The performance of the Mosaic CMOS Wide Field Camera for Transneptunian Automatic Occultation Survey (TAOS II)

Shiang-Yu Wang; Bo-Jhou Wang; Chung-Kai Huang; Hung-Hsu Ling; Yin-Chang Chang; Shu-Fu Hsu; Hsin-Yo Chen; Zhi-Wei Zhang; Matthew Lehner; John C. Geary; Stephen M. Amato; Andrew Szentgyorgyi; Timothy Norton; Charles Alcock; Joel Castro-Chacón; Mauricio Reyes-Ruíz

doi:10.1117/12.3018461

18 July 2024 The performance of the Mosaic CMOS Wide Field Camera for Transneptunian Automatic Occultation Survey (TAOS II)

Shiang-Yu Wang, Bo-Jhou Wang, Chung-Kai Huang, Hung-Hsu Ling, Yin-Chang Chang, Shu-Fu Hsu, Hsin-Yo Chen, Zhi-Wei Zhang, Matthew Lehner, John C. Geary, Stephen M. Amato, Andrew Szentgyorgyi, Timothy Norton, Charles Alcock, Joel Castro-Chacón, Mauricio Reyes-Ruíz

Author Affiliations +

Proceedings Volume 13096, Ground-based and Airborne Instrumentation for Astronomy X; 130962Y (2024) https://doi.org/10.1117/12.3018461
Event: SPIE Astronomical Telescopes + Instrumentation, 2024, Yokohama, Japan

Conference Poster

Abstract

The Transneptunian Automated Occultation Survey (TAOS II) is a three robotic telescope project to detect stellar occultation events generated by TNOs. TAOS II aims to monitor about 10000 stars simultaneously at 20Hz to generate a significant event rate. The TAOS II cameras are designed to cover the 1.7 degree diameter field of view of the 1.3m telescopes with a mosaic of ten 4.5k × 2k e2v CIS 113 CMOS sensors. The CIS 113 has a back-illuminated thinned structure to provide similar performance to that of back-thinned CCDs. The CIS 113 device has 16 micron pixels with 8 outputs, with a plate scale about 0.63”/pixel. With the freedom of direct row and column addressing, star boxes with sizes of 8 × 8 pixels in each sensor can be sampled at 20 Hz or higher with a pixel rate of 1M pixel/sec per channel. The sensors, mounted on a single Invar plate, are cooled to an operating temperature of about 200K by a cryogenic cooler. The gap between two sensors is about 0.5mm. The control electronics consist of an analog part and a Xilinx FPGA based digital circuit. One FPGA is needed to control and process the signal from each CIS 113 chip. Two large PCBs were used to fanout signals from the 10 CMOS devices through the vacuum chamber wall. A synchronization circuit receives a pulse from the control building to ensure the timing error of exposures of the three cameras is within 1 ms. The cameras were delivered and installed on the TAOS telescopes in 2023 and series of tests and adjustments have been carried out to optimize the performance. In this presentation, the camera performance in the full frame mode and the window mode will be detailed. The synchronization and the adjustment among the three cameras will also be presented.

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Shiang-Yu Wang, Bo-Jhou Wang, Chung-Kai Huang, Hung-Hsu Ling, Yin-Chang Chang, Shu-Fu Hsu, Hsin-Yo Chen, Zhi-Wei Zhang, Matthew Lehner, John C. Geary, Stephen M. Amato, Andrew Szentgyorgyi, Timothy Norton, Charles Alcock, Joel Castro-Chacón, and Mauricio Reyes-Ruíz "The performance of the Mosaic CMOS Wide Field Camera for Transneptunian Automatic Occultation Survey (TAOS II)", Proc. SPIE 13096, Ground-based and Airborne Instrumentation for Astronomy X, 130962Y (18 July 2024); https://doi.org/10.1117/12.3018461

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