SiD Tracking using VXD Nick Sinev, University of Oregon Plan Motivation Track reconstruction algorithm Performance for single tracks Does it have any limits ? With backgrounds To do Motivation Tracking in SiD is a challenge, especially pattern recognition. ... Limitations caused by reconstruction speed consideration In the presence of high number of background hits, number of 3-point combinations used as track seed became enormous if we consider all combinations. ...

Ground Support of RadioAstron . Control and Tracking Stations . RadioAstron satellite control (command transmission, telemetry, orbit measurements) will be conducted from Evpatoria and Bear Lake control stations. ... Coarse orbit measurements will be carried out from control stations. Each measurement takes ten minutes. ... Orbit measurements at tracking stations give only radial component of spacecraft velocity but the measurements are going continuously during observing sessions. ...

... The MROI makes use of optical interferometry, much like COAST . ... As a major collaborator, the Cambridge Astrophysics Group is currently developing some of the mechanisms below, specifically the delay line and the fast tip-tilt system. ... Fringe tracking is used to control the positions of the delay line trolleys to make sure the light beams from the different telescopes in the MROI arrive at the science camera beam combiners in phase so that an interference pattern can be produced. ...

Russell Owen , Charles Hull and Walter Siegmund The Apache Point Observatory 3.5m telescope, located in the Sacramento Mountains of New Mexico at an elevation of 2.8 km, is awaiting the installation of the primary mirror. ... Important features of the design include a fast (f/1.75) lightweight honeycomb mirror, a compact altitude/azimuth mount, friction-coupled drives and position encoders, and use of a telescope model to compensate for mechanical errors (1) . ... Table 1: The current telescope model. ...

... HST . Moving COS FUV Spectra to the Third COS FUV Lifetime Position . ... HST Overview . Overview . ... Sometime near the start of Cycle 22, the location of COS FUV spectra on the detector is expected to be moved from the second COS FUV Lifetime Position (LP2) to the third COS FUV Lifetime Position (LP3). ... With the LP3 move, spectra will be shifted below the original LP1 position by about -2.5", which maximizes resolution and the detector area available for future lifetime positions. ...

On,off position switching is done to remove standing waves from the resulting spectra. ... 1,5,10,20,25,50,100 samples corresponding to great circle angular offsets of .004,.02,.04,.07,.09,.18, and .35 degrees. ... Page 1: rms vs great circle offset. ... Page 2: rms vs little circle offset. ... The rms increase correlates better with great rather than little circle offsets. the 1 usec standing wave starts to be seen in the .07 degree offsets. a .9 usec standing wave is seen at .35 degrees offset. ...

... Pre-university education . ... For the year Samara State Aerospace University moved up in the ranking of Vladimir Potanin Foundation from the 44th to the 10th place and added three positions in the ranking of universities reputation Expert RA in the field of Engineering, natural and exact sciences . Samara State Aerospace University has significantly improved its position in the ranking of universities of Vladimir Potanin Charitable Foundation at the end of academic year 2014-2015. ...

MSSSO Annual Report 1997 . ... The Duffield Heliostat was designed and constructed for the Stromlo Exploratory, and forms the central feature within the building. It produces a stationary, high-quality image of the sun, which is one of the major exhibits in the Exploratory, and was installed in time for the opening ceremony on July 26, 1997(Fig. ... The tracker module of the Heliostat is located at the top of the pier in the central area of the building, under a roll-off roof. ...

European Southern Observatory La Silla Paranal Observatory HARPS Secondary Guiding 1 Poster 7739-171 2 Gerardo Ihle1, Ismo Kastinen1, Gaspare Lo Curto1, Alex Segovia1, Peter Sinclaire1, Raffaele Tomelleri gihle@eso.org, 1glocurto@eso.org, 2r.tomelleri@tomelleri.com Introduction HARPS, the High Accuracy Radial velocity Planet Searcher at the ESO La Silla 3.6m telescope, is dedicated to the discovery of exosolar planets and high resolution spectroscopy. ... Fig. 5a Details Fig. 5 Tip Tilt table. ...

Next: The ESO VLT CCD Detectors Software . ... Up: Instrument-Specific Software . ... The framework for data calibration and analysis of the VLT instrumentation is presented, based on the concepts of a calibration plan, pipeline calibration, quality control, and archiving of calibrated data for a ground-based observatory. ... Quality Control Pipeline provides quality assessment for instrument performance data and observing conditions, and tests the results of the Reduction Pipeline. ...

BTA control information and schematic view of telescope position . ... Control: Tracking . ... Target: Object . ... 092 o 45'02.4" . ... Object: . ... Difference: . 000 o 00'00.0" . 00 o 00'00.0" . ... Position: . ... Focus position: 035.00mm . ... Outdoor temperature: -01.6 . ... Indome temperature: -00.5 . ... Main mirror temperature: -02.5 . Temperature difference: 0.9 ...