WFC3 Instrument Handbook for Cycle 24 . ... Wide Field Camera 3 Instrument Handbook for Cycle 24 > Appendix A: WFC3 Filter Throughputs > IR/F125W . ... Wide J filter. Figure A.196: Integrated system throughput for F125W. Figure A.197: Point source S/N vs. ... for the F125W filter, assuming high sky backgrounds and a 3 в 3 pixel aperture. Figure A.198: Extended source S/N vs. ... for the F125W filter, assuming high sky backgrounds and a source uniformly filling a 1 arcsec 2 aperture. ...

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... This is possible at modest cost due to the low moments of inertia of the telescope and enclosure. ... This same performance will be achieved in higher winds when the telescope enclosure is facing away from the wind, or by using wind screens. ... The telescope system (MILT) will be remotely operable with an on-site operator's assistance by an astronomer located at one of the ARC member institutions. ... Mean Wind Speed . ... Offsets > 10 deg: 1 arc sec rms max . ... 5 sec max, tracking to tracking . ...

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... Alternatively, the PI channel boundaries will be read directly from the data subspace extension of the input image (not yet implemented). ... EPIC PN offset columns (as specified in the offsets extension of the photon event list) are set to zero in the exposure map, if they had been removed from the input reference EPIC image. ... The task tries to determine the exposure time by looking for gti extensions in the input image of the form STDGTInn, STDGTIn, STDGT, or GTI. ...

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Next: Summary of reduction Up: Echelle Reduction Previous: Saving the Data . In the present version we will be concerned with the standard configuration of CASPEC, the Cassegrain Echelle Spectrograph which is in operation at the Cassegrain focus of the ESO 3.6 m telescope. ... In its standard configuration CASPEC uses a a 31.6 lines/mm echelle grating together with a 300 lines/mm grating cross disperser. ... The table shows the change in resolution with the order number. Table: Resolution . ...

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• Echelle Spectra
• General Description
• Instrument file

... 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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• Gemini NIFS Brief Description.
• Other Infrared Instruments.

... Up: Telescope and Instrument Control Systems . ... 216, Astronomical Data Analysis Software and Systems IX, eds. N. Manset, C. Veillet, D. Crabtree (San Francisco: ASP), 271 . ... NASA Goddard Space Flight Center and AppNet, Inc. are developing AIML to command and control astronomical instruments. Our software architecture combines the platform-independent processing capabilities of Java with the power of XML. ... Instrument description is too tightly coupled with details of implementation. ...

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• Imaging by an Optimizing Method
• Modelling Spectro-photometric Characteristics of Eclipsing Binaries
• The Communication of Images from New Generation Astronomical Telescopes

... Calculated exposure times do not take into account instrument and telescope overheads. ... The reference area for the S/N is circular with a radius equal to FWHM of the Image Quality PSF at the airmass and wavelength of observation. ... begin{equation} \mathit{FWHM}_{\text{IQ}} = \sqrt{\mathit{FWHM}_{\text{atm}}^2(\mathit{s},x,\lambda)+\mathit{FWHM}_{\text{tel}}^2(\mathit{D},\lambda)+\mathit{FWHM}_{\text{ins}}^2(\lambda)} \end{equation} } \) . ... The Exposure Time is the product of DIT and NDIT . ...

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• VLTI Calibrator Selection Help Page
• SINFONI Exposure Time Calculator
• Documentation

... Instrument Description . Software: Version 4.0 . Version 3.0:Complete Documentation . ... ИОНОЗОНД ПАРУС, разработанный в ИЗМИРАН, предназначен для диагностики ионосферы и оперативного прогноза КВ связи. ... Общая структура ИОНОЗОНДА ПАРУС, Технические Характеристики , Конструктивные параметры на настоящий момент соответствуют модификации Комплекса: ВЕРСИЯ 3.0 . ... Там же находится полное описание Комплекса ИОНОЗОНД ПАРУС: ВЕРСИЯ 3.0 . ... 2004 IONOSONDE PARUS ...

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hstpolpoints -- Reduce linear polarization data for HST instruments for a set of apertures . ... imalis = "" [list of file names] . ... Name of STSDAS table file giving the parameters for polarization determination for the instrument corresponding to the input images. ... A 13 column table is produced listing the aperture names, X and Y positions (from the input pointab table) together with the normalised Stokes I, Q and U parameters and errors, the linear polarization and position angle and errors. ...

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• HSTPOLIMA (V1.00) --- April99 --- HSTPOLIMA (V1.00)
• HSTPOLSIM (V1.00) --- April99 --- HSTPOLSIM (V1.00)

... As I mentioned at the recent Groningen international SKA meeting, there is a need for a large-area multi-beaming demonstrator for at least two reasons. ... The LOFAR instrument, to operate in the frequency range 10-250 MHz, will contribute vital information to the design and operation of a new class of multi-beaming telescope. ... The different operating frequency range also means that LOFAR cannot illustrate the scientific potential of area re-use (multi-beaming) in the cm-wave band. ...

