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 . ...

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• Examples of GHRS Phase II Proposals
• Phase II Example: NICMOS Parallel Observations
• Introduction to Special Requirements:Syntax and Rules

... 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. ...

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• Parallelization of Widefield Imaging in AIPS++
• Constructing and Reducing Sets of HST Observations Using Accurate Spacecraft
• ADASS 2003 Conference Proceedings

... 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: . ...

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... Observation codes for VSOP General Observing Time observations have the form . ... The first letter indicates which AO period the observation was proposed in: the letter `v' indicates the first AO period, and the letter `w' indicates the second and third AO periods. The three digits indicate the proposal number. ... For proposals with more than 26 experiments (see next item), 300 is added to the proposal code for the 27th and subsequent experiments. ...

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• casacore: casa::MSObservationIndex Class Reference
• VLA-Only Project Example
• Example FITS WCS files

... Here follow some typical calls to epchain : epchain This processes the first IMAGING mode exposure (i.e. PNS010) and is equivalent to one of the calls epchain datamode = IMAGING odfaccess = odf exposure =010 schedule=S epchain datamode = IMAGING odfaccess =oal exposure =1 epchain datamode = IMAGING exposure =1 epchain odfaccess =name ... The call epchain datamode=ALL odfaccess=all will process all exposures of an ODF, independent of observing mode. ...

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Pulkovo NEO Page . ... NEA Accuracy Estimation . ... The estimation of accuracy of the current CCD observations of asteroids and comets is constantly performed at Pulkovo Observatory. ... The (O-C) values, so called "Observed" minus "Calculated" positions, characterize numerically the observations of any observatory, both professional and amateur, during a short period (one or several close nights). ... So the (O-C) values for these objects nearly entirely define the errors of observations. ...

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• Pulkovo NEO Page: Ephemeris Support
• Pulkovo NEO Page: Estimation of Observational Accuracy
• Pulkovo NEO Page: Observations

. First page Back Continue Last page Summary Graphics .

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• Example Observing Projects
• Alfa_ang - IDL procedure for calculating the optimum rotation angle for ALFA

... LEDA has been the first Extragalactic Database. ... select pgc, objname, al2000, de2000 where de2000 > 76 and al2000 < 1 . select pgc, galaxy_name, al2000, de2000 where de2000 > 76 AND al2000 < 1 . ... For each parameter the method of the calculation (or the definition) is given in the Third Reference Catalogue (de Vaucouleurs et al., 1991) and/or in Paturel et al. (1997) and/or in some additional references given below. ... de Vaucouleurs et al., 1991, 1997 . ... 1995 ; Paturel et al., 2000 . ...

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• An example of a Classification Process
• The Data Organizer
• An example of selection criteria

... This thread uses PINTofALE to generate a simulated Chandra spectrum. ... define a DEM . ... pset marx .par ExposureTime=50000 OutputDir='sim_ marx ' \ ; GratingType='NONE' DetectorType=' ACIS-I ' SourceFlux=-1 \ ; SpectrumType='FILE' SpectrumFile='spec_ marx .dat' \ ; SourceType='POINT' DitherModel='INTERNAL' ; marx TSTART=2006.46 ; marx2fits sim_ marx / spec_ marx .evt ; dmextract infile= spec_ marx .evt[EVENTS][(x,y)=circle(4018,4141,10)] ; [bin pi=1:1024:1] outfile= spec_ ...

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• The AstroStat Slog aneta
• An Example - 3C 120
• An example of a typical timing analysis

... grep -s keith > /dev/null then echo keith is logged in else echo keith not available fi . This lists who is currently logged on to the sytem and pipes the output through grep to search for the username keith . The -s option causes grep to work silently and any error messages are directed to the file /dev/null instead of the standard output . If the command is succesful i.e. the username keith is found in the list of users currently logged in then the message keith is logged on . ...

