HST Call for Proposals and HST Primer for Cycle 24 . ... Hubble Space Telescope Primer for Cycle 24 > Appendix A: Orbit Calculation Examples > A.2 COS Examples . ... Example 1: COS NUV Imaging and Spectroscopy in One Orbit . ... First, an image is taken, followed by obtaining a TIME-TAG spectrum with two exposures using different gratings. The specific observations, as requested by the user, are summarized in Table A.4 . ... Example 2: COS NUV Imaging and FUV Spectroscopy in Two Orbits . ...

... Tpram - time of the PRAM instrument (aquisition computer) . ... Bx - DC magnetic field with a fixed amplitude calibration; X component . ... The color lines present FFT from the AC magnetic field (Waveform); Bwx, Bwy, Bwz - from the bottom. ...

... Tpram - time of the PRAM instrument (aquisition computer) . ... Bx - DC magnetic field with a fixed amplitude calibration; X component . ... The color lines present FFT from the AC magnetic field (Waveform); Bwx, Bwy, Bwz - from the bottom. ...

... rgssources (rgssources-6.0.1) [xmmsas_20080701_1801-8.0.0] . ... If the file name is in either the PPS or the rgsproc formats, then rgssources is able to deduce the instrument name from the file name. The PPS format is PooooooooooiiteeeSRCLI_0000.FIT; the rgsproc format is rrrrooooooooooiiteee00_sources.ds. In these templates, rrrr is the rev number, oooooooooo is the observation identifier, ii the instrument (either R1 or R2), eee the exposure number and t the exposure type (either S or U)). ...

... Up: Data Analysis and Processing Techniques . ... Also, a method for quality control of CCD observations is suggested. ... Everyone who observes a celestial object using a CCD detects moving celestial objects as a ``by product''. ... We hope that our investigations may be useful for near-Earth space control and also for searches of the moving celestial objects through analysis of old and new CCD frames obtained at any amateur or professional astronomical observatory. ...

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 . ...

... The J, H and K bands are characterized by a bright background, such a background is mainly due to the emission of atmospheric lines and of thermal radiation. ... If the source cover a large fraction of the slit, spectra off-source must be observed to adequately sample the sky background. ... The on chip integration time (time spent in each position of the slit) must not exceed 40 seconds in J and H bands and 60 seconds in K band. ... We suggest a sequence of 10 for each elementary integration time. ...

... Spectral regions highlighted by green bars have been used to detemine the тЯиB z тЯй value from H Balmer lines, and the magenta bars highlight the spectral regions used to estimate the magnetic field from metal lines. ... The FORS1 instrument of the ESO Very Large Telescope was used to obtain low resolution circular polarized spectra of nearly a thousand of different stars, with the aim of measuring their mean longitudinal magnetic fields. ...

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The VLTI Calibrator Selector Tool is a tool intended to assist in the selection of suitable interferometric calibrators for VLTI observations with MIDI and AMBER. It uses a model of the VLTI and its instruments to assess the fringe visibility, given the observed bandpass, the geometry, spectrum, and coordinates of the target and the time at which the observations are to be made. ... The tool offers an HTML/Java based interface and consists of two pages. ... The quality flag depends on LDD_chi2. ...

It is easy to incorporate information from an instrument or the telescope into your scripts. ... mess with the getKeyVar statements because getKeyVar returns None in debug mode, making the commands run, which is perfect. import TUI .TCC.TCCModel import TUI .Inst. DIS .DISModel from TUI .Inst. DIS .StatusConfigInputWdg import StatusConfigInputWdg InstName = DIS class ScriptClass(object): Simple script to configure DIS . def __init__(self, sr): Display ...

... Example of an association table . Example of a CCD reduction table . ... CCD commands . ... Command parameters (1) . ... Checklist of necessary table files . ... DO commands . ... Observation Summary Table with file classifications appended in column :EXPTYPE and :OPATH as defined and applied in Table . ... Columns for star-catalog table files . ... Passband columns of the instrument table file . ... Detector columns of the instrument table file . ... Instrument table file for a simple CCD setup . ...

... На самом деле, когда я писал эту -- -- программу, мне хотелось потренироваться в проведении интервью по -- -- правилам SADT методологии. ... Логическое описание блоков SADT модели. ... Основное предназначение этих классов - хранить перечень посуды и -- -- инструментов, соответствующих различным блокам SADT модели. ...

... Because of the potential impact of poor weather on 3mm observations, the ATCA has used a "swap" system of flexible scheduling for these observations. ... This was both to encourage more proposals that could be used as swaps and to reduce the burden of swapping (the swap system tends to discriminate against the centimetre observer). ... For example Directors Time could be used for 3mm proposals if there was no bad weather (this would not be possible if a centimetre swap were mandated). ...

... Primordial theory review : Dick Bond . Defects and the CMB review : Andy Albrecht . ... Gravitational wave contribution to CMB anisotropies : V.B. Lukash and E.V. Mikheeva . C_l from cosmic strings : Lloyd Knox . Some aspects of CMB anisotropies induced from topological defects : Mairi Sakellariadou . ... CMB anisotropies from scaling sources : Ruth Durrer . ... SZ observations I : Sarah Church . ... Holes in the microwave sky? ... Detecting cosmic strings in the CMB : James Robinson . ...

... In order to compare the number of different evolutionary stages obtained and X-ray luminosity of the chosen X-ray sources with the observed galactic values we use the sum of C/O+O/C , where C and O are the calculated and observed values of a given binary type, respectively. If we make comparison for a number of different binary species (for example, we compare the number of CV, number of X-ray pulsars,   total X-ray luminosity of LMXB, etc.), we write this criterion in the form: . ...

STEP INTO THE BLUE - MEADE INSTRUMENTS PRODUCT GUIDE . ... Telescopes . LX850 Series . ... Superb optical performance coupled with time proven computerized pointing and tracking has made the LX200 ACF series a best-seller in the high-performance telescope class. ... Meade's revolutionary LS LightSwitchтДв series of telescopes use advanced technologies to do what no other consumer telescopes have done before: take all the hassle out of using a telescope. ... Coronado€о Solar . ... Spotting Scopes . ...

... Telescope . ... In 2009 a new Electron Multiplying Frame Tranfer CCD Andor iХon DU-888 was purshased with support from Excellence Cluster Universe, Technische Universitaet Muenchen and delivered to RTT150 telescope. ... First scientific observations were made on 3--10 November 2009. In particular, the time resolved observations of Crab pulsar were made (33 ms pulse period). In the Figure we show the pulse profile with 7 msec time resolution, obtained in a single 10 minute long observation. ...

. This diagram shows a small table with three transparent cells and illustrates how their final background is determined. The table consists of two rows. Four (labeled) cells lie in the first row, but the second cell spans the first and second row. The first, third, and fourth cells of the second row are "empty". Each non-empty cell has a red background and a double black border. Each empty cell has the table's background color (specified as #ff0) as its own. Return to image.

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