... HST . ... HST Overview . ... Phase I Proposing . ... You will need to allow time for an acquisition in virtually all cases. ... If the STEP-TIME you need to get 100 or more counts in the peak pixel exceeds about 2 seconds then you have a faint-target acquisition, and you should use the longer time on the Phase I work sheets. ... In either case you must allow for more time for the acquisition because internal calibrations of the mirror locations take longer (because they reflect less light). ...

... A further spin off of this project is that more reliable pointing information for all exposures is provided. In 1995 the ST-ECF introduced, along with the CADC, the re-calibration on-the-fly (OTF) of archived HST exposures. ... By correlating the HST Mission Schedule and the time-tagged engineering telemetry data stream downloaded from HST it is possible to reconstruct with great accuracy the pointing sequence of any given scientific observation. ... taken within the same HST visit . ...

... The procedure simply observes ON your source for x minutes and then takes a `blank sky' observation OFF your source for the same amount of time and tracking the same azimuth and zenith angle range. ... If your scans are for 5 minutes or less, your wait time should be set to 1 minute (the default setting). ... 2 (scan duration) + (slew time) + (calibration time) A 5 minute ON/OFF + 10s CAL takes 11.3 minutes. A 7 minute ON/OFF, (which has a 2 minute slew time plus a cal) takes 16.3 minutes. ...

Next: GOCG Post-Observation Products . ... Reconstructed Orbit . JPL MMNAV Reconstructed Orbit . ... The JPL MMNAV files will be made available on the JPL MMNAV FTP site in directory [RAstron.ODDATA.JPLICV.TRACK] (note the capital letters). back to top . ... What: X-band Doppler tracking data will be transmitted in near real-time from the DSN GTS to the JPL MMNAV team and from the Pushchino GTS to the ASC navigation team, and post-pass (via FTP) from the GBTS to the JPL MMNAV team. ...

... 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"). ...

... The dayside auroral precipitation consist of magnetosheath related boundary layer precipitation, and plasma sheet related BPS/CPS precipitation (extensions of the nightside precipitation regions). ... For example, the much lower fluxes from the LLBL region when compared to the cusp are compensated by the bidirectional electron beams found in the LLBL: the precipitating energy fluxes in the LLBL and the cusp are not that different. ... directly through the cusp and plasma mantle . ...

... of polarisations ( 1 = DAS inputs 1 and 2 are X, # 2 = DAS input 1 is X and 2 is Y) # # rest freq1 = Rest freq ( MHz ) in IF1 # # rest freq2 = Rest freq ( MHz ) in IF2 (set to 0.0 if no 2nd IF) # # BW1 = bandwidth of IF1 # # BW2 = bandwidth of IF2 (set to 0.0 if no 2nd IF) # # Time = Time needed ON SOURCE ( min ) # # Cor config = correlator config file # # No Avg = number of integrations to average before writing # # ... Pos time = (in min) Time spent at each position offset. ...

Next: Program use Up: Description of program searchdup Previous: Description of program searchdup . Parameter input is done with a graphic user interface. ... Input file: Name of the input catalog file. It has to be formatted, one record per source/observation, according to the format used in the Arcetri observations and source archives. ... Minimum number of observations per source Source with less than this number of independent observations are not included in the output file . ...

Next: Calar Alto 2.2m telescope Up: Spectral observations and data Previous: Observations . ... We used a 2'' 205'' slit with a KPC-10A grating (316 grooves mm -1 ) in its first order, and a GG 375 order separation filter cutting off second-order contamination for wavelengths blueward of 7400?. ... Next: Calar Alto 2.2m telescope Up: Spectral observations and data Previous: Observations Laboratory "Structure" . ...

... 8, ``Celestial Mechanics'', 2002 Physical libration of the Moon: the results and the perspectives N. Petrova 1 , A. Gusev 1 , K. Heki 2 , H. Hanada 2 , N. Kawano 2 and ILOM Research Group 2 1 Kazan State University, Kazan, Russia 2 National Astronomical Observatory, Mizusawa, Iwate, Japan Beginning of the new millenium is marked by the reviews of results and problems in the field of lunar physical libration (LPhL) (Petrova, Gusev, 2001; Williams et al., 2001). ... 2001, 80, 215. ... 2001, 106, No. ...

