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/Pug/Publications/m44_70_pugacheva.pdf
• http://selena.sai.msu.ru/Greg/Publications/ms40/81_Ushkin_Michael.pdf
• http://selena.sai.msu.ru/Greg/Publications/ms38/ms090.pdf

... Parameter . ... list of files . A list of one or more spectrum files, all produced by rgsspectrum . ... A list of response matrix files, all produced by rgsrmfgen . Each response matrix is paired with the corresponding spectrum and must be compatible with it. ... file . ... This parameter controls how the quality flags from the input spectrum files are propagated into the output fluxed spectrum. ... When only one quality value is permitted, the quality column is omitted from the output file. ...

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The current set of keyword-value pairs of a task can be monitored by typing ESC K while the name of the task is present in the User Command Area. This causes (part of) the Common Output Area to be overlaid with a display containing the current user input parameters of the task. ... If there is currently a set of parameters displayed on the screen (as the result of typing ESC K ), these parameters will be edited; otherwise the name of the task is derived from the User Command Area contents. ...

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• Polarization/Stokes Handling (stokes and select)
• Input Parameters to the Self-Calibration Tasks
• User Parameters - Spectral-line Imaging CentralProcessor 0.11 documentation

The vopt parameter is computed from the optical measurements in the compilation of redshifts by rejecting outliers and measurements marked for their bad quality and computing a weighted average of the remaining measurements. ... The optical measurements are first selected and converted to a uniform system as: vop = cz + zeropoint(iref) , where cz is the compiled value and zeropoint(iref) a zero-point correction for the reference iref . ... Finally, the individual corrected measurements are combined. ...

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• HyperLEDA documentation: parameter: brief
• HyperLEDA documentation: catalogue of aperture photometry
• Mean astrophysical parameters from LEDA

... The spherical aberration affecting the HST primary mirror (Burrows et al. 1992) can seriously alter the core brightness profile of elliptical galaxies. ... In this paper we test the performance of deconvolution in recovering the original surface brightness profile in the case of elliptical galaxies observed with the HST Planetary Camera (PC). ... Keywords: Elliptical Galaxies, Deconvolution . ...

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• Ferrarese Ford: Surface Brightness Parameters from Deconvolved Images
• The CO-to-H2 Conversion Factor and Dust-to-gas Ratio on Kiloparsec Scales in
• COS Instrument Handbook

Science and metrology windows specification release 1.doc Page 1 of 5 MRO Delay Line Specification of the Science and Metrology Windows for the MROI Delay Lines INT-406-TSP-0004 The Cambridge Delay Line Team rev 1.1 20 April 2010 Cavendish Laboratory JJ Thomson Avenue Cambridge CB3 0HE UK Change Record Revision Date Author(s ... Scope The specifications produced are for the science window and the two metrology windows of the delay line. ... 2.1 Science Window Requirements .. ...

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• http://www.mrao.cam.ac.uk/projects/OAS/pmwiki/uploads/MROIDelayLine.Requirements/Science%20and%20metrology%20windows%20specification.pdf,1269009640
• http://www.mrao.cam.ac.uk/projects/OAS/pmwiki/uploads/MROIDelayLine.Requirements/Science%20and%20metrology%20windows%20specification.pdf,1271779436
• http://www.mrao.cam.ac.uk/~bn204/phd_era/publications/ursi-oof-a0poster.pdf

... 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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• Fitting and Modeling in the ASC Data Analysis Environment
• A Python-based IRAF Task Parameter Editor
• Exploring Interactive Archive Data Presentation at the COSSC

External influences on spin parameters for INTERBALL - AP . ... The main interest is that almost all kind of external influences to parameters of motion (eclipse, normalization, ROS) are presented in the one time interval. Three upper panels illustrate the spin velocity, the angle between kinetic moment and sun direction, and the nutation.All external events are represented on the lowest panel as blue, green and yellow columns. ...

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

... spectrum . ffit . ... grids . ... These commands read in a grid of model spectra. ... Values for the parameters are taken from the input models themselves, to avoid mixups. The syntax of the command arguments is precise. model{ . ... If there is only one spectrum to fit, one should set default parameters for the secondary which lie within the model grid, with <L_2/L> being a very small value. ... The output is saved in a file <file.fit> , where <file> was the name of the spectrum being fitted. ...

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• SCL Sfit SLV Commands
• White Dwarf Merger Movie
• Armagh Observatory

Russian SHAREABLE DATA CENTER Institute of Solar-Terrestial Physics SB RAS . ... Here we present the ionospheric parameters variations for quiet conditions. ...

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• East Siberian Center for the Earth's Ionosphere Research. Capabilities and

Here we compare the optical properties of porous particles of two kinds: . ... Below we show the behaviour of the efficiency factors Q ext (x), Q sca (x), Q abs (x), the asymmetry parameter g (x) and albedo (x) as well as for x = 3 and 100 the phase function i (theta) and polarization of scattered radiation p (theta) for different values of the parameters m and P . ... factors . ... Qext(x) . Qsca(x) . ... i (theta) . ... albedo (x) . ...

