... The HST uses an onboard model of its orbit to perform in real-time various control functions relating to spacecraft operations and observation support. ... New coefficients for the ephemeris are updated every other day, and are archived as FITS keywords for each HST observation data set. Using these coefficients,an observer can perform a variety of calibration and characterization calculations relating to the orbital position and velocity of the telescope. ...

... 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. ...

Next: XMM_MISCDATA Up: CCF Components Previous: Appendix: List of valid Contents . While some relevant RGS calibration data are given in the general-purpose CCF components . ... Some information concerning the maintenance of RGS CCF files is given below, though more details are available in the release notes that accompany new file releases and other technical notes. ... Use of CCF components by RGS SAS tasks . ... Purpose . Functionality . Ground calibration . Maintenance procedures . ...

Circumstances of (99942) Apophis, approaches to the Earth in 2029тИЪ2036 . ... In so doing we consider A2 component of additional acceleration in orbital coordinate system, which is present in many near-Earth asteroids and some small main belt asteroids, as a manifestation of Yarkovsky effect. ... It means that Yarkovsky effect does not serve to increase the collision probability in 2036. ... asteroid Apophis, collision with the Earth, the Yarkovsky effect. ...

Next: Examples and Photometric Up: Image Restorations of High Previous: Introduction . ... where is the intensity of the point sources (mainly zero apart from -functions at the positions of designated sources) and is the intensity of the background. ... When is zero the objective function becomes the same as that of the standard Lucy-Richardson technique. takes the form of an entropy expression which may be calculated in two ways, relative to a flat background: . ...

Next: Results and discussion Up: Observations and data reduction Previous: Reduction of photometric data . ... Since HS 0822+3542 had a known optical redshift, we split the 1024-channel autocorrelator in two halves and used a dual-polarization receiver to increase the S/N ratio. ... 0.077 0.005 . ... 0.004 0.003 . ... 0.005 0.004 . ... 0.005 0.04 . ... 0.49 0.03 . ... Next: Results and discussion Up: Observations and data reduction Previous: Reduction of photometric data Labaratory "Structure" . ...

... Radio emission at around 90 GHz from star-forming galaxies is expected to be strongly dominated by the free-free component due to ionising radiation from massive, short-lived, stars. We present high surface-brightness sensitivity observations at 90 GHz of the nearby star-forming galaxy Messier 66 with resolution of about 9 arcsec (corresponding to a physical scale of about 500 pc) and analyse these observations in combination with archival lower frequency radio and mid-infrared measurements. ...

... 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 ...

... The PSF image (after tapering/weighting) and weights image. ... Directory listing: total 145G -rw-r--r-- 1 whi550 at-astro 534M 2010-12-11 23:22 ASKAPsim.FLASH.cont.catalogue.dat - rw-rw-r -- 1 whi550 at-astro 50M 2010-12-10 15:10 ASKAPsim.FLASH.cont. image .restored.fits - rw-rw-r -- 1 whi550 at-astro 50M 2010-12-10 15:10 ASKAPsim.FLASH.cont.imagemodel.fits - rw-rw-r -- 1 whi550 at-astro 127M 2010-12-14 10:15 ASKAPsim.FLASH.cont. model .input.fits - rw-rw-r -- 1 whi550 ...

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. ...

Peremennye Zvezdy", . ... Star Name: . GSC 3710-00312, USNO-A2.0 1425-04252279 . ... Variability type: . ... USNO-A2.0 1425-04252279 is located at the distance of 15?.7 from the X-ray source 1RXS J031707.9+572942, which is larger than the position error of the source (12?), but its hardness ratio HR1 = 0.03 0.29, typical of chromospherically active stars, and its character of variability allow us to assume that the star is related to the X-ray source. ... Eclipsing variability . Sine wave 1 . ...