... mm] CAMCOORD1 2 translation in X . ... mm] CAMCOORD2 origin in SACCOORD - X . ... mm] origin of telescope frame in SACCOORD - X . ... X-coordinate of center of PIXCOORD1 pixel (RAWX0/RAWY0) in CAMCOORD1 system . ... absolute uncertainty associated with X0 (currently unused) . ... absolute uncertainty associated with EULER_PHI (currently unused) . ... absolute uncertainty associated with EULER_THETA (currently unused) . ... absolute uncertainty associated with EULER_PSI (currently unused) . ...

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... The first of the equations defines the position of the spectral orders, m , in the raw image, while the second equation gives, for each order, the dispersion relation in one dimension. ... where the coefficients are computed using least squares techniques on a grid , i.e. sample number and line number of points located within the spectral orders of the image. These points in the grid are found automatically by an order--following algorithm, normally using the FLAT or STD image. ...

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• General Description
• Product Folder(Obsolete): TC215, 1024- X 1024-PIXEL CCD IMAGE SENSOR
• Product Folder: TC213, 1024- X 512-PIXEL CCD IMAGE SENSOR

... GSAOI Home . Instrument . ... The Gemini South Adaptive Optics Imager (GSAOI) is a near-infrared adaptive optics camera that will be used with the Multi-Conjugate Adaptive Optics (MCAO) system on the Gemini South 8-m telescope . ... Gemini's major instrumentation goal is to develop its Multi-Conjugate Adaptive Optics (MCAO) system for scientific use on Gemini South. ... Existing adaptive optics systems use a single natural guide star or artifical laser guide star to measure this image blur. ...

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. This diagram illustrates how the definition of a pixel depends on the users distance from the viewing surface (paper or screen). The image depicts the user looking at two planes, one 28 inches (71 cm) from the user, the second 140 inches (3.5 m) from the user. An expanding cone is projected from the user's eye onto each plane. Where the cone strikes the first plane, the projected pixel is .28 mm high. Where the cone strikes the second plane, the projected pixel is 1.4mm high. Return to image.

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• Long description for the second Bach/XML formatting example
• Long description for example illustrating absolute positioning
• Long description of example illustrating floating with clear

... 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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• NICMOS3 Homepage

... Required_Reading SPK . Brief_I/O Variable I/O Description -------- --- -------------------------------------------------- handle I Handle of an SPK file open for writing. body I Body code for ephemeris object. center I Body code for the center of motion of the body . frame I The reference frame of the states. first I First valid time for which states can be computed. last I Last valid time for which states can be computed. segid I Segment identifier. epoch I Epoch of ...

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• CSPICE Routines: ETCAL_C
• HDF-S Flanking Fields Data Reduction / Technical Issues
• Reference File Descriptions Logs

... It was then mounted on the telescope and the cal values were measured using absorber and sky (see measuring the cals on the telescope using absorber and sky for a description). ... Blue: the cal value computed using the absorber and sky (y factor). ... Blue: a 3rd order polynomial fit to the absorber (red) and ratio (blue) cal values versus frequency (the green sky only cal values were not used). ... The 3rd order polynomial fit versus frequency only used the absorber and absorber/sky ratio values. ...

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• WAPP Radar Interface
• GALFA System Description
• ALFA Performance

... Classes . ... casa::Timer . ... user () const . ... Get the user+system time (in seconds) since last "mark()". double . ... Get the user+system time (in seconds) since last "mark()". double casa::Timer::all_usec . ... Get the user+system time (in microseconds) since last "mark()". void casa::Timer::mark . ... Show real, user, system time (in seconds) on cout or a user supplied stream. double casa::Timer::system . ... Get the system time (in microseconds) since last "mark()". double casa::Timer::user...

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• Channel Selection, Averaging and Doppler Correction - UV Linetypes
• casacore: casa::MRBase Class Reference
• casacore: casa::MeasRef< Ms > Class Template Reference

Stellarium 0.12.3 . ... Classes . ... File Structure . ... StelMainGraphicsView Class Reference . ... More... #include < StelMainGraphicsView.hpp > . void  . ... Definition at line 37 of file StelMainGraphicsView.hpp . ... Definition at line 105 of file StelMainGraphicsView.hpp . ... Definition at line 100 of file StelMainGraphicsView.hpp . ... Definition at line 103 of file StelMainGraphicsView.hpp . ... Definition at line 108 of file StelMainGraphicsView.hpp . ... StelMainGraphicsView.hpp . ...

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• Stellarium: ScreenImage Class Reference
• Stellarium: StelSkyPolygon Class Reference
• Stellarium: gTimeSpan Class Reference

... Here is an example of the output header of CATS data. ... SIMPLE=T / BITPIX=8 / character information NAXIS=0 / no image data array present EXTEND=T / may be standard extensions OBJECT= CATS SEARCH / CATS search result ORIGIN=SAO RAS DATE=01/01/1997 / date of file creation END XTENSION=TABLE / F-file table extension BITPIX=8 / 8-bits ... NAXIS1=93 / No. of characters per row NAXIS2=1000 / the number of lines (sources) TFIELDS=10 / there are 16 fields per row EXTNAME= CATS / object name: ...

