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. ...

. XMM-Newton Science Analysis System . testodf (testodf-0.45.1) [xmmsas_20070708_1801-7.1.0] . Meta Index / Home Page / Description . This test ODF is an observation of a point source that is placed on-axis, and whose spectrum consists of 30 lines. Each line has a Gaussian profile; the width is 1/100th of the energy of the center of the peak. This source is observed with all instruments in their 'default' configuration during 10 ks. XMM-Newton SOC/SSC -- 2007-07-08

Next: Summary of reduction Up: Echelle Reduction Previous: Saving the Data . In the present version we will be concerned with the standard configuration of CASPEC, the Cassegrain Echelle Spectrograph which is in operation at the Cassegrain focus of the ESO 3.6 m telescope. ... In its standard configuration CASPEC uses a a 31.6 lines/mm echelle grating together with a 300 lines/mm grating cross disperser. ... The table shows the change in resolution with the order number. Table: Resolution . ...

... The FOS employed one of six basic data taking modes to acquire science data: . Spectrophotometry (ACCUM). ... Image. ... ACCUM was by far the most commonly used observing mode. ... In IMAGE mode observations both the number and length of rasters and the y- position of each raster could be specified, so that: 1) a white-light image of all or a portion of the aperture was possible with the MIRROR, and 2) spectra from different portions of the aperture were sampled with a disperser. ...

... 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 . ...

... Up: Proposal Processing . ... ESO is prototyping a distributed ``Phase II'' system that will allow astronomers to prepare their observations at their home institutions, while maintaining a central repository for all observation data. ... ESO is developing a Phase II Proposal Preparation system (P2PP) to collect detailed scientific programme descriptions, in the form of observation blocks (OB). ... ESO's Phase II Proposal Preparation system is an integral part of the VLT Data Flow System (DFS). ...

... Description(Russian): [ HTML ] [ PDF ] . ... 2002 : source L A T E X and export to [ HTML ], [ PDF ], [ PS ], [ OpenOffice ], [ MSWord ] . 2003 : source L A T E X and export to [ HTML ], [ PDF ], [ PS ], [ OpenOffice ], [ MSWord ] . 2004 : source L A T E X and export to [ HTML ], [ PDF ], [ PS ], [ StarOffice ], [ MSWord ] . 2005 : source L A T E X and export to [ HTML ], [ PDF ], [ PS ], [ StarOffice ], [ MSWord ] . ... 2014 : source HTML and export to [ PDF ], [ MSWord ], [ ODT ] . ...

... They are concerned with Attitude Control System of the spacecraft, satellite visibility from tracking stations, limits on the satellite autonomous operations during the orbit, and needs for auxiliary operations with the spacecraft. ... Among the operational constraints the most important one is the number of programmed slews per orbit, which determines the maximum number of radio sources to be observed during one orbit. ... System temperature (K) . ... Progress of the RadioAstron Project in Pictures...

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. ...

... 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. ...

. Statistics of sunspot activity . The sunspot indices . My observations . NGDC's observations . The solar regions . Links . About authors . Russian pages . The solar regions . NOAA 11300's . NOAA 11200's . NOAA 11100's . NOAA 11000's . NOAA 10900's . NOAA 10800's . NOAA 10700's . NOAA 10600's . NOAA 10500's . NOAA 10400's . NOAA 10300's . NOAA 10200's . NOAA 10100's . NOAA 10000's . NOAA 09900's . NOAA 09800's . NOAA 09700's . NOAA 09600's . NOAA 09500's . NOAA 09400's . NOAA 09300's .

... 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. ...

... The schedule assigned id (example: AS05) for your observing program. ... Use the time you started using the telescope including when you started taking calibrations. The time you opened for on sky observations can be entered later in the activity log. UTC End Time: . ... Focus Log: . ... The focus position can be obtained under the Telescope column of the System Status in ACP or from the run log. ... When all fields are filled out press this button to email the log to the ARCSAT and community. ...

... GSAOI Home . Instrument . ... Other Links . NIR Camera Links . NIR IFU Spectrograph Links . Other NIR Spectrograph Links . NIR Instruments by Observatories . NIR Survey Links . Mid-Infrared Instrument Links . ... NIRI on Gemini . ... ISAAC on the VLT . ... Omega-Prime from MPIA, Heidelberg . ... IRCAM3 on UKIRT (InSb) and here . UFTI for UKIRT ( pictures ; UKIRT links here; ; and here ) . ... Gemini instrumentation . ... UKIRT instrumentation ( Future Instruments ) . ...

... Meade Instruments Corporation . ... Refracting telescopes (Meade Models NG-60, NGC-60, DS-2070AT, ETX-70AT, LXD55-AR5, LX55-AR6 ) and mirror-lens telescopes ( ETX-90AT, 105AT, 125AT, LXD55-SC8, 8LX90, LX200 GPS Series ) are generally more versatile in a wide array of land and astronomical applications. ... The intermediate-level observer, or the non-casual telescope user who wishes to purchase one telescope for a lifetime, should consider a Meade Model LXD55 series, 8LX90, or LX200GPS. ... Meade 4M ...

... Click on an object in the solar system or choose from the list at left to learn more . The Arecibo Observatory planetary radar is the world's most powerful instrument for post-discovery characterization and orbital refinement of near-Earth objects. ... The Solar System Studies group is a department of the Arecibo Observatory, which is an NSF facility operated under cooperative agreement by SRI International, Universities Space Research Association (USRA), and la Universidad Metropolitana (UMET). ...

... The x-ray spectral analysis consists of a comparison between the observed pulse height spectrum and a pulse height spectrum calculated using a given spectral model. ... To obtain the spectral parameters for an x-ray source, several steps need to be followed. For each source: . ... obtain the best fit parameters for a spectral model - repeated for each model of interest . obtain a 1-D or 2-D grid of values around the best fit values - this can be done for as many models as desired . ...

... Iowa Robotic Telescope | ... Talon is based on OCAAS, a software suite developed by software engineer Elwood Downey ( Clear Sky Institute ) for use at the University of Iowa ?s first remote facility (the ATF, or Automated Telescope Facility). ... XObservatory : Telescope Control Interface . ... This program calls upon and coordinates much of the interrelated portions of the Talon architecture, and forms the primary control panel for the telescope, dome, and peripheral systems when used locally. ...

... The low energy plasma composition spectrometer AMEI-2 is built to be able to find in the low energy range of the phase space (E, q, j) and separate the fluxes of the major ion species in the magnetotail - H+, He++, He+ and O+, and analyse their energy and angular distributions. ... Electrostatic angular scanning in one direction and the use of the spin of the satellite to sample the other angle give the ability to measure 2-D distributions for each ion specie several times per spin. ...

GRANAT is the Russian x-ray sattelite launched to the high apogee orbit (200,000 km) and operated almost for 10 years (1989 -1999) , carrying out four major instruments: French SIGMA coded-mask hard x-ray telescope (30-1000 keV), Soviet ART-P coded-mask telescope (2??-60?? keV), all-sky monitor WATCH (6-150 keV), and a gamma-burst detector PHEBUS . ... Since September 1994, GRANAT is in the survey mode. ... Explore pages devoted to individual GRANAT instruments (including main scientific results): . ...