STIS Instrument Handbook for Cycle 24 . ... Space Telescope Imaging Spectrograph Instrument Handbook for Cycle 24 > Chapter 17: Calibration Statusand Plans > 17.10 SM4 and SMOV4 Calibration . ... STIS-08: Aperture Wheel and Lamp Functional Tests . ... Measurement of the location of the CCD spectra and images on the detector for each CCD spectral element ( G230LB , G230MB , G430L , G430M , G750M , G750 ) and MIRVIS using the HITM calibration lamps. ... STIS-16: CCD Image and Pointing Stability . ...

... The Science Operation Department is composed of Astronomers, Telescope Instruments Operators(TIOs) and Data Handling Administrators(DHAs). ... Astronomers have proposed several methods to quantitatively measure the amount of turbulence above the telescope, which the most common ones is Differential Image Motion Monitor (DIMM). In optical testing, the Hartmann test is the common method to test the quality of optical components. ... Hartmann mask consists of 48 lenses. ...

... As modern observatories evolve to production units delivering data products and calibrated scientific data to the end users, new challenges arise in assessing the quality of data products. ... Taking the analogy of speed control on a motorway we can describe the system as a device (radar) collecting measurements of the system performance (passing cars). ... One of the direct applications of quality control is the verification of instrument performance based on the analysis of calibration exposures. ...

... An OBJECT column gives the name of the object observed (usually a star name). ... In critical cases, it is common practice to measure sky on two or more positions around a target object, and these positions must be identified. ... A general treatment of this problem requires a column called OBJECT, bearing the usual name of the object (as in the star tables); a column labelled STARSKY, to distinguish between star+sky, star alone, or sky alone; and additional columns to identify the sky position. ...

... Where exposures are to be ignored by the PCMS, the task will generate an error. ... EPIC MOS supported modes Prime full window, Prime partial RFS, Prime partial W2, Prime partial W3, Prime partial W4, Prime partial W5, Prime partial W6, Fast mode uncompressed EPIC pn supported modes Prime full window, Prime large window, Prime small window, Fast mode timing, Fast mode burst OM supported modes OM science user de ned, EPIC M1 ...

IBIS Data Analysis . ... IBIS . ... Flat Fielding - Introduction . The images obtained by IBIS will have intensity variations across the field of view that are not due to the solar image, but rather caused by instrumental effects that alter the observed intensity in each point of the field of view. ... IBIS Flat Fielding Techniques . ... Therefore, it is desirable to obtain the flat field measurements center on a point along the equator near the heliographic center of the solar disk. ...

ST-ECF Technical Instrument Report WFC3-2009-04 The cross dispersion profiles of the WFC3 grisms H. Kuntschner, H. Bushouse, M. KЭmmel, J. R. Walsh April 30, 2009 ABS TRACT This document summarizes the analysis of the cross-dispersion profile width for the three grisms of the WFC3. For the IR grisms, the cross dispersion profile width derived from white light images and monochromator steps obtained in TV3 provide consistent results also in agreement with estimates derived from direct images. ...

New reduction of minor planets photographic plates obtained with Pulkovo Normal Astrograph A.A. Berezhnoy Pulkovo Observatory of RAS, Saint-Petersburg, Russia Minor Planet observations at Pulkovo Periodical observations of 14 bright asteroids named Selected Minor Planets (SMP) were performed at Pulkovo since 1948 within the international framework started by works of B.V. Numerov and D. Brouwer. ... 108 133 113 74 124 67 97 88 14 84 64 5 20 19 Epochs (YYYY.MM) 1200 Mean values of total obs. ...

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... Circular polarization of the bright side of Iapetus versus wavelength, obtained with FORS2 at the ESO VLT during the night 2011-03-28 at a phase angle of 0.77 . ... It can be noted that a change in signal occurs in circular polarization observations that are taken after rotating the instrument by 90 degree with respect to the intial position angle on the sky. ...

... In order to realize the optimal scientific return from the VLT, ESO has undertaken to develop an end-to-end data flow system from proposal entry to science archive. The VLT Data Flow System (DFS) is being designed and implemented by the DFS Group (ESO Internal access only) in collaboration with VLT Division and Instrumentation Division . ... VLT Control System Interface . ... OBs are the quantum of data that flows within the DFS, collecting state, data and status information as they flow. ...