Beginning from the May of the 1997 we started to publish our daily solar radio observations at RATAN-600 radiotelescope. ... Periscope System: South Sector+Flat Mirror . ... It is possible to track a source by moving the secondary mirror along the arc-shaped railway tracks or to perform azimuthal 2D map synthesis . ... 1) It is possible to simultaneously carry out independent observing programs using individual sectors at various discrete azimuths and secondary mirrors on corresponding railway tracks. ...

RTT150 . ... HEAD IKI . This page is a search interface through RTT150 observationsdatabase which is stored at IKI. According to the agreement between participantsof RTT150 project, observational data fully belong to the institution which hascarried out this observation for one year, are available to all three partiesinvolved (IKI, KSU and TUG) during the second year and become freely accessibleto the whole astronomical community starting two years after observation date. ...

The close position of main satellite and subsatellite (distance between them about 1000 km) and using the similar sets of Faraday cups (VDP and VDP-S) with high resolution measurements (up to 16 Hz for the main satellite and up to 10 Hz for the subsatellite) allow us to determine the small-scale variations of the magnetopause shape and position and to estimate the velocity of the magnetopause motion. ... Two point observation of the magnetopause motion: the INTERBALL project. ...

... Science . ... Data Handling and Products > Data Reduction FAQ > The calibration data for my observations look strange. Can you confirm that they look as the are supposed to look? ... Science Users Information . Observing Facilities . ... Paranal Facilities . La Silla Facilities . ... Observing with ESO Telescopes . ... Data Pipelines and Calibrations . ... Science Data Products Forum . ... Science Archive Facility . ... ESO Data . ... ESO Data Access Policy . ... ESO Science Newsletter . ...

... Flux density at 1 GHz (/Jy): 160 . ... Radio: Limb-brightened to NE, with faint extension to the E. Optical: Brightest to the NE, with faint filaments outside the NE boundary. ... Fesen 1984, ApJ, 281, 658. ... ADS . ... 151 MHz observations (1'.2?3'.1) and Half-Mile Telescope at 1.4 GHz (2'.1?5'.4). ... Radio, IR, optical, UV and X-ray comparison, including VLA at 1.6 GHz (3".8?3".3 and 40''). ... 1988, ApJ, 335, 215. ... IR observations of shocked O 2 . ... Observations of shocked molecular...

... On­The­Fly Re­Calibration of HST Observations B. Pirenne and A. Micol Space Telescope -- European Coordinating Facility, ESO, Garching, D­85748 D. Durand and S. Gaudet Canadian Astronomy Data Centre, DAO, Victoria, BC Abstract. ... On­the­fly re­calibration data flow: from request submis­ sion to data delivery. ... On­the­fly re­calibration has another advantage for our archive sites: we only need to keep the raw data and calibration reference files on­line for the process to be automatic. ...

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... The interface between the lower solar atmosphere where energy is generated by subsurface convection and the corona comprises the chromosphere, which is dominated by jet-like, dynamic structures, called mottles when found in quiet regions, fibrils when found in active regions and spicules when observed at the solar limb. ... In addition, how they affect the coronal heating and solar wind need to be further explored. ...

... 2009 March 21 . Fermi's Gamma-Ray Sky . ... What shines in Fermi's gamma-ray sky? ... Within our galaxy: the Sun traces a faint arc across the map between the observation dates, LSI +61 303 is an X-ray binary star about 6,500 light-years away, PSR J1836+5925 is a type of pulsar (spinning neutron star) that is only seen to pulse at gamma-ray energies, and 47 Tuc is a globular star cluster some 15,000 light-years away. ... About APOD | ...

Fermi s Gamma Ray Sky . ... Credit Copyright: NASA , DOE , Fermi LAT Collaboration Explanation: Scanning the entire sky in gamma-rays, photons with over 50 million times the energy of visible light, the Fermi mission's Large Area Telescope (LAT) explores the high-energy universe. ... A new paper describes the 205 brightest gamma-ray sources, but this map highlights a Fermi "top ten" list of five sources within, and five sources that lie beyond our Milky Way Galaxy . ... NASA Official: Jay Norris. ...

... Our scientific interest is an accuracy of asteroid CCD observations obtained by amateurs and professional astronomers all over in the World. ... These data help us to analyse an accuracy of real CCD positions in the MPC Database. ... Do you test your observations of the small Solar System bodies permanently before sending them to the International Minor Planets' Center? ... Do you know a real accuracy of your positional CCD-observations in comparison with the other observatories' one ? ...