... The described procedure returns the one-dimensional response distribution in PI channels, based on an input energy. The redistribution function of the MOS cameras comprises a main peak (roughly centred on the input photon energy); a lower-energy secondary peak, whose relative magnitude is inversely correlated with the photon energy, and a noise term which extends down to the detection threshold energy. Details of the current calculation are given in the CCF release note, CAL-SRN-272. ...

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• Description
• XSPEC session thread
• Input

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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• Dependence on the Scenario Parameters and Initial Distributions
• Initial binary parameters
• Parameters of binary compact star evolution

... The technology needed to implement a Distributed Astronomical Data Archive (DADA) is available today (e.g., Fullton 1993). Query interface standards are needed, however, before the DADA information will be discoverable. ... These parameters would be used to index each dataset in each catalog. ... The technology is available today to perform cross-catalog queries, to fetch the data at the click of a mouse, quickly to add new observation catalogs, and to distribute the load across multiple machines. ...

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• The SuperCOSMOS Sky Surveys
• Bias-Free Parameter Estimation with Few Counts, by Iterative Chi-Squared
• A New Entropy Measure Based on Multiple Resolution and Noise Modeling

... Radio Catalog . The corrections in NVSS fluxes leading to the corrected Version 1.1 also result in changes to some of the figures and tables in Kimball Ivezi? ... The results are qualitatively the same. ... The new versions of the figures, along with the original versions (in high resolution), are available here . ... These figures, along with Table 4, continue to motivate t = 0.35 as the optimal separator between "simple" and "complex" sources). ... Complex Sources . ... t NVSS . ... galaxy . ...

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• simager CentralProcessor 0.11 documentation
• User Parameters - Preparation of the Science field data CentralProcessor 0.11
• Pulsar Group PmWiki/Available Actions

Orbital data : INTERBALL AZ GSE and GSM cartesian coordinates, GSE cartesian velocity (once per 10 minutes). ... Magnetic field data from IMAP experiment. Magnetic fileld absolute value and magnetic field index (the difference between absolute value and model value), status flag. ... Counts of H+ and O+ ions are accumulated during one spin period by detectors D6 (antisunward looking), D8 (spin plane), D10 (sunward looking) of TRICS2 subsystem (1.0-30 keV). ... TRICS1, TRICS2, TRICS3 subsystems: . ...

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• AZ Key parameters, 1997
• AZ Key parameters, 1998
• AZ key parameters, 1996

... 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
• IFP parameters

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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• COS Instrument Handbook
• Benchmarking the calculation of stochastic heating and emissivity of dust
• HDF-S Filename Legend

Static Fourier spectrometers are often used for spectral measurements of the ionosphere emissions. There are two main advantages of Fourier spectrometers (FS) - large geometric factor and high spectral resolution; these parameters are two orders better than for grating spectral instruments. ... In scanning Fourier spectrometer optical and electric modulation of signal is used to avoid this problem, for static Fourier spectrometer there are no such ways. ...

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• ION AND ELECTRON ENERGY DETECTOR PAN-2
• Theoretical Astrophysics

. 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

... The value of tile-size, NW , may be thought of as a sixth coordinate axis in the chirplet transform parameter space - TF-area. Including this sixth coordinate axis provides us with a hierarchical (multi-resolution) CCT. ... Various 2- D slices through the multiresolution CCT may correspond to useful tilings of the TF plane with true parallelograms (true to the extent that the DPSS define a truly rectangular region in the TF plane). ...

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• Relationship Between Auto Chirplet FF Plane and Radon Transform
• Gaussian Chirplet Transform (GCT)

Observed maximum rotation velocity uncorrected for inclination effect. This quantity is calculated from 21-cm line widths at different levels and/or rotation curves (generally in H_alpha). ... These data are characterized by some secondary parameters: telescope, velocity resolution, level of the 21-cm line width and bibliographic reference. ... we start from a standard sample (a set of measurements giving a large and homogeneous sample). ... HyperLeda . ...

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• Outline of the Available Methods
• Documentation: LEDA: parameter: vrot
• HyperLEDA documentation: parameter: celpos

As in the last years, the Ephemerides of Minor Planets for 2015 are prepared by the IAA RAS only in the electronic form. ... Orbital elements of all numbered planets have been determined in IAA all over again on the ground of available observations in the catalog of the Minor Planet Center. ... More detailed information on orbital elements used in the present volume of EMP and their accuracy is given in section "Information on new orbital elements". ... a) information on new orbital elements; . ...

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• ENGAMPLE
• IAA GPS Analysis Center
• Keywords_262

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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• ESO - Newsletter May 2014
• Stellar parameters from calibrations of spectral types
• ESO - Science Announcements

... 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
• Sternberg Astronomical Institute
• Zen: NewExtentsBasedRanking

... Archives . ... Reduced and Processed Data . ... 2 distribution plays an incredibly important role in astronomical data analysis, but it is pretty much a black box to most astronomers. ... Comment ( RSS ) | ... I guess in the typical analysis we call chi2 a ?random variable? that follows the chi2 distribution: . ... where D(i) is the observed data, M(i) is the model predicted data and we ?silently? assume that D(i) is normally distributed and each i measurement is independent. ... Chandra Blog . ...

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• The AstroStat Slog Blog Archive Quotes from Common Errors in Statistics
• Regions and Source Parameters
• Produce a spectral data set using the PROS task 'xray.xspectral.qpspec'

... A Bayesian value for may be found simply by treating it as another parameter in our hypothesis space. ... where in the last factor we can drop the conditioning on since it is alone that induces the data . ... Evaluating the appropriate Gaussian integral gives . ... Nevertheless, for realistically large data sets, the distribution is so strongly peaked that it overwhelms any reasonable prior on , and so we assign the Bayesian value of the regularisation constant to be that which maximises . ...

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• Inference of Coefficients for Use in Phase Correction Bojan Nikolic web pages
• DUST: dustiface.h File Reference
• Paper I: Method Bojan Nikolic web pages (r. 329)

Toshinori Abe & Masako Iwasaki 1/8/2002 1/5/02 1 l l MIP energy distribution Energy linearity and resolution Momentum and Impact parameter resolution l 1/5/02 2 l l l l Detector geometry is given by XML file for a flexible detector setting. Output data (hits,...) is written in ROOT file format to take advantage of object oriented I/O. The package works on various computer plat forms (Linux, SunOS, Windows,.. ... Tracking performance with SD calorimeter has been studied using Geant4. ...

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• http://zebu.uoregon.edu/~uochep/talks/talks05/trackrecon.pdf
• Low Surface Brightness Galaxy Gallery

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/suvorkin.pdf
• http://www.gao.spb.ru/english/as/j2014/presentations/ding.pdf
• Pulkovo NEO Page: Ephemeris Support

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
• Population of Galactic globular clusters, tabl

... There are a lot of computer codes simulating this scattering and freely available in the Internet (see e.g. links on our JPDOC page ). ... The code and input file are available in the directory . ... A slightly modified code of Barber Hill with a C-shell and input files is available in the directory . ... The code, input and test output files are available in the directory . ... See also readme file. file. ... The code, input file and their description (a TeX file) are available in the directory . ...

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• Linear polarization: wavelength dependence
• Polarization properties (transmitted radiation)
• Project HILYS