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• AI SPbU library of scattering codes
• Linear polarization: wavelength dependence
• Database of Optical Properties -- Level: subsubpage

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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• Galaxy Gallery Page III
• Potential Energy
• U of O High Energy Physics Seminars

... Guider functions . ... Guide Sensor Performance . ... Guide Sensor Sky Coverage/ Star Availability . Guide Star Selection Criteria . ... Guide fiber organization and reach at plug plate . ... Plug plate holes for guide stars are identical to those for science FO . ... FOV for each of 9 guide stars is 7.4 arcsec dia. (0.45 mm FO, Sumitomo IGN-05/10) . ... Selected guide stars must have no neighbor stars within TBD (5 arcsec) radius that have a brightness within TBD (5 mag.) of guide stars . ...

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• Mirror actuators

... Prev . ... comedi_from_phys -- convert physical units to sample . ... lsampl_t comedi_from_phys (double data, comedi_range * range, lsampl_t maxdata); . Converts data given in physical units (data) into sample values (lsampl_t, between 0 and maxdata). The parameter rng represents the conversion information to use, and the parameter maxdata represents the maximum possible data value for the channel that the data will be written to. Conversion is not affected by out-of-range behavior. ...

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• comedi_to_phys
• harak_e
• shmidt_e

EPM-ERA2012 Lunar Ephemeris and selenodynamical parameters from LLR data(1970-2012) M.V. Vasilyev, E.I.Yagudina IAA RAS, St-Petersburg, Russia Reflector at the Moon The reflector 's positions at the Moon surface 3.5 m telescope at Apache station INTRODUCTION MODERN EPHEMERIDES: 1. ... IAA RAS, Russia-EPM-ERA2012 The present analysis of (17580) LLR observations, (time interval 1970, March - 2012, February) Model ( brief description). The dynamical model EPM-ERA has been developed by G.A. Krasinsky. ...

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• http://www.ipa.nw.ru/conference/2002/sovet/PS/MELNIKOV.PS
• http://www.ipa.nw.ru/conference/2002/sovet/PS/PROKHOR.PS
• Keywords_75

Mesoscale Atmospheric Models: optical turbulence (C N 2 ) and meteorologic parameters * . ... Masciadri, E., Optical Turbulence Modeling and Forecasts - Toward a new era for the ground-based astronomy, . ... Forecast of surface layer meteorological parameters at Cerro Paranal with a mesoscale atmospherical model . Lascaux, F., Masciadri, E., Fini, L., MNRAS, 2015, 449, 1664 . ... MOSE: optical turbulence and atmospherical parameters operational forecast at ESO ground-based sites. ...

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• http://www.arcetri.astro.it/irlab/doc/library/javascript/clientreference/boolean.htm
• Program parameters
• Where are the tunable parameters of the kernel?

Atmospheric influence on the different radio-engineering system functioning . ESTIMATION OF ATMOSPHERIC OPTICAL CHARACTERISTICS AND REMOTELY SANSED IMAGE CORRECTION . ... Direct transmittance estimation results for 12 channels of the spectrometer CHRIS. ... We have managed to develop a direct method of estimating the discrete Normalized Atmospheric Point Spread Function (NAPSF) from available images alone, not using any external sources of information about the atmosphere. ... IRE RAS 1996-20 11 ...

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• SYNCHRONIZATION OF DRIVE-RESPONSE SYSTEMS ON CONDITION OF A LARGE MISMATCH OF
• Project 6 - RFBR - Multilayer epitaxial heterostructures of high-temperature

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 parameters of compact stars
• Other parameters of the evolutionary scenario
• Initial binary parameters

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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• MISSION WARNING
• Sun orbital parameters for Computer Ephemeris for 2014 (DE200/LE200).
• SPECTRUM ANALYZER OF MAGNETIC PHENOMENA SAMW

Do we need various assumptions to get a good FCN? A new multiple layer spectral method Cheng-li HuangMian Zhang Shanghai Astron. ... No FCN ! ... FCN,FCN,FCN.. Multiple layer spectral method (MLSM) + Linear Operator Method (LOM) Finite Element Method (FEM) · · Traditional approach solves one order ellipsoid only. ... Main Idea of FEM Boundary Surface could be described as: Let's consider how to solve the dynamic equation: Traditional Approach: Equivalent Spherical Domain . ...

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• http://www.gao.spb.ru/english/as/j2014/presentations/tercjak.pdf
• http://www.gao.spb.ru/english/as/j2014/presentations/perepelkin.pdf
• http://www.gao.spb.ru/english/as/j2014/presentations/mosenkov.pdf