Magnetic field measurements onboard the Interball Tail spacecraft are carried out by the FM-3I instrument which consists of two flux-gate magnetometers covering two different ranges: [-200, +200] nT and [-1000, +1000] nT. Besides scientific goals, the FM-3I experiment data is used to perform the attitude control of the Interball Tail spacecraft. ... August 22, 1995 . ... October 18, 1995 . Top of the page . ... Back to the Interball Home Page . ...

The large magnetic cloud caused by coronal mass ejection at the Sun on January 6, 1997 came to the Earth at early morning on January 10 and continue to interact with Earth's magnetosphere till January 11 (see for example home page of this event prepeared by Dr. M.Peredo http://www-istp.gsfc.nasa.gov/istp/cloud_jan97/event.html ). ... During the days discussed here INTERBALL-1 satellite was in the magnetosphere (MS) near its dusk flunk - see the Fig. 1 for compearing. ...

Static Fourier spectrometers are often used for spectral measurements of the ionosphere emissions. There are two main advantages of Fourier spectrometers (FS) - large geometric factor and high spectral resolution; these parameters are two orders better than for grating spectral instruments. ... In scanning Fourier spectrometer optical and electric modulation of signal is used to avoid this problem, for static Fourier spectrometer there are no such ways. ...

Peremennye Zvezdy ( Variable Stars ) 32 , No. ... We report on our photometric analysis of the poorly studied cataclysmic variable in Ophiuchus, 1RXS J174320.1-042953 (DDE 11). ... The long-term behavior of J1743-0429 shows that it is a probable magnetic cataclysmic variable (polar), with a large difference between its low and high states. The orbital period obtained from our observations is 0 0866, or 2 08, close to the lower boundary of the period gap of cataclysmic variables. ... Fig. ...

Astron 193 Lecture 2, Jan.28, 2015 NOTES 1/ Data vs. ... 4/ Data Storage View Your Data Software to read the data files rrent Astronomy Formats FITS inary with standards, Cu b defined keywords, but may become not good enough for large data of the future LOFAR, SKA in radio, LSST ds9 display the data mage gui, but also access to catalogs download and image the files i event files contain all the information about the observation photons , energy, arrival times ...

We report first results of a multifrequency campaign from radio to hard X-ray energies of the prominent gamma-ray blazar 3C 279 during the first year of the INTEGRAL mission. The variable blazar was found at a low activity level, but was detected by all participating instruments. Subsequently a multifrequency spectrum could be compiled. ... In addition, this 2003 broadband spectrum is compared to one measured in 1999 during a high activity period of 3C 279. | ...

... According to theoretical calculations, this effect can be measured by observing PSR B1937+21 for four hours. The measured magnitude and frequency dependence of the HI resonance delay will complement measurements of the HI optical depth thus giving us more information about HI clouds in the ISM than can be obtained from optical depth measurements alone. Students involved in the Arecibo Remote Command Center at UT Brownsville will be involved in the observations and data analysis. ...

... Team . ... All the results we present were obtained with the SCORPIO instrument mounted at the 6-m telescope of SAO RAS. TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1090 SUBJECT: GRB001109, Host Galaxy Spectroscopic Observations DATE: 01/09/08 07:28:47 GMT FROM: Vladimir Sokolov at SAO RAS <sokolov@sao.ru> . ... TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1092 SUBJECT: GRB001109, Host Galaxy Astrometry DATE: 01/09/11 08:19:24 GMT FROM: Vladimir Sokolov at SAO RAS <sokolov@sao.ru> . ...

... Polish scientists at the Space Research Centre, Polish Academy of Sciences, in Wroclaw, south-west Poland, have constructed an instrument called SphinX (short for Solar PHotometer In X-rays), which is an X-ray spectrophotometer, that will obtain spectra in the energy range 0.5--15 keV in 256 energy channels with frequency of up to 100 times a second. ... SphinX is part of a package of instruments known as TESIS (PI Prof. Sergei Kuzin, Lebedev Institute, Moscow). ... Space Research Centre, . ...

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 . ...