System and method for observing continuous spectrum of Tiangma telescope

Abstract

The invention relates to a celestial telescope continuous spectrum observation system comprising a celestial telescope which is configured to receive radio signals from the depth of the universe; the receiver module is configured to amplify and process the radio signal received by the Tiangma telescope and output an intermediate frequency signal; the intermediate frequency transmission module is configured to receive the intermediate frequency signal output by the receiver module; the continuous spectrum terminal is arranged in a feed source cabin of the Tiangma telescope and is configured to receive the intermediate frequency signal from the intermediate frequency transmission module and convert the intermediate frequency signal into a digital signal; and the data processing module is configured to receive the digital signal from the continuous spectrum terminal and process the digital signal to obtain a measurement result of the flow of the radio power source so as to complete the continuous spectrum observation of the Tiangma telescope.

Description

Technical Field

[0001] The present invention relates to the field of radio astronomy technology, and more specifically to a continuous spectrum observation system and method for a Tianma telescope. Background Art

[0002] Continuum spectrum refers to the fact that the intensity of radiation from a celestial body changes continuously with frequency over a wide frequency range, without obvious absorption or emission line characteristics. Continuum spectrum observation is very important for radio telescopes. First, it can be used to test the performance of the telescope. Second, multi-band continuous spectrum observation can determine the spectral index of the source, which helps to study the magnetic field of the Milky Way, supernova remnants and other topics. Finally, monitoring the continuous spectrum flux helps to study the time-varying characteristics of radio sources and the structure of the interstellar medium.

[0003] The Green Bank Telescope (GBT) in the United States uses two continuous spectrum observation methods: on-off observation and on-the-fly (OTF). The continuous spectrum observation terminal of GBT is the Caltech Continuum Backend (CCB), which is designed for GBT's dual-beam Ka-band receiver and covers the frequency range of 26 GHz to 40 GHz. In addition, the Parkes radio telescope in Australia uses an Ultra-Wideband-Low (UWL) receiver for continuous spectrum observation, covering the radio frequency range of 704 MHz to 4032 MHz. The continuous spectrum terminal of the Australia Telescope Compact Array (ATCA) is the Compact Array Broadband Backend (CABB), and its observation bandwidth is 2048 MHz.

[0004] The Tianma telescope uses two methods for continuous spectrum observation: single-point observation and mapping observation. It is currently the largest all-round rotatable radio telescope in Asia, with a main reflector diameter of 65m and equipped with 7 sets of receivers, including L, S / X, C, Ku, K, X / Ka, and Q, which can cover a wide frequency range from 1MHz to 50GHz.

[0005] At present, the Tianma telescope continuous spectrum observation system uses DIBAS equipment as its continuous spectrum observation terminal. However, DIBAS has many limitations and shortcomings: there is radio frequency interference inside the equipment or signal attenuation during microwave link transmission, resulting in low measurement accuracy; DIBAS is an imported device, which is difficult to maintain and repair, lacks self-diagnosis and rapid repair capabilities, and relies on original manufacturer support, which increases maintenance time and cost and may cause observation work interruption; the DIBAS system is limited by hardware structure in terms of function expansion and performance optimization, and the upgrade and optimization cost is high and complex, the response speed is slow, and it is difficult to adapt to new needs and technological development. Summary of the invention

[0006] To solve the above problems in the prior art, the present invention provides a continuous spectrum observation system and method for the Tianma telescope, which adopts a universal software radio peripheral (USRP) hardware device as a continuous spectrum terminal to overcome the problems of low measurement accuracy, difficult maintenance, and limited upgrading and optimization.

[0007] The present invention provides a Tianma telescope continuous spectrum observation system, comprising:

[0008] The Tianma telescope is set up to: receive radio signals from deep in the universe;

[0009] The receiver module is configured to: amplify and process the radio signal received by the Tianma telescope and output an intermediate frequency signal;

[0010] An intermediate frequency transmission module is configured to: receive the intermediate frequency signal output by the receiver module;

[0011] A continuous spectrum terminal is installed in the feed cabin of the Tianma telescope and is configured to: receive the intermediate frequency signal from the intermediate frequency transmission module, and perform digital down-conversion and AD sampling on the intermediate frequency signal to obtain a baseband signal;

[0012] The data processing module is configured to: receive a baseband signal from the continuous spectrum terminal, and process the baseband signal to obtain a measurement result of the radio source flow, and complete the continuous spectrum observation of the Tianma telescope.

[0013] Preferably, the continuous spectrum terminal adopts a USRP X410 device.

