Next: Outputs Up: Fitting of Data Previous: External Functions . ... EDIT/FIT fitname . SET/FIT options . ... The commands have been designed so that defaults exists for almost all the parameters, (see description in Volume C of the MIDAS User Guide). ... The MIDAS command SET/FIT is used to specify the different options of the FIT command, for instance the method to be applied or the type of used functions. The instruction SET/FIT METHOD=CGNND PRINT=1 WEIGHT=S FUNCT=BLACBODY FCTDEF=USER . ...

The determination of the detector parameters is based on sets of images of a spatially uniform-illumination scene (flatfield frames) and without any illumination (dark frames), putting a plug in place of the filter, taken at a series of exposure times. ... We interleave before and after each exposure time in the series of flatfield frames a set of reference images at an exposure time of 1 sec to determine the possible temporal variation of the illumination level. ...

ESO Phase 3 Data Release Description Please start from this template when preparing the documentation for your ESO Phase 3 data release. ... Finally, the release description will be published as submitted - without further editing by ESO - to support the user community in utilizing the data. ... Please indicate if this is a catalogue data release. ... Data Reduction and Calibration Please address the following questions for scientific catalogue data, particularly in case of source catalogues: . ...

... Input via keyin format is of the form keyword = value . ... The input keywords are not case sensitive. Most of the values required by SCHED, except for file names in case sensitive systems like unix, are also not case sensitive. keywords are, in all cases, limited to 8 characters in length. ... Keyin values can be mathematical statements in parenthesis; for example, dur = 15 rep = (4*5) This example shows the most likely way in which this capability might be used in SCHED input files. ...

Next: Three-dimensional Data Analysis in IRAF and ZODIAC+ . ... A data analysis system has been developed at SRON, which has been designed to allow rigorous control of the quality of its processed data products. ... This means recording all parameters of all steps which lead to the establishment of the final data products (Figure 1 ). ... Figure: A processing pipeline is a sequence of tasks with several input/output files and parameters, which pass data from one task to the next. ...

Next: DETAILED LIST OF ROSAT Up: PROS USERS GUIDE Previous: List of Related Documents . This section lists all PROS tasks (some of which are not described in this guide) and some useful IRAF tasks which are included. ... converts FITS to images and/or tables . ... delete a list of images . ... convert an Einstein FITS file into an IRAF/PROS QPOE file . ... convert a list of IRAF/PROS IMAGE files into RDF compatible format . ... convert a list of IRAF/PROS QPOE files into RDF compatible format . ...

The MOD and IOPT parameters value depend of the external magnetic field model (MOD), used during magnetic mapping and IOPT version (IOPT = Kp + 1), see the table: . MOD . External model . IOPT range . ... N.A.Tsyganenko, Planet. Space Sci., ... N.A. Tsyganenko, A magnetospheric magnetic fields model with a warped Tail current sheet: Planet. Space SCI., ...

... Exploring the physics of Type Ia supernovae through spectral analysis . ... Their progenitor scenario as well as the details of the explosion mechanism remain a mystery. ... It produces a supernova spectrum for a given luminosity, photospheric velocity, time since explosion and several elemental abundances. Tweaking these parameters to produce a spectrum that fits an observed spectrum is a complex, as of yet, manual task. ... The search space is large and complex. ...

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 ...

This is a list of all currently available observing modes in CIMA. Different modes are available depending on whether CIMA is run in pulsar or in spectral line mode. ... Note that the appearance of the windows refer to CIMA version 3.1 , which for most observing modes is slightly different than from CIMA version 2.3 and 3.0 and completely different from CIMA version 2.2. ... Non-ALFA . ... Pulsar cross calibration . ... Drift map . ... ALFA : indicates whether the observing mode works with ALFA . ...

... 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) . ...

... 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 . ...

The beam pattern and the polarization characteristics . of the radio telescope RATAN-600 . The Mueller matrix elements was computed via formulas [1]: . ... The BP were computed by the aperture method, proceeding from the fild distribution in the aperture of the primary mirror. The components of the main and cross-polarization components of the electric field in the vertical aperture of the primary mirror was computed in Frenel diffraction approximation. ...

RTT150 . ... This optical scheme is similar to 1:7.7 system but has the different parameters of secondary mirror 2 and corrector 3. Primary mirror 1 reflects light to the secondary mirror 2 which collects it on the focal surface of system. Lens corrector 3 is placed between focal surface and the secondary mirror which allows to obtain large flat linear field of 100 mm diameter. Focal length, mm . ... Linear field of view, mm . ... Angular field of view . ... 0.039 mm, %, at least . ...

... 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 . ...

... UNIX commands . C shell (csh) . ... with special meaning for shell . changing . directories . ... command line . ... command alias . command history . command interpreter . command path . command substitution . command syntax . commands . ... arguments to . ... creating . ... executing in shell scripts . ... read arguments as input to shell scripts . ... use in shell scripts . ... files . ... conditional statements See shell script . ... programs See shell scripts . ...

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. ...

... FTP access the basic models is here . ... Below, we put short descriptions of the used SED models for the photometric redshifts providing by the current server . ... The uniqueness of this model consists in expanding to the near IR (NIR) of Rocca-Volmerange and Guiderdoni's (1988) atlas of synthetic spectra with a revised stellar library, which includes parameters of cool stars. ... Homepage of the GISSEL model). ... Another model used earlier is the model of synthetic spectra of Poggianti (1997). ...

The Agile window provides complete control over the Agile high-speed photometer. ... All other parameters are specified as part of the command that starts an exposure sequence. ... To connect the filter wheel controller, issue this command in the command bar at the bottom of the Log window: agile connDev fw . ... To home the filter wheel controller, issue this command in the command bar at the bottom of the Log window: agile fwhome (there must be a filter wheel mounted in Agile for homing to succeed). ...

Title : Ace1 Filename : Ace1.wad Release date : 8/1/03 Author : P.Westlake....aka "Ace" Game : DOOM2 Level : Map 01 Email Address : Other Files By Author : Misc. ... You may use any port to play this level but please disable mouselook and jumping as it was intended to play under vanilla Doom2 parameters ;) It took 2-3 weeks to complete and most of that time was taken learning the editors I used so hopefully its a bit playable. ...