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1. HDF-S Observing Strategy
Discussions about the observing strategy for the HDF-S focussed primarily on the questions: . What filters/gratings to use for each instrument ? What exposure time to use for each filter/grating ? ... Different areas of the Version 1 output image correspond to variable amounts of exposure time, due to the relatively large pointing shifts necessitated by the multi-instrument observing strategy. ... WFPC-2 Filters, exposure times and limiting AB magnitudes for Version 1 images . Filter . ...
[ Сохраненная копия ]  Ссылки http://www.stsci.edu/ftp/science/hdfsouth/obs_strategy.html -- 10.0 Кб -- 24.05.2000
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2. VLTI Calibrator Selection Help Page
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. ...
[ Сохраненная копия ]  Ссылки http://www.eso.org/observing/etc/doc/helpcalvin.htm -- 13.1 Кб -- 10.04.2016
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3. ETCs and Observations Simulation at the VLT
... Second, the observatory can control the configuration, test data analysis procedures, and provide calibration solutions with the help of instrument models. This paper presents the VLT object-oriented framework for the development of ETCs (Exposure Time Calculators) and data simulators. ... Instrument simulations are being developed for the purpose of predictive calibration, instrument configuration control, and evaluation of data analysis procedures. ...
[ Сохраненная копия ]  Ссылки http://www.adass.org/adass/proceedings/adass99/P1-22/ -- 12.4 Кб -- 09.10.2000
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4. Multipoint correlations of the solar wind parameters observed by several
The problem of solar wind data correlation for the observations onboard several spacecraft is very important for three points of view: . ... This problem is studied now in detail by systematic determination of ion flux and ion velocity data correlations by INTERBALL-1 (IKI group), WIND and IMP 8 (both - MIT group). ... Solar wind plasma correlation lengths from IMP 8, WIND and INTERBALL-1. ... Correlation of solar wind observations onboard several spacecraft: INTERBALL-1, IMP 8 and WIND data. ...
[ Сохраненная копия ]  Ссылки http://www.iki.rssi.ru/tail/results/vdp/correla.html -- 5.6 Кб -- 21.01.1997
[ Сохраненная копия ]  Ссылки http://www.cosmos.ru/tail/results/vdp/correla.html -- 5.6 Кб -- 21.01.1997
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5. Making a Fake Observation
... The Miriad task uvgen can be used to simulate a variety of observing modes. ... Simulating a telescope approximately, let alone in some detail, requires a good many parameters. uvgen takes an appreciable number of parameters and input files to describe the telescope, correlator and source. Fortunately keyword and set-up files for some common situations exist ( e.g. simulating the ATCA and VLA). ... For example, to load typical parameters for the ATCA, use miriad% source $MIRCAT/uvgen.def.atca . ...
[ Сохраненная копия ]  Ссылки http://www.atnf.csiro.au/computing/software/miriad/userguide/node56.html -- 12.7 Кб -- 10.04.2016
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6. VISTA ETC - Exposure Time Calculator
... 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. ...
[ Сохраненная копия ]  Ссылки http://www.vista.ac.uk/observing/etc/index.html -- 15.1 Кб -- 28.03.2013
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7. Submitting New Observing Modes to AO
The Arecibo telescope is a versatile instrument with multiple receivers, backend processors, and telescope scanning modes. ... Observing modes are implemented at Arecibo through the Control Interface Module for Arecibo (CIMA). ... In this case, the observer is encouraged to submit a proposal for a new observing mode. ... Proposals for new observing modes will be evaluated by a technical review panel consisting of Arecibo technical and scientific staff. ... Flow chart. ...
[ Сохраненная копия ]  Ссылки http://www.naic.edu/~astro/Modes.shtml -- 6.5 Кб -- 01.10.2012
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8. Description
... The SF does not contain all the information required to process the ODF with the SAS. odfingest extends the SF with data extracted from the instrument housekeeping data files and the calibration database. It creates a new summary file: the SAS ODF Summary File (SOSF). ... The user need not have write access to the ODF directory. odfingest uses the parameter outdir to learn where to write the SOSF. ... Alternatively, the name of the SOSF can be passed to odfingest with the parameter summaryfile . ...
[ Сохраненная копия ]  Ссылки http://xmm.vilspa.esa.es/sas/8.0.0/doc/odfingest/node3.html -- 8.5 Кб -- 01.07.2008
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9. Procedures for Observations
... 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. ...
[ Сохраненная копия ]  Ссылки http://www.arcetri.astro.it/irlab/instr/longsp/doc/proc_ob.html -- 7.9 Кб -- 16.02.2000
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10. Session Parameters
Next: The Reduction Session Up: Echelle Reduction Previous: Standard orientation . ... The command SHOW/ECHELLE displays only those parameters which must be set according to the options and methods chosen for the reduction. ... Current parameters are saved with the command SAVE/ECHELLE name , where name is the session name. ... Current parameter values are set to the default value with the command INIT/ECHELLE , or set to the values of a previously saved session with INIT/ECHELLE name . ...
[ Сохраненная копия ]  Ссылки http://www.sao.ru/precise/Midas_doc/doc/95NOV/vol2/node468.html -- 5.4 Кб -- 23.02.1996
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11. The spectrograph design and the observing procedure
... The choice of the spectrograph design (Fig.2) is determined by the quantity R, the overall dimensions of the PF cage and the restrictions on the rigidity of the structure of the device. ... As the camera's objective a fast 4-lens aplanat is used having a focal distance F cam =140 mm and a relative aperture of 1:1.8, the resolution at the centre is no less than 80 gr/mm, that over the field at a distance of 3 mm from the edge along the frame ( ) diagonal is 35 gr/mm. ...
[ Сохраненная копия ]  Ссылки http://mavr.sao.ru/hq/ssl/PFES/node4.html -- 10.4 Кб -- 02.10.2012
[ Сохраненная копия ]  Ссылки http://www.sao.ru/hq/ssl/PFES/node4.html -- 10.4 Кб -- 01.10.2012
[ Сохраненная копия ]  Ссылки http://jet.sao.ru/hq/ssl/PFES/node4.html -- 10.4 Кб -- 01.10.2012
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