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28 July 2008 VLTI behind the scene: 1001 nights of data flow operations at ESO
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Since the beginning of the Paranal Service Mode observations, the DFO group is dedicated in monitoring the VLT/VLTI instruments, in controlling the quality of the data and in providing the principal investigators (PI) with reduced calibrated data whenever possible. Each year, new instruments are coming into operations, bringing more complex challenges for our Data Flow Operations. We will briefly present the VLTI data flow operations implemented for the first VLTI instrument VINCI, then we will focus on the monitoring of the instruments MIDI and AMBER. For each of these instruments, basics parameters such as the detector, the instrument alignment are monitored. Calibrations are also processed either for to monitor the stability of the instrument or/and to be applied to the science data. We also developed more complex procedures to follow the behavior of the subsystems such as MACAO (adaptive optics), IRIS (fast guiding), FINITO (fringe tracker). Some procedures have been developed to monitor the instrumental Transfer Function for the different instrument setups and configurations will be shown. To understand the Transfer Function, it is important to have a good knowledge of the objects (calibrators) used for the measurement. We will discuss the issue of interferometric calibrators and present the work on this subject done specifically for VLTI. In 2008, PRIMA facility will start operations. Its astrometry mode will be commissioned. Like each new VLT/VLTI instrument this PRIMA astrometric mode will be supported by our group.
© (2008) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
I. Percheron "VLTI behind the scene: 1001 nights of data flow operations at ESO", Proc. SPIE 7013, Optical and Infrared Interferometry, 70134E (28 July 2008);


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