Radio astronomy narrow band spectral line observation platform based on agile transceiver

Abstract

A radio astronomy narrow band spectral line observation platform based on an agile transceiver consists of an agile transceiver AD9361 circuit board, an FPGA control circuit board and a control computer which are connected in sequence. The input signal bandwidth of the agile transceiver AD9361 circuit board can reach DC-6GHz, a signal input end of the agile transceiver AD9361 circuit board is connected with a radio frequency output end of a radio astronomy telescope, a control end and a data output end of the agile transceiver AD9361 circuit board are connected with the FPGA control circuit board, the FPGA control circuit board is connected with the main control computer through a network port, control software is integrated at the main control computer, and parameters including a center frequency point, observation bandwidth and AGC (automatic gain control) gain are sent to the AD 9361 through an FPGA chip on the platform according to the narrow band spectral line radio source red shift, the center frequency point, the contour extension and other parameters. As for observation targets of a narrow band spectral line in radio astronomy, the invention has the advantages of high band-pass selection flexibility, high spectral resolution and the like as compared with a conventional device.

Description

technical field [0001] The invention relates to the field of spectrum analysis and observation of narrow-band spectral lines in the centimeter-decimeter band below 6 GHz in radio astronomy, and is especially suitable for the observation requirements of large-scale L-C band telescopes for maser and molecular spectral lines. technical background [0002] Microwave spectral lines play a pivotal role in radio astronomical observations, and can be used to diagnose the basic physical and chemical conditions of related celestial bodies, such as excitation temperature, particle density, velocity field in the material movement area, magnetic induction intensity, and chemical abundance of various elements, etc. . After obtaining the spectral line data of molecular clouds and star-forming regions through observation, the statistical equilibrium radiation transfer equation can be solved by appropriate approximation methods, so as to obtain various information of celestial bodies. [00...

AI Technical Summary

Problems solved by technology

[0011] With the increase of acquisition speed, the number of FFT points required to achieve the same frequency resolution will increase greatly, which will bring huge pressure to the back-end calculation, storage and transmission

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