... 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 . ...

Next: The Schedule File Up: THE SCHED USER MANUAL Version Previous: Satellite Tracking Contents . This chapter covers the main input files that SCHED reads. ... See the SCHED Input and Output Files section of this manual for brief descriptions of the files and pointers to the standard versions. ... Summary List of SCHED Parameters . ... List of Frequency File Parameters . Setup Files . Standard Setup Files . ... Summary List of Setup File Parameters . Details of Setup File Parameters . ...

Next: Individual data Up: Final results Previous: Residual plots . After the last residual plot, the final parameter values (and their errors) are printed, including the magnitudes and colors of the individual stars in the extinction solution. ... This is followed by a table of the individual residuals, which includes the symbols used to identify different stars in the residual plots. ... Mon Jan 22 15:08:15 MET 1996 ...

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. ...

... A detector map is used to provide a grid of positions over which to calculate and flux weight the ARF. The default detector map is 'flat' which has a weighting of 1.0 for each detector map pixel and is rectangular having sides which just encompass the region specified in the DSS. Only detector map pixels falling within the source region are included in the ARF calculation, e.g. for a circular source box, the pixels in the corners of the detector map will be ignored. ... flat : . ...

Arecibo World Day data description . ... The F-region program covers the altitude range of 140 - 660 km. ... The KINDAT code in the CEDAR database for these parameters is 2010. ... The KINDAT code in the CEDAR database is 2021 for this kind of data. The barker-code program allows the measurement of electron concentration at a height resolution of 0.6 km with a very high S/N. This program typically covers the altitude range of 60 - 500 km. The KINDAT code in the CEDAR database is 2015. ...

... SFIT is a general-purpose code designed to optimize theoretical stellar spectra to an observed spectrum. ... While the programme expects input from "stdio", it is more natural to save commands in a file (eg "sfit_input") and run the code simply by . ... If the spectra to be fitted have a filename "star_spectrum", then the best fit spectrum will be written out, together with the renormalized input spectrum, to a file called "star_spectrum.fit". ... sets up model spectrum grid (and for 2nd star) . ...

... Several of the tasks in the spectral package share a common set of parameters. ... Each task in the spectral package has a hidden parameter which points to the pkgpars parameter file. The parameters stored here include the observed data sets and the model descriptor, and instrument-specific parameters. ... The observed counts and error data set contained in the table file ( *_obs.tab ) produced by qpspec will be the input data for subsequent spectral tasks. ...

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: . ...

... esorex.caller.recipe-dir=/home/quality/pipelines/vcam-1.0.7:/home/quality/pipelines/detmon . ... See extraction of config.processAB : # ====================================================================== # 2. esorex configuration file names for generic pipelines # List here the name(s) of esorex configuration file (s) of general pipeline (s) (e.g. detmon ) # RAW_TYPE: usually just one, but could be more # DET_ID: required only if you need to specify config files per detector (avoid ...

lsst.tcc љ 1.2.2-3-g89ecb63 . ... Files . ... include . tcc . tcsShim.h . ... 51 љ double const FL = 1.0; . ... 97 љ std::ostream & operator<< (std::ostream &os, ASTROM const &astrom); . ... 99 љ std::ostream & operator<< (std::ostream &os, FLDOR const &fldor); . ... 101 љ std::ostream & operator<< (std::ostream &os, PORIG const &porig); . ... 103 љ std::ostream & operator<< (std::ostream &os, SITE const &site); . ... 105 љ std::ostream & operator<< (std::ostream &os, TARG const &targ); . ...

... 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). ...

Comedi Documentation . ... Right to the source: #include <stdio.h> /* for printf() */ #include <comedilib.h> int subdev = 0; /* change this to your input subdevice */ int chan = 0; /* change this to your channel */ int range = 0; /* more on this later */ int aref = AREF_GROUND; /* more on this later */ int main(int argc,char *argv[]) { comedi_t *it; lsampl_t data; it=comedi_open("/dev/comedi0"); comedi_data_read(it,subdev,chan,range,aref,&data); printf("%d\n",data); return 0; } . ...

The magnetic mapping is fulfilled by the magnetic field line tracing from the satellite position up to the Ionosphere (stop trace at the altitude 110 km). ... As a rule the Tsyganenko [1987] external magnetic field model and IOPT = 3 (Kp = 2) are used. ... The output file includes the following information: . ... For example the file with name aa9610d1.geo contains the information corresponding to the aposteriory magnetic mapping for INTERBALL Auroral Probe for the first decade of October 1996. ...

... 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 . ...

... Tiny Tim has been used for generating Hubble Space Telescope ( HST ) point-spread functions (PSFs) for deconvolution, algorithm testing, proposal planning, and optical studies. ... Tiny Tim is a stand-alone program for simulating HST PSFs as viewed with the on-board imaging cameras (WF/PC-1, WFPC2, FOC, COSTAR/FOC). ... The measured aberrations for FOC f/96, WF/PC-1 PC6, WFPC2, and COSTAR/FOC are used by Tiny Tim . ... Figure: FOC f/96 observed and Tiny Tim model PSFs (pre-COSTAR) at 253 nm. ...

Next: Program use Up: Description of program searchdup Previous: Description of program searchdup . Parameter input is done with a graphic user interface. ... Input file: Name of the input catalog file. It has to be formatted, one record per source/observation, according to the format used in the Arcetri observations and source archives. ... Minimum number of observations per source Source with less than this number of independent observations are not included in the output file . ...

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. ...

... SphereParams Struct Reference . ... SphereParams (const float radius) . ... Definition at line 50 of file StelGeometryBuilder.hpp . ... Definition at line 103 of file StelGeometryBuilder.hpp . ... Definition at line 120 of file StelGeometryBuilder.hpp . ... Definition at line 112 of file StelGeometryBuilder.hpp . ... Definition at line 118 of file StelGeometryBuilder.hpp . ... Definition at line 110 of file StelGeometryBuilder.hpp . ... Definition at line 114 of file StelGeometryBuilder.hpp . ...

... 2014 February 3 . Lunar Time Lapse Panorama including Yutu Rover . ... Explanation: Where has the Yutu rover been on the Moon? ... Because it uses solar power , the mechanical Jade Rabbit goes into sleep mode to endure the two-week long lunar night. Pictured above is a digitally created time-lapse composite panorama showing the region surrounding the Chang'e 3 lander , capturing the desk-sized rover in three positions. ... Organize Your Universe: Free APOD 2014 Calendar in PDF format . ...