... 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. ...

... subroutine atthkgen * get ODF * get start and end times of complete observation * open output fits file * loop through time (timestep) set attitudeFromAhf to true + call OAL_getAttitude ( get AHF attitude ) set AHF info to OAL_getAttitude info (or to NULL if bad) calculate summed attitude information for AHF set attitudeFromAhf to false + call OAL_getAttitude ( get OM ...

... Correcting ETC Calculations of CCD Spectral Observations for CTE Effects . ... HST Overview . Overview . ... Post-Observation . ... ETC . ... ID: CL Script for Applying CTE Loss to Output of Spectroscopic ETC . ... However, the STIS ETC calculations do not incorporate these CTE effects as yet. ... The output from this script should then be used to calculate the appropriate input flux level for a second run of the ETC, which will then yield output which is corrected for the CTE effect. ...

... Basic Observables: Zero-differenced phase and code ionosphere-free combinations of global GNSS network stations, corrected by P1-C1 satellite code biases (cc2noncc), daily observations with 30 seconds sampling rate Sites coordinates : IGb08 reference frame coordinates and velocities Displacements: solid tides, ocean loading, pole tide loading (IERS 2010) Geometric model : Receivers antennas eccentricities, absolute receiver and ...

... 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: . ...

The beam pattern and the polarization characteristics . of the radio telescope RATAN-600 . The Mueller matrix elements was computed via formulas [1]: . ... The BP were computed by the aperture method, proceeding from the fild distribution in the aperture of the primary mirror. The components of the main and cross-polarization components of the electric field in the vertical aperture of the primary mirror was computed in Frenel diffraction approximation. ...

Alfa_ang is a GUI for the rotang routine. The purpose of this routine is to calculate the optimum rotation angle for ALFA given the RA and Dec of a source and the date and time of the observation. The routine also returns the azimuth and zenith angle of the telescope at the requested time, thus it can be used to find the correct rotation angle and azimuth for the Fixed Azimuth Drift Scan observing mode used by the AGES drift precursor observation. ... To run alfa_ang at Arecibo: . ...

... Parasitic polarization effects in RATAN-600 solar observations . ... We report the results of numerical simulation of parasitic circular polarization as observed by RATAN-600 operating in the "Southern Sector with a Flat Reflector" mode. ... We estimate the differences between R and L polarization beam pattern of the telescope and compute M11 and M41 for the case of observation of R and L polarization at different points of the focal line. ...

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. ...

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... Lightcurve of HW Vir from images obtained using the Faulkes Telescope South, operated by Las Cumbres Observatory . The blue triangles show the difference between two stars whose brightness is constant. ... This shows the value of the Faulkes Telescopes in the follow-up observations of eclipsing binaries with the aim to detect and characterise additional circumbinary companions. ...

... Categories: calibration GPDOF estimates the likely error in a calibration solution, by calculating the errors in the "Degrees-of-Freedom" (dofs) of an interferometer. This is useful for calibration of high-precision circular polarization observations. ... Finally, GPDoF calculates the std and standard error of the derived dofs, which you can use to estimate the errors in the Stokes V of a target observation. ... GPDoF estimates the std and standard error in the dofs. ...

Next: Polarization efficiency: size/shape/orientation effects Up: Optical properties of cosmic Previous: The 2175? feature . To model the interstellar polarization one needs to calculate the forward-transmitted radiation for an ensemble of non-spherical aligned dust grains. ... Let non-polarized stellar radiation passes through a dusty cloud with a homogeneous magnetic field. ... The angle between the line of sight and the magnetic field is ( ). ... where the angle is connected with and ( ). ...

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? ...

... Time calculated from Fermi GBM Trigger Time = 14:12:08.67 ( Connaughton, GCN 9230 ). 1% coincident with our start zero image time. 3x3 degrees around Swift XRT position . ... SUBJECT: GRB 090424 : MASTER-Net prompt optical limit DATE: 09/04/25 20:29:42 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski ... Our observations results: ---------------------------------------------------------------------- Fermi GRB Trigg.* ...

Abstract -- Calculations are performed for the linear polarization of starlight due to extinction by aligned dust grains when the starlight traverses a medium with irregular magnetic fields. This medium is intended to represent the optically thick components of interstellar clouds which are observed to make little, if any, contribution to the polarization of starlight. ...

... 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 . ...

... Up: Description of program searchdup Previous: Program use . Input records are ordered per date of observation, and the list of known (observed) sources is cleared. Each record is compared in position to all the known sources. If the sky distance is less or equal to the specified one, the record is added to the list of observations for that source. If no known sources are within the specified radius, a new source is created, with the coordinates of the observation record. ...

We present the results of our observations of the white-light corona in polarized light performed at Criciuma eclipse, Brazil. During the observation of 3.11.94 we have made five couple of pictures of the solar corona in polarization light. ... Koutchmy S., Molodensky M., Starkova L., Ershov A., Matsuura O .: ... Molodensky M., Starkova L., Koutchmy S., Ershov A .: ... Koutchmy S., Molodensky M.M., Starkova L.I . ... Koutchmy S., Molodensky M.M., Starkova L.I. Koutvitsky V. and Ershov A . ...

Geomagnetic storms and substorms are a natural hazard similar to hurricanes, floods etc. ... Solar and geomagnetic activity also probably influences the Earth's climate and human health. ... Under southward directed IMF the Earth's magnetosphere is open to input from the solar wind flow. ... Since practical importance of solar wind measurements was recognized, a number of approaches was developed for prediction of the geomagnetic activity basing on the solar wind data. ...

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 ...