E. Birsin, J. Colomé, D. Hoffmann, H. Koeppel, G. Lamanna, T. Le Flour, A. Lopatin, E. Lyard, D. Melkumyan, I. Oya, J-L. Panazol, S. Schlenstedt, T. Schmidt, U. Schwanke, R. Walter, P. Wegner for the CTA Consortium
The Cherenkov Telescope Array (CTA) \cite{CTA:2010} will be the successor to current Imaging Atmospheric Cherenkov Telescopes (IACT) like H.E.S.S., MAGIC and VERITAS. CTA will improve in sensitivity by about an order of magnitude compared to the current generation of IACTs. The energy range will extend from well below 100 GeV to above 100 TeV. To accomplish these goals, CTA will consist of two arrays, one in each hemisphere, consisting of 50-80 telescopes and composed of three different telescope types with different mirror sizes. It will be the first open observatory for very high energy $\gamma$-ray astronomy. The Array Control working group of CTA is currently evaluating existing technologies which are best suited for a project like CTA. The considered solutions comprise the ALMA Common Software (ACS), the OPC Unified Architecture (OPC UA) and the Data Distribution Service (DDS) for bulk data transfer. The first applications, like an automatic observation scheduler and the control software for some prototype instrumentation have been developed.
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http://arxiv.org/abs/1211.5618
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