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ASTRONOMICAL YEARBOOK for 2006 (in Russian) . Preface . In the тАЬAstronomical YearbookтАЭ (AY) the ephemerides of the Sun, Moon, major planets and stars computed with the maximum precision in accordance with the resolutions approved by the International Astronomical Union (IAU) are published. ... N.I. Glebova, M.L. Sveshnikov; . ... N.I. Glebova; . ... The data control of the different part of the Yearbook was carried out by N.I. Glebova, N.K. Omelyanchuk, and I.A. Lebedeva. ... N.I. Alehina. ...

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• AY2008 (preface)
• AY2011 (preface)
• AY (preface)

... The experience of determination of the link between radio sources and dynamical reference frames is presented. To obtain this connection we used a series of very long baseline interferometry (VLBI) observations of the spacecraft Phobos-2 and angularly nearby quasars. ... The dynamical reference frame is determined by equator and equinox of these ephemerides. ... References . ... The relative orientation of the radio and dynamical reference frames can be described by a sequence of three rotations . ...

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• De-convolution of a Gaussian beam from planetary observations Bojan Nikolic web
• Computing dispersive atmospheric delay with AATM
• High-frequency Radio Continuum Observations of Giant Radio Galaxies

This diagram shows the six superimposed "layers" of the CSS table model. This diagram illustrates the algorithm for calculating a cell's final background. ... The diagram shows how, looking down on the six rectangles, one may compute the background color of each cell. ... A cell without a background color in the top layer is depicted as a "window" onto the lower layers, which give its final background color. ...

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• Long description of example illustrating background calculation
• Long description of example illustrating table row height calculations and
• Long description of float and text flow example

Determination of short-term proper motions of fast stars with Pulkovo Normal Astrograph. ... Khovritchev Laboratory of Astrometry and Stellar Astronomy of the Pulkovo Observatory, RAS, Saint-Petersburg Observations Normal Astrograph (D/F=33 cm/3.5m), CCD camera: S2C, FOV = 18x16 arcmin, Pixel size 900x900 mas Determination of the new proper motions of 413 LSPM stars 1 epoch : CCD-surveys and catalogs -- M2000, CMC14, 2MASS, SDSS DR7 2 epoch : CCD-observations with the ...

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• http://www.puldb.ru/nikolaev_2011/PUB_NIKOLAEV_2011/damian.pdf
• http://www.puldb.ru/nikolaev_2011/PUB_NIKOLAEV_2011/plates2.pdf

. (Data examples) . Russian . 4/03/1997 21:00 GMT . Image with coastal line and coordinate grid overlayed . (image size 784x521) . 6/03/1997 21:00 GMT . Image with coastal line and coordinate grid overlayed . (image size 512x512) . Moon disc captured by GOMS . (image size 1024x1024) . For information send a mail to: admin@planeta.rssi.ru . All rights reserved. ? 1997-2002 SMIS IKI RAN and SRC PLANETA, Moscow, Russia.

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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. ...

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• ESO - Historic examples of ESO-developed technologies
• ESO - Examples of ESO developments that have been used for other similar
• Plot data from the WDS

Taking into account the result by Watanabe P=2.5 days in outburst, I reconstruct old set of photographic observations being partly lost, and add some new observations. ... The periodogram calculated with the method by Lafler and Kinman is shown. ... The last periodogram indicates peaks corresponding following possible periods with the double-wave light curve: 0.4236, 0.4650, 0.5379, 0.6064, 0.7365, 0.871, 1.168, 1.5437, 2.8173, and 6.89 days. ...

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• Fabry-Perot Interferometer: Data cubes
• Emission molecular bands
• shmidt_e

.

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• Astronomy HyperText Book
• Lecture XVII.
• CCD Astronomy Magazine Article Page 4

Databases (NSDC) of the Natural Planetary Satellites. ... NSDC: Database of astrometric observations of Natural Planetary Satellites . ... They are thoroughly looking for observations in different sources, creating their owndatabases which are then mostly inaccessible to other researchers. ... In the file "content" with explications, the reference is given to the data source as well as the bibliographic reference. ... Data sources. ... Why a specific bibliographic database for Natural satellites? ...

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• Data bases of Natural Satellites. Documentation. Sources
• IDL programs
• Y.Kupryakov, SAI, MSU

... 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