribution, their normalization and the comparison of obtained dependencies with Serkowski's curve representing observational data for a chosen star. ... Variations of the polarization factors with wavelength are shown in Fig. 16 for homogeneous spheroidal particles with PF orientation. ... The distinction between prolate and oblate spheroids is also clearly seen. ...

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The problem of solar wind data correlation for the observations onboard several spacecraft is very important for three points of view: . ... This problem is studied now in detail by systematic determination of ion flux and ion velocity data correlations by INTERBALL-1 (IKI group), WIND and IMP 8 (both - MIT group). ... Solar wind plasma correlation lengths from IMP 8, WIND and INTERBALL-1. ... Correlation of solar wind observations onboard several spacecraft: INTERBALL-1, IMP 8 and WIND data. ...

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Some peculiarities of orbits of observed comets. ... Icarus, 2005 Simulation and reality Distribution of anti-perihelia of short-period comets with e 0.9 ( ecliptic coordinates ) Distribution of anti-perihelia of short-period comets with e 0.9 ( ecliptic coordinates ) Distribution of anti-perihelia of long-period comets with 0.9 e 1 ( ecliptic coordinates ) ­ ...

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• http://www.gao.spb.ru/english/as/j2014/presentations/kudryashova.pdf
• http://www.gao.spb.ru/english/publ-s/viii-rfs/p099.pdf

... Our resulting sample of ELGs presented in Tables 2 and 3 is not artificially biased to any specific type of galaxies. ... Since we are looking for selection of a sample of Case BCGs, it is interesting to examine how the detected BCGs are connected with Case emission-line codes. ... Altogether BCGs comprise about 60 % of all Case ELGs which display emission lines in our spectra, or about 44 % of all Case galaxies with some emission-line code. ... Among those with the code ``w'' about 40 % are BCGs. ...

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• Regression Analysis
• Sky and redshift distribution
• Estimation

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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• A New Database of Observed Spectral Energy Distributions of Nearby Starburst
• Modeling Dust and Starlight in Galaxies Observed by Spitzer and Herschel: NGC
• Fundamental Parameters, Integrated Red Giant Branch Mass Loss, and Dust

... 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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• Determination of atmospheric parameters and calculation of chemical composition
• harak_e
• Emission molecular bands

... A list of spectrum files from a set of observations, referring to one RGS instrument and one spectral order. These spectra files must be produced using the attstyle=user and associated parameters from a call to rgsproc . ... A list of accompanying event list files, in the same order as the spectra files. ... If this parameter is set to yes, the spectra files of the input lists will be combined to produced a combined spectrum file each for both spectra and background spectra files. filermf . ...

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Next: The derived luminosity and Up: The galactic population of Previous: The galactic population of . Figure 16: The observed distribution of pulsar dispersion measures. Dotted curve is the total known population, solid curve is the Parkes survey. Figure 17: The observed distribution of pulsar distances above the galactic plane. ... Figure 18: The observed distribution of pulsar flux densities. ...

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• Cosmological Parameter Survey Using the Gravitational Lensing Method
• Pulsar Group Main/Psrfits
• PPTA Wiki | Projects / RedGW

... Fit Teff, theta and E(B-V) to IUE spectrum and uvby photometry using a grid of helium-rich model flux distributions. models{ . ... simon/models/01980001/19325he90L.s . simon/models/01980001/20325he90L.s . simon/models/01980001/21325he90L.s . simon/models/01980001/22325he90L.s . simon/models/01980001/23325he90L.s . simon/models/01980001/24325he90L.s . simon/models/01980001/25325he90L.s . simon/models/01980001/26325he90L.s . ... IUE data file in "spectrum format 2" . ...

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• Armagh Observatory
• sfit help file

... Bojan Nikolic web pages (r. 329) . ... We present a Bayesian approach to calculating the coefficients that convert the outputs of ALMA 183 GHz water-vapour radiometers into estimates of path fluctuations that can be used to correct the observed interferometric visibilities. ... Inference of Coefficients for Use in Phase Correction . ... Simulating Atmospheric Phase Errors, Phase Correction and the Impact on ALMA Science . ... Copyright 2005 -- 2016, Bojan Nikolic feedback welcome ...

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• Astrophysics Group MADCOW
• Paper I: Method Bojan Nikolic web pages (r. 329)
• B Bayesian value for

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/Shev/Publications/ms38/ms084.pdf
• http://selena.sai.msu.ru/Pug/Publications/ms38/ms080.pdf
• http://selena.sai.msu.ru/Shev/Publications/m44_76_sinitsin_shevchenko.pdf

Next: Redshift Distribution Up: Sample Identification Previous: Previously Identified Sources . ... In Figure 3, we plot the redshift distribution of DXRBS FSRQs opposite that of the 1 Jy and S4 samples. In Figure 4, we plot the redshift distribution of DXRBS BL Lacs opposite the Slew and 1 Jy samples. ... The apparent deficit of objects at the very highest luminosities is a result of the smaller area of sky covered by DXRBS compared to, e.g., the Slew and 1 Jy samples. ...

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• List procedures
• Sky Distribution of ~14.000 Observed Stars | ESO
• ESO - ESO-MIDAS Releases and Distribution

... 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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• Galaxy sector, archive 2012
• Metagalaxy sector, archive 2005

. N OTE: . Only clusters with R<60 kpc were used to compute the spatial parameters and metallicity gradients for all subsystems except the corona. The numbers in parantheses give the number of clusters for which the corresponding parameter is known. The X O scale length of the old halo is strongly distorted by the observed asymmetry of the distribution of the corresponding clusters projected onto the XY plane ( Fig. 4А ) . discussion in the text | previous table .

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• Vladimir Marsakov Publication List
• Vladimir Marsakov Abstracts
• Mid Scales Role

The radial distribution of metallicity of star-forming galaxies in a galaxy cluster can inform us about the mass assembly and enrichment history of the galaxy cluster. ... Both galaxy clusters are cool-core clusters at redshift z т?? ... The gas-phase metallicity of star- forming galaxies in MACS1115+01 exhibit anti-correlation with projected distance т??0.15 ТБ 0.08 dex/Mpc, whereas the radial metallicity distribution of RXJ1532+30 is statistically flat (т??0.09 ТБ 0.12 dex/Mpc). ...

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• COALA - Wolfgang Kerzendor
• The SMS Survey

... Публикации и издания Публикации профессорско-преподавательского состава СГАУ Издания проф. Сосниной Т.Н. Biosphere: Analysis of Value Parameters . ... Besides, the ways of saving the use value and value properties of biosphere are analyzed. The expediency of transformation of two-criterion theory of value into the three- criterion theory of the balance of value, where the ecologic component performs the function of the key criterion has been founded. ... BIOSPHERE USE VALUE OF THE PRODUCT: MAIN . ...

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... The Search of a pulsar Once the dedispersed time series is obtained, a Fourier transformation is performed. ... 2 Binary parameters The orbit of a pulsar , as well as any object, in a binary system is determined in its geometrical characteristics, space displacement and syncronised in time by the following parameters : Semimajor axis Eccentricity Longitude of periastron Binary period Time of ascending node a e PB T0 True spin period and observed spin period The ...

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• http://www.naic.edu/~astro/School/Talks/handson_ao2.pdf
• Orbits in the period / acceleration plane
• INTRODUCTION to Spectral Line Observing at AO