[0014] Furthermore, the data processing module includes:

[0015] The data acquisition module is configured to: configure the sampling frequency, center frequency and required total number of samples of the continuous spectrum terminal, and after the configuration is completed, receive sample data from the continuous spectrum terminal, and detect whether there is error information in the sample data, if error information is detected, re-receive the sample data; if no error information is detected, stop receiving sample data after the total number of samples is reached;

[0016] The data preprocessing module is configured to: perform calibration processing on the sample data, read the antenna position data at the same time, and perform linear interpolation on the antenna position data according to the calibrated data to obtain preprocessed data;

[0017] The data post-processing module is configured to: calculate the pre-processed data to obtain the target source flow.

[0018] Furthermore, the data acquisition module may be further configured to: configure a clock source so as to synchronize the sampling operation of the continuous spectrum terminal with the operation of the data acquisition module receiving sample data.

[0019] Furthermore, the data preprocessing module can also be configured to determine whether pointing correction is required; if necessary, perform Gaussian fitting on the preprocessed data to obtain pointing errors in the right ascension and / or declination directions, convert the pointing errors in the right ascension and / or declination directions into pointing errors in the azimuth and / or pitch directions, and then implement pointing correction.

[0020] Furthermore, the data post-processing module includes:

[0021] A baseline correction module, configured to: remove background noise in the preprocessed data, and correct the angle deviation between the sample data and a preset target;

[0022] A parameter calculation module is configured to: extract the amplitude of the target source signal, calculate the half-power beam width and the root mean square of the preprocessed data;

[0023] A gain curve drawing module is configured to: analyze the relationship between antenna gain and elevation angle / azimuth angle according to the preprocessed data to generate a gain curve graph;

[0024] The target source flow calculation module is configured to obtain the relative error related to the target source signal amplitude according to the calculation result obtained by the parameter calculation module, and convert the observed temperature of the target source into flow to obtain the target source flow.

[0025] Furthermore, the target source flow calculation module is configured to obtain the maximum amplitude and standard deviation of the target source signal according to the amplitude of the target source signal, calculate the correction factor by fitting, and obtain the observed temperature of the target source after combining the maximum amplitude of the target source signal with the correction factor.

[0026] The present invention also provides a method for observing a continuous spectrum of a Tianma telescope, comprising:

[0027] Step S1, providing the above-mentioned Tianma telescope continuous spectrum observation system, the data processing module configures the sampling frequency, center frequency and required total number of samples of the continuous spectrum terminal, and configures the clock source to synchronize the sampling operation of the continuous spectrum terminal and the operation of the data processing module receiving sample data;

[0028] Step S2, receiving sample data and detecting whether there is error information in the sample data, if error information is detected, re-receiving sample data; if no error information is detected, stopping receiving sample data after reaching the total number of samples;

[0029] Step S3, calibrating the sample data, reading the antenna position data, and performing linear interpolation on the antenna position data according to the calibrated data to obtain preprocessed data;

[0030] Step S4, calculating the preprocessed data to obtain the target source flow.

[0031] Furthermore, step S4 also includes: determining whether pointing correction is required, and if necessary, performing Gaussian fitting on the preprocessed data to obtain pointing errors in the right ascension and / or declination directions, and converting the pointing errors in the right ascension and / or declination directions into pointing errors in the azimuth and / or pitch directions to implement pointing correction.

[0032] Furthermore, the step S4 comprises:

[0033] Step S41, removing background noise in the preprocessed data and correcting the angle deviation between the observed data and the preset target;

[0034] Step S42, extracting the amplitude of the target source signal, calculating the half-power beam width and the root mean square of the pre-processed data;

[0035] Step S43, analyzing the relationship between antenna gain and elevation angle / azimuth angle according to the preprocessed data, and generating a gain curve graph;

[0036] Step S44, according to the calculation result obtained in step S42, the relative error related to the target source signal amplitude is obtained, and the observed temperature of the target source is converted into flow rate to obtain the target source flow rate.

[0037] The present invention has the following beneficial effects:

[0038] (1) Significantly improved measurement accuracy: The present invention uses the USRP X410 hardware device and installs it in the feed cabin, effectively avoiding the signal passing through optical fiber transmission, down-conversion system and long-distance link. This greatly reduces radio frequency interference and signal transmission loss, so that the flow measurement accuracy of the radio source can be doubled, and the continuous spectrum data of celestial bodies can be captured more accurately.

[0039] (2) Easier maintenance and troubleshooting: Compared to the DIBAS system, the USRP X410 device used in the present invention has higher maintainability. It supports software-defined system configuration, allowing rapid self-diagnosis and fault detection, thereby greatly simplifying the maintenance and repair process. This improvement reduces dependence on external support and reduces the cost and time of equipment maintenance.

[0040] (3) Enhanced system flexibility and scalability: The present invention utilizes the programmable features of the USRP X410 to achieve a modular design of the system. This flexibility allows the system to be easily upgraded and optimized, and can quickly integrate new functions or adapt to new observation requirements. This feature not only supports current scientific tasks, but also provides expansion space for future technological development.

