Next: Amplitude Distribution Previous: Gravitational Wave Background from . To get rid of the extragalactic GWB produced by binaries, one can use the above considerations to find the optimal detector halfwidth and frequency for observations. ... for the flat red end of the GWB, and . ... Equating to unity, one finds the critical detector halfwidth . ... In contrast, by observing the sky with a GW detector with a narrow enough halfwidth , one will not ``see'' the extragalactic GWB at frequencies . ...

... A SPYBAL is executed to center the spectrum in the cross-dispersion (or GHRS ydirection) on the diode array. ... A SPYBAL actually produces science data consisting of a wavelength calibration exposure. ... This means that as long as the grating does not change, no new SPYBAL will be inserted, unless one has several exposures and the total alignment time (not real orbital time) exceeds 90 minutes. ...

Next: Correlator Products . Previous: RSOG Post-Observation Products . ... Merged Correlator Input Log . Calibration and Flag files . SRT Amplitude Calibration Data . ... Phase Calibration (PCal) Data . ... DPC to Correlators . What: The RSOG produces the `merged' correlator input log file based on the Data Processing Logs supplied by the GTSs and on Executed Sequence of Events supplied by GOCG to produce a single correlator input log for all the GTSs for each observation. ...

... Radio telescope interferometers exhibit chromatic aberration effects. ... Reduction packages such as AIPS and AIPS++ will produce a beam pattern image for each frequency channel. This allows these packages to compute a spectral-line cube which has a pixel size (cellsize) independent of frequency. ... Because of this, Miriad produces cubes where the pixel size changes with frequency. ... The correct approach is to produce a cube in Miriad which does not have a variable pixel size. ...

... News Latest News News Archive Newsletter Quarterly Status Report . ... Data Analysis SAS News What is SAS? ... Other Links Project Related Links Research Projects Other X-ray Missions Space Weather Links . This page contains links to four sorted lists of observations planned or performed as of 12 March 2003. ... Planned Observations (sorted by type. ... Planned Observations (sorted by RA/DEC) . Performed Observations (sorted by RA/DEC) . Planned Performed Observations (sorted by RA/DEC) . ...

... 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. ...

Next: An On-the-fly Calibration Pipeline for the HST WFPC-2 using OPUS . ... An Astrometry Data Processing Pipeline has been developed and deployed at the Space Telescope Science Institute (STScI). This pipeline is responsible for producing Hubble Space Telescope (HST) Astrometry Data Sets used to analyze astrometry observations and the operation of the HST Fine Guidance Sensors (FGS). ... This application is used in scenarios where complete astrometry data sets could not be produced. ...

Detected Supernovae . The search have produced till now the detections of 4 SNe. ... This result highlights the power of infrared monitoring in detecting Obscured SNe and indicates that optical surveys are probably missing a significant fraction of SNe, especially in obscured systems such as starburst galaxies. ... In Fig. we show the archival SOFI image of NGC3256 (left) and the first image obtained in 2001 (right) where SN2001db has been detected. ...

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Peremennye Zvezdy ( Variable Stars ) 35 , No. ... We present the results of our new observations of QS Draconis, a recently discovered double-mode high-amplitude Scuti variable, HADS(B) type. ... Our CCD observations in the Johnson bands were performed at the Tien Shan Astronomical Observatory of the V.G. Fesenkov Astrophysical Institute, at the altitude of 2750 m above the sea level. ... The finding chart (Fig. 1) identifies the variable star, comparison star, and check star. ... Fig. ...

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 . ...

... Moscow State University, Sternberg Astronomical Institute . ... Moscow State University, Sternberg Astronomical Institute, Cremian Laboratory . Dr. Vladimir Amirhanyan - Soft, Radioobservations, Interpretations . Sternberg Astronomical Institute . Aleksandr Belinskiy - mechanics, soft, observations, interpretation . ... Mikhaylo Kuznecov - mechanics, soft, observations, interpretation . ... Moscow State University, Physics Department . ... Gleb Antipov - observations, interpretation . ...

... Observation pre-processing consists of standard bias, dark and flat-field corrections. The package provides different commands to average images, extract sub-images or normalize flat-fields. General information related to preprocessing commands is available in the section Dark, Bias and Flat-Field of SHOW/LONG and can be obtained by: . ... The command PREPARE/LONG extracts sub-images. ... The command processes a catalog by default or an image if the name is provided with the extension .bdf . ...

Pulkovo Database of Observations of Visual Double Stars . ... Catalog of relative positions of visual double stars, based on photographic observations performed since 1960 in Pulkovo on the 26-inch refractor (A.A.Kiselev, O.A.Kalinichenko, O.V.Kiyaeva, N.A.Shakht, L.G.Romanenko, I.S.Izmailov, O.P.Bykov, K.L.Maslennikov, E.A.Grosheva, D.L.Gorshanov), 2010 . ... Enter either ADS or WDS number. Click here to display full list of visual double stars observed at Pulkovo. ADS . ...

... We give evidence that lower pressure model chromospheres can alos reproduce the Balmer line profiles, but give Lyman surface fluxes overestimated by more than an order of magnitude. ... We obtain the Paschen lines in emission and Paschen decrements as large as 41 for Pa$_{\beta}$. ... Formation of all Hydrogen series is collisionally controlled and takes place in a rather thin layer at the top of the chromosphere (Balmer, Paschen, and Brackett) or in the transition region (Lyman). ...

... These partially reduced images of the Pleiades were taken by WISP using its longer-wavelength (2180 ) UV filter. Point-spread functions (PSFs) of the brightest stars have been removed to reveal much of the inner reflection nebula, both in a centralized diffuse glow and in the nebulosity south of Merope, the bottom star in the Pleiades ``bowl''. The PSF removal process was improved since these images were produced. Better ultraviolet images can be found here . ...

. Observations performed with the Australia Telescope Compact Array produced this radio image, at wavelength 7mm, of the remnant of Supernova 1987A. // ICRAR

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. ...

... 8, ``Celestial Mechanics'', 2002 Estimation of masses of some minor planets from observations of perturbed bodies O. M. Kochetova Institute of Applied Astronomy, St. Petersburg, Russia The most straightforward method of mass determination of minor planets is the dynamical one which uses the gravitational perturbations produced by minor planet in the motion of other bodies. ... The values of the masses of minor planets (15), (29) and (65) appear to be rather close in both papers. ...

... A radio galaxy is a galaxy that emits an unusually big amount of energy at radio wavelengths. ... Inside of each galaxy with an active nucleus (radio galaxies are among them) there must be a system of a "central machine" responsible for the colossal amount of the emitted energy from radio to gamma ranges. ... Sometimes a radio source in an active galaxy may flare again if the needed conditions appear (a new portion of matter would fall into the furnace of the "central machine"). ...