The Nobeyama Radioheliograph --- Hardware System ---

Details The Nobeyama Radioheliograph --- Hardware System --- The Nobeyama Radioheliograph --- Hardware System ---

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994kofu.symp...19n&link_type=abstract

In: Proceedings of Kofu Symposium, Kofu, Japan, Sept. 6-10, 1993, p.19-33.

Computer Science

6

Scientific paper

The Nobeyama Radioheliograph began routine observations in late June, 1992, and radio full-disk images of the Sun have been observed for 8h every day. This instrument is a 17-GHz radio interferometer dedicated for solar observations, which consists of eighty-four 80-cm-diameter antennas arranged in a Tee-shaped array extending 490m in east-west and 220m in north-south directions. The spatial resolution is 10" and the temporal resolution is 1s and 50ms for selected events. The array configuration is optimized to observe the whole sun with high spatial and temporal resolution and a high dynamic range of images. Image quality of better than 20dB is realized by incorporation of technical advances in hardware and software, such as (1) low-loss phase-stable optical fiber cables for local reference signal and IF signals, (2) newly developed phase-stable local oscillators, (3) custom CMOS gate-array LSIs of one-bit quadra-phase correlators for 4 x 4 combinations, (4) an expanded real-time self-calibration method of gain and phase errors using redundant antenna combinations, and (5) new image processing techniques to suppress large sidelobe effects due to the solar disk and extended sources. A newly developed control system with fully distributed computers enable us to continue observations even in a condition where some portions of the radioheliograph are malfunctioning. In this paper, a detailed description is given of the radioheliograph's hardware, with particular emphasis on the stability and accuracy of the total system.

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