The Wide Field Survey Telescope (WFST) is a dedicated photometric surveying facility equipped with a 2.5-meter diameter primary mirror, an active optics system, and a mosaic CCD camera with 0.765 gigapixels on the primary focal plane for high quality image capture over a 6.5-square-degree field of view. The mosaic CCD camera is the key device for high precision photometric and high frequency observation and the ‘eye’ of the telescope for deep survey with wide field. The focal plane consists of three kinds of CCD including scientific imaging sensors, wavefront sensors and guiding sensors. In the scientific imaging area, there are 9 back-illuminated full frame scientific CCDs –CCD290-99 from E2V company with pixels of 9K by 9K and pixel size of 10um, which is mosaicked by 3 by 3 with flatness of 20μm PV. The R&D of the camera including the high precision large-scale mosaicking of detectors, detectors’ cryocooling and vacuum sealing, readout and driving with low noise and low power, data acquisition, imaging control, data storage and distribution. Furthermore a camera control system (CCS) was developed at same time.
Effective and continuous monitoring of space debris in satellite orbit is an important issue in resolving potential threats to aerospace equipment. The SDM (Space Debris Monitoring)-16803 is a front-illuminated high-readout-speed, low-noise scientific CCD camera designed for the needs of space debris monitoring telescopes. The camera is designed with drift scanning function in which mode the moving target will be presented as a static image, so that a fixed telescope can track the moving space target. The electronics of the camera provides driving signals for the CCD, samples the video signals of the CCD, and also communicates with the host computer. The maximum readout speed of the CCD is 10Mpixels. The mechanics structure of the camera is designed with a sealed chamber in which a TEC (Thermo Electric Cooler) is used for cooling the sensor and provide a stable temperature.
In a CCD camera system, the CCD sensor must be cooled to low temperature to reduce the dark current. Many factors will affect the cooling performance as we use TEC. Therefore, quantitative analysis of the effects of the various factors on the cooling performance is very important for designing the cooling structure of the CCD vacuum head. In this paper, the length and diameter of the wires between the CCD and the vacuum feedthrough, the thickness of the cold end, and the vacuum degree are taken into consideration and analysis. Through the simulation, useful conclusions are obtained to guide the machanics and cooling design of the CCD vacuum head.
A 1K*1K CCD camera is designed, implemented and tested for CSTAR telescope in Antarctica, including its mechanics, CCD controller, power and temperature controller unit. Mechanical and electronic design for low temperature environment is taken into consideration fully. The camera has reliable mechanics and stable electronics performance. The readout noise is as low as 3.99݁ି when the CCD readout speed is 100kpixs/s. We fully tested every part of the camera in a Cryogenic refrigerator (-86 degree centigrade) and proved that our camera has the ability to work in Antarctica for a long term. Finally, the camera was tested on the CSTAR telescopes to take observations and the imaging quality meets requirement.
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