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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