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• http://www.atnf.csiro.au/projects/askap/techdocs/Array_Lens_Hybrid_SKA_presentation.pdf
• http://www.atnf.csiro.au/computing/software/gipsy/sub/gds_extend.dc2
• casacore: casa::LCExtension Class Reference

... Astrophysics Group . ... VSA . ... CAT . ... The Very Small Array is a custom-built radio telescope (operating between 26-36 GHz), designed expressly to make high resolution observations of the cosmic microwave background (CMB) radiation on angular scales around and below one degree. ... The VSA has been operated in ?compact array? and ?extended array? configurations (see the technical description below) and data collected to achieve high sensitivity in both regimes have been analysed. ... 1.75 GHz)...

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• Astrophysics Group Integration of the NIRSpec instrument
• OptInt PmWiki : Wiki Style Examples
• Description of the OOF software architecture Bojan Nikolic web pages (r. 329)

... The low energy plasma composition spectrometer AMEI-2 is built to be able to find in the low energy range of the phase space (E, q, j) and separate the fluxes of the major ion species in the magnetotail - H+, He++, He+ and O+, and analyse their energy and angular distributions. ... Electrostatic angular scanning in one direction and the use of the spin of the satellite to sample the other angle give the ability to measure 2-D distributions for each ion specie several times per spin. ...

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• INTERBALL/ELECTRON EXPERIMENT
• OMNIDIRECTIONAL PLASMA SENSOR VDP
• List of currently available KP AZ.

. The description of the instrument is divided into the following sections: . Optical Design . Cryogenics and Mechanics . Electronics and Software . Determination of Detector parameters . Some photos of the instrument . Other high resolution images .

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• IBIS: Technical Description
• Descrizione tecnica NICS
• LonGSp: Optical Design

... 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

... HYPERBOLOID is a plasma spectrometer aimed at the investigation of the low energy ions dynamics in the polar ionosphere and magnetosphere on the INTERBALL Auroral Probe . ... The instrument is basically a multi-directional ion mass spectrometer measuring ion distribution functions over an energy range from ~0.1 to 80 eV. ... The ion angular and energy distribution are obtained by means of an electrostatic optics defining 2 planes with several entrance windows. ...

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• PhSRM
• SKA-3 Experiment Description
• Mars96

. This diagram illustrates how a background image may be repeated within the content and padding areas of a box. In this example, a background image is first centered within a box (established by the BODY element of the example). The box contains paragraphs of text, shown in gray to make them discrete. The image, a blue wavy line on a pale yellow background, is then repeated vertically, to the top and bottom of the BODY box. The effect is to create a wavy band down the center of the page. Return to image.

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• Long description of example illustrating background calculation
• Long description of example of cell background calculation
• Appendix B: Changes from CSS1

Next: *imcalc* - Obtain a Up: Calibration Previous: Exposure Map . Background maps are provided by the standard processing for all ROSAT and Einstein instruments. For the PSPC and IPC these are in three standard bands: soft, hard, and broad (Table 6.2). ... N.B.: ROSAT PSPC background maps in SASS 5-6 or higher are generated by smoothing a source-subtracted, exposure corrected image (see the ROSAT Data Products Guide). ... imcalc* - Obtain a background subtracted image for ROSAT PSPC Data . ...

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• Charged Particle Subtraction
• ISDN References
• Funtools and DS9 Image Display

... Galaxies 99 Cosmic background with model of cloudy interstellar medium Yu. ... Figure 1: Averaged spectrum of the cosmic background I f in frequency range 0.25 200 MHz for the Galactic poles. ... First interpretation of the cosmic noise background spectrum at broad band frequency range 0.25 200 MHz with a model of the cloudy interstellar medium ISM is presented here. ... Synthesized background spectra I f for regions of the Galactic poles at the frequency range 0.25 200 MHz is presented in Fig. ...

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• Extended time series of Solar Activity Indices

... 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). ...

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xyz2grd - Converting an ASCII or binary table to grd file format xyz2grd xyzfile -G grdfile -I x _ inc [ m|c ][/ y _ inc [ m|c ]] -R west / east / south / north [ r ] [ -D xunit / yunit / zunit / scale / offset / title / remark ] [ -F ] [ -H [ nrec ] ] [ -L ] [ -N nodata ] [ -V ] [ -Z [ flags ] ] [ -: ] [ -bi [ s ][ n ] ] xyz2grd reads a z or xyz table and creates a binary grdfile. xyz2grd will report if some of the nodes are not filled in with data. ... H Input file(s) has Header record(s). ...

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• http://xray.sai.msu.ru/~ivan/gmt/man/grdfft.html
• Conclusion
• Gravitational wave background from nearby galaxies