KEYWORDS: Control systems, Design, Data modeling, Instrument modeling, Data storage, Computer simulations, Logic, Control systems design, Process control, Telescopes
Modern astronomical telescopes often rely on control systems for observations. Many factors may affect the development of control systems, such as the differences in the development phases of devices, the robustness of devices. A simulation framework which mocks the component of each device is needed to speed up the development of control system, facilitating behavior-level simulation to support the upper layer development. Presently, many industry-standard simulation systems are predominantly based on actual hardware systems, which necessitate the development of independent hardware logic, such as the simulator of LSST. We have designed the Rsimu framework. This framework is built upon the RACS2 and is highly proficient in behavior simulation of devices. Rsimu's behavior is entirely configurable, and the properties of different components can be dynamically defined by pluggable configuration files. A shared data-plane is provided for components to synchronize their status, therefore helps developers to separate the behavior model of components apart. A series of designs, including pull-update, state-machine etc. are provided to help users to establish the simulation system.
WFST telescope is a large-aperture sky survey telescope jointly built by the University of Science and Technology of China and Purple Mountain Observatory. It is currently the most powerful optical time-domain sky survey telescope in the northern hemisphere. Its scientific goals are diverse, and the urgency and observation window period of different scientific tasks are different. During the observation period, the control of equipment requires accuracy, real-time, efficiency and safety. Therefore, we design and implement the OCS (Observatory Control System) of WFST which performs multi-layer abstraction on each hardware device and puts more attention on the operation of the observation process and the scheduling of observation tasks. In order to ensure the safety of equipment during the observation process, the OCS introduces a weather alarm system and fault diagnosis system. At the same time, we design an observation strategy system in the OCS to adjust the observation plan based on task priority, equipment information and meteorological information to maximize the efficiency of sky survey.
Chinese scientists plan to build an 80 centimeter caliber near-infrared astronomical telescope in Antarctica, consisting of one telescope and two terminal devices. The K-band astronomical imaging system is one of the main terminals. We designed and characterized a 1x3 K-band near-infrared mosaic camera and the MCT detectors form Shanghai Institute of Technical Physics. The single pixel array of this camera is 640x512, with a single pixel size of 15 μm. Three detectors arranged in a mosaic configuration generated a focal plane pixel array of 1920x512. To ensure the optimal performance of the K-band astronomical imaging system, we used Dewar sealing, vacuum maintenance, and thermoacoustic refrigerator to cool the detector to 80K and the optical lens and components to 150K. In addition, a low-noise power supply design and electronic devices with low readout noise are adopted to ensure the minimum dark current and low readout noise of the mosaic infrared camera. The flatness of the mosaic detector is less than 20 μm . Complies with the design specifications for K-band astronomical imaging system.
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