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• comedi_sv_measure
• SCORPIO-2 project: description
• Description of algorithm

The following papers summarize the characterization and technical performance of IBIS : . ... Characterization of Fabry-Perot interferometers and multi-etalon transmission profiles. ... Righini, A., Cavallini, F., Reardon, K. P., 2010, Astronomy and Astrophysics , 515 , A85, . ... The filter wheel is located between the two interferometers. ... The interferometers can be rapidly tuned, simultaneously, so to allow sequential scanning of the spectral lines of interest (see movie in IBIS Intro ). ...

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• Determination of the Detector Parameters
• Ranger 7
• Descrizione tecnica NICS

... Previous: The HERSCHEL/PACS Common Software System as Data Reduction System . ... The basic data reduction routines are coded in ANSI C. The high level scripting language Python is used to connect the C-routines allowing fast prototyping. Several Python scripts are written to produce the needed calibration data and to generate the final result, a wavelength calibrated data cube with the instrumental signatures removed. ... Figure 2: Mosaicked collapsed data cube of the galactic center . ...

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• Representations of Celestial Coordinates in FITS
• Automatic Detection of Linear Features in Astronomical Images
• Modelling Spectro-photometric Characteristics of Eclipsing Binaries

RTT150 . Russian-Turkish 1.5-m Telescope . ... Until 2002 observations were mostly performed with ST-8E CCD in the 1:7.7 Cassegrain focus. ... In April, 2003 telescope was equipped with a larger-size CCD Andor DW436 . ... 2048 x 2048 pixels, . ... Since summer of 2002 the main focal detector of the RTT150 telescope was AP47p CCD in 1:7.7 Cassegrain focus. ... During September 3-13, 2002 works on installation of new autoguiding system ( photo 1 ) were carried out on RTT150 telescope. ...

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I/146 Positions and Proper Motions (Roeser+ 1988) ================================================================================ Catalogue of Positions and Proper Motions Roeser S., Bastian U. =1988A .. ... 449R ================================================================================ ADC_Keywords: Positional data; Proper motions Description: PPM North gives J2000 positions and proper motions of 181,731 stars north of -2.5 degrees declination. ... The mean epoch is near 1931. ...

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• Positions and Proper Motions - South
• Supplement to the PPM Star Catalogue
• SAO Star Catalog

The FSP3 event includes those parts of the magnetic conjugations between any couple of four considered spacecraft, which satisfied to the FSP1 or to the FSP2 criterion. ... The value of the relative geocentric angular distance between magnetic field line's footprints is considered during FSP3 situation selection. The mentioned angular distance value less then 5 deg is used as a criterion of the magnetic conjugation. ... for the first SC the red color and the first line are used, . ...

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• The magnetic conjugation numerical file description
• HYPERBOLOID Results Page
• Microsatellite bus ?Chibis?

GENERAL DESCRIPTION OF DATABASE . It is a matter of common knoledge, that solar magnetic fields and, in particular, magnetic fields of sunspots, play important role in many solar events. In Pulkovo observatory the long-term data set of daily observations of magnetic fields of solar sunspots was accumulated, which contains great potential for further researches in solar physics. ... Second section includes files containing sum data about magnetic fields for every observational day. ...

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• General description of the database

... In the above example, the second region uses the global coordinate system (PHYSICAL by default). ... Supported systems include: name description ---- ----------- PHYSICAL pixel coords of original file using LTM/LTV IMAGE pixel coords of current file FK4, B1950 sky coordinate systems FK5, J2000 sky coordinate systems GALACTIC sky coordinate systems ECLIPTIC sky coordinate systems ICRS currently same as J2000 LINEAR linear wcs as defined in file In addition, two mosaic coordinate ...

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• Infrared Data
• Getting Common Information About Access Points
• Model Spectra for Spectral-Fitting Program

... Exposure Time Calculator (ETC) . ... ESO - Public Surveys . ... the recommended values to use for DIT, . ... Detector on-chip integration (DIT): seconds. to your chosen value - a separate page gives recommended values to use for DIT - for modes 1 and 2 below you may wish to start with the maximum recommended values as these will minimize the effect of read noise (a total object exposure of Y secs with DIT=X secs will produce Y/X lots of read noise) and give you a lower limit on the time needed. ...

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• VISTA - Visible and Infrared Survey Telescope for Astronomy

ntpdate [ -bBdosu ] [ -a key ] [ -e authdelay ] [ -k keyfile ] [ -o version ] [ -p samples ] [ -t timeout ] server [ ... ] . ntpdate sets the local date and time by polling the Network Time Protocol (NTP) server(s) given as the server arguments to determine the correct time. ... A number of samples are obtained from each of the servers specified and a subset of the NTP clock filter and selection algorithms are applied to select the best of these. ... The default is /etc/ntp.keys . ...

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• Gadget Box PPS Level Converter and CHU Modem
• Spectracom 8170 and Netclock/2 WWVB Receivers
• Scratchbuilt CHU Receiver

Multi-Frequency Synthesis in K-band . The Multi-Frequency Synthesis (MFS) permits to realize a good quality imaging of the continuum radio sources in short time. ... The RadioAstron mission will operate one K-band circular polarized channel at fixed frequency 22,232 GHz. ... In general one K-band RadioAstron channel with fixed frequency will be unchanging and compatible with all the ground radio telescopes. ... Progress of the RadioAstron Project in Pictures . ...

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• Description of the RadioAstron project, russion version