Next: Front End Construction Up: Minutes of the 1st Previous: Minutes of the 1st . ... Calculated system temperature: 25-26K at 1525 MHz, 29-30K at 1375 MHz and 34-25K at 1225 MHz. ... Calculated G/T - again, center pixel better . ... Multi Beam Sky Footprint: Separation 2 beam widths between individual beams . ... Calculated Beam Comatic Level about 8 dB . ... German . ... Slide 1.9 shows calculated T sys with 2 points for each frequency; one is for the center beam and other is for the outside. ...

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Pulkovo NEO Page . ... EPOS Software Package . ... EPOS ( E phemeris P rogram for O bjects of the S olar system) is the Windows PC application for study and ephemeris support of observations of the Solar system objects. ... It controls the part of common data and transfers the control to one of the programs that solve the restricted set of tasks. ... So with the EPOS software package one can calculate the accurate ephemerides for many objects and get the quick illustration of their motion as well. ...

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... insbs instrument=<instr> ra=<ra> dec=<dec> apos=<apos> bstoolsout=true|false . ... Given the viewing direction of the star tracker in terms of Right Ascension and Declination of the boresight + astronomical position angle insbs computes the viewing direction of the instrument specified via the instrument parameter - result is written to stdout in verbose form (default) or as a strbs command line if bstoolsout =true. ...

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• Elaborations.

... The FOS employed one of six basic data taking modes to acquire science data: . Spectrophotometry (ACCUM). ... Image. ... ACCUM was by far the most commonly used observing mode. ... In IMAGE mode observations both the number and length of rasters and the y- position of each raster could be specified, so that: 1) a white-light image of all or a portion of the aperture was possible with the MIRROR, and 2) spectra from different portions of the aperture were sampled with a disperser. ...

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• CCD Position and Orientation on Sky
• Observing with Linear Ramp Filters
• ACS Instrument Handbook for Cycle 20

Program: DECIM Purpose: Decrease size of a set in any direction with an integer factor Category: MANIPULATION, CALCULATION File: decim.c Author: M. Vogelaar Keywords: INSET= Give set (, subsets) to decimate: Maximum number of subsets is 2048. ... SHIFT= Shift in start of decimation: [0] Specify which of the 'decim' number of pixels will be transferred to the new created output pixel. ... The number of output subsets is the same as the number of input sub- sets. ...

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• casacore: casa::ParAngleMachine Class Reference
• TPSPEEDH
• imstat

... A vector , that's what. ... Graphically, each stretch on the ground or velocity can be represented by an arrow in its direction, its length giving the magnitude--for instance, an arrow AB 200 mm (milimeters) long for the airplane's motion and another one BC 40 mm long, in the same direction, for the wind. ... Just as one can combine two vectors into one--their sum--so it is also possible to move in the opposite direction--given a single vector, find two vectors whose sum it is. ...

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• How Orbital Motion is Calculated
• Trapped Radiation -- History

... A vector , that's what. ... Graphically, each stretch on the ground or velocity can be represented by an arrow in its direction, its length giving the magnitude--for instance, an arrow AB 200 mm (milimeters) long for the airplane's motion and another one BC 40 mm long, in the same direction, for the wind. ... Just as one can combine two vectors into one--their sum--so it is also possible to move in the opposite direction--given a single vector, find two vectors whose sum it is. ...

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• How Orbital Motion is Calculated
• The Sine of the Sum of Angles

... Note that the size of a region cannot be specified in celestial coordinates (e.g., arcminutes) for this task (1 pixel = 0.5 for the ROSAT HRI). xs srcint source qpoe file ( ): xdata$rh110267.qp source region descriptor ( ): c 2326 4406 120 background qpoe file ( ): bkgd region descriptor ( ): a 2326 4406 150 200 output root name (_ccr.tab): (arlac) --- Creating aspect histogram table from qpoe --- --- Computing vignetting ...

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• *qpspec* - Time Resolved Spectral Fitting
• Array File Specifications
• *xflux, hxflux* - Calculation of X-ray Flux

... Restrictions ) are used. If specified form of output is EMP then astrometric equatorial coordinates are printed in the form usual for Ephemerides of Minor Planets, with formal precision of 0.01 minute of time in R.A. and 0.1 minute of arc in declination. ... It should be noted that the near-opposition ephemerides are not calculated for bodies/ points with numbers from –12 to 0 (in case they are included into task for computation of such ephemerides only their names are displayed in the results). ...

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IV International Astronomy Olympiad . ... Text of these problems is available also . ... To solve every problem you may use constants and well-known values you know by heart. ... The apparent diameter of the Moon, as seen from the Earth, is 31'. ... Can you observe a star with magnitude . ... Consider the stars as black bodies. ... Estimate the diameter of a black hole constructed using this patent from a ship with the mass of 5000 tn (1 tn = 1000 kg). ... What stars would you observe this nigth? ...

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• II International Astronomy Olympiad, Problems to solve
• III International Astronomy Olympiad, Problems to solve

Reciprocity relation in checking calculations of the optical properties of non-spherical particles V.G. Farafonov St.Petersburg University of Aerocosmic Instrumentation, St.Petersburg, 190000, Russia and V.B.Il'in Astronomical Institute, St.Petersburg University St.Petersburg, 198504, Russia ABSTRACT There are many methods to solve the problem of light scattering by non-spherical particles , but only the separation of variables method ( ... Michel B., Farafonov V.G. (2000) J. Quant. ...

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• Database of Optical Properties -- Level: subpage

. Back to A.Zasov's homepage.

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To main of Laboratory . The research work and design of optical and optical-electronic devices are carries out by laboratory staff: . ... Lens: . ... In the layout 1 prism systems perform functions of dispersive element, corrector of aberrations, optical reducer. ... Spectral range 200 - 400 nm; . ... Back Forward . ... The main corrector's function are compensation of field aberrations of the main spherical mirror of a telescope (diameter of 600 mm, f'=1200 mm) and increase aperture ratio. ...

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The basic characteristics of the instrument are set by the aperture, focal length and resolution of the image forming lens, the dispersion of the spectrometer, and the sensitivity of the detector. ... The lens is internally focused, and maintains acceptable focus (2 pixels in the detector plane) over a typical spectral coverage of one grating setting. ... along the spatial dimension of a 25mm square detector in the final spectral image plane the 400mm lens is 3.2њ. ... Diffraction grating . ...

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• Transit Finder
• FractalBoxCounter (ImageJ API)
• Orthogonal_Views (ImageJ API)

... A program packet is developed for the detailed research into the 3D structure of the magnetic fields of solar active regions as well as the overall solar magnetic field. ... Solar activity is the result of motion and interaction of the coronal magnetic fields, so their study is of primary interest of solar physicists. We have developed a program packet for the detailed research into the 3D structure of the magnetic fields of solar active regions as well as the overall solar magnetic field. ...

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• Calculating the Position and Velocity Components of HST
• Modelling Spectro-photometric Characteristics of Nonradially Pulsating Stars
• A New PROS Task for Calculating HRI Source Intensities or Upper Limits

... SPIcam is a general purpose, visible-wavelength, direct imaging CCD camera with > 50% QE between 400-900 nm. It may be operated in either traditional point-and-stare mode or in a drift-scanning mode. The detector in SPIcam is a backside-illuminated SITe TK2048E 2048x2048 pixel CCD with 24 micron pixels and an unbinned plate scale of 0.14 arc seconds per pixel, giving a field of view of 4.78 arc minutes. ... CCD pixel size = 24 m . ... CCD read noise = 5.7 e - / pixel 0.1 . ...

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• TUI:Telescope:Slew Window:Options:Drift Scan
• Plug-plate coordinate system
• TUI:Telescope:Offset Types

Russian SHAREABLE DATA CENTER Institute of Solar-Terrestial Physics SB RAS . ... The algorithm and appropriate program for decametric radiosignal propagation conditions prediction for paths from 500 to 9000 km have been developed at ISTP SB on the basis of normal wave method (AltyntsevaB.I,Iliyin N.V., Kurkin V.I. and others //Decameters channel simulation on the base of normal wave method . ... Solar activity indices are chosen automatically from the prediction date from the database . ...

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grdvolume - Calculating volume under a surface within a contour grdvolume grdfile [ -C cval or -C low / high / delta ] [ -L base ] [ -R west / east / south / north [ r ] ] [ -S [ k ] ] [ -T ] [ -V [ l ] ] [ -Z fact [/ delta ] ] grdvolume reads a 2-D binary grd file and calculates the volume contained between the surface and the plane specified by the given contour (or zero if not given). ... Alternatively, search using all contours from low to high in steps of delta . ... Default is no scaling]. ...

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• http://xray.sai.msu.ru/~ivan/gmt/man/pshistogram.html
• http://xray.sai.msu.ru/~ivan/gmt/man/psrose.html
• http://xray.sai.msu.ru/~ivan/gmt/man/grdgradient.html

Next: Specifying Pixels in Up: MIDAS Data Structures Previous: Specifying Keywords . The MIDAS table file system is described in detail in chapter 5 of this volume. Here we just explain briefly how to access the various elements in a table file. To do so, it is necessary to specify the table name , the column and the row . ... would display the element in column 3 of row 10 in table file tname.tbl . ... All table commands default the data files to tables with extension .tbl . ...

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• Specifying Pixels in an Image
• Numerical Values of Image Pixels
• Specifying Keywords

... This plug-in enables you to add various types of lighting effects to your (RGB) image. ... Directional light . ... Well, you get the idea :) The default settings for this light-type is [-0.5,-0.5,-1.0]. ... Higher values makes your image reflect a lot of light (appear lighter or more intense), while smaller values makes it appear more dull or matte. ... A value of 1.0 makes your image very shiny (bright high-lights) while smaller values makes you image less shiny, making the high-lights dimmer. ...

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• APOD: 2000 January 14 - Chandra Resolves the Hard X Ray Background
• APOD: 2000 December 30 - A Year of Resolving Backgrounds
• Configuration Options