[0041] (4) Improved reliability and stability: By reducing radio frequency interference and link loss, the present invention significantly improves the reliability of the system and ensures high-quality observation data.

[0042] (5) Faster response speed: The system architecture of the present invention enables faster response to new observation requirements. Using software-defined radio technology, the system can be reconfigured and adjusted in a short period of time to quickly adapt to new scientific goals and operating environments, thereby improving the operating efficiency of the Tianma Telescope. BRIEF DESCRIPTION OF THE DRAWINGS

[0043] Figure 1 It is a block diagram of the continuous spectrum observation system of the Tianma telescope according to the present invention. DETAILED DESCRIPTION

[0044] The preferred embodiments of the present invention are given below in conjunction with the accompanying drawings and described in detail.

[0045] Embodiment 1

[0046] like Figure 1 As shown, the first embodiment of the present invention provides a continuous spectrum observation system for the Tianma telescope, which includes an antenna module 1, a receiver module 2, an intermediate frequency transmission module 3, a continuous spectrum terminal 4 and a data processing module 5 connected in sequence.

[0047] The antenna module 1 is configured to receive radio signals from the depths of the universe. In the present invention, the antenna module 1 is the Shanghai Tianma 65m radio telescope. As one of the largest fully movable radio telescopes in China, the Tianma telescope has extremely high sensitivity and resolution, and can receive radio signals in a wide frequency range.

[0048] Receiver module 2 is configured to amplify and process the radio signal received by antenna module 1 to output an intermediate frequency signal. The Tianma telescope is equipped with 7 different receivers that can cover a wide frequency range from 1MHz to 50GHz, including L-band, S / X-band, C-band, Ku-band, K-band, X / Ka-band and Q-band. Each receiver is targeted at a specific frequency range, as shown in the following table:

[0049] The intermediate frequency transmission module 3 is configured to stably and effectively transmit the intermediate frequency signal output by the receiver module 2 to the continuous spectrum terminal 4. This module ensures the integrity and quality of the signal during transmission, and maintains the clarity and strength of the signal by performing necessary signal adjustment and amplification. The intermediate frequency transmission module 3 is consistent with the intermediate frequency transmission module in the prior art, and will not be described in detail here.

[0050] The continuous spectrum terminal 4 is installed in the feed cabin of the Tianma telescope, and is configured to receive the intermediate frequency signal from the intermediate frequency transmission module 3, and perform digital down-conversion and AD sampling on the intermediate frequency signal to obtain a baseband signal.

[0051] In this embodiment, USRP X410 is used as the Tianma telescope continuous spectrum terminal. USRP is a universal software radio peripheral (Universal Software Radio Peripheral) developed by Ettus Research, which can be used to receive, send and process various wireless signals. The center frequency range supported by USRP X410 is 1MHz to 7.2GHz, and can be tuned to 8GHz at most when the radio frequency performance is reduced. Therefore, using USRP X410 as the Tianma telescope continuous spectrum terminal can effectively receive signals in L band (1.25-1.75GHz), S band (2.2-2.4GHz) and C band (4.0-8.0GHz).

[0052] The structure of USRP X410 is mainly divided into RF part and digital part. The RF part includes ZBX daughterboard, timing and synchronization module and GPS Disciplined Oscillator (GPSDO). Among them, ZBX daughterboard is a dual-channel superheterodyne transceiver, including amplifier, mixer and filter. The timing and synchronization module is responsible for the clock and synchronization signal management of the whole system, including reference input, pulse per second signal input and trigger input / output. GPSDO obtains accurate time signal through GPS antenna to ensure time and frequency synchronization in the system. The main modules of the digital part include Xilinx Zynq Ultrascale-ZU28DR chip, debugging and control module and high-speed interconnection module. Among them, Xilinx Zynq Ultrascale-ZU28DR chip integrates central processing unit, field programmable logic gate array, Streaming DSP module, analog-to-digital converter, digital-to-analog converter and other functional modules.

[0053] The data processing module 5 is configured to receive the digital signal from the continuous spectrum terminal 4, and process the digital signal from the continuous spectrum terminal 4 to obtain the measurement result of the radio source flux and complete the continuous spectrum observation of the Tianma telescope.

[0054] Specifically, the data processing module 5 includes a data acquisition module, a data preprocessing module and a data post-processing module, which are described in detail below.

[0055] The data acquisition module is set as follows: configure the parameters of USRP X410, including sampling rate, center frequency, bandwidth, observation time, total number of samples, data output format, etc. After the configuration is completed, receive sample data from USRP X410 and detect whether there is error information in the sample data (such as timeout or unknown error condition). If error information is detected, re-receive the sample data; if no error information is detected, stop receiving sample data after reaching the total number of samples.

[0056] To ensure synchronous operation, the data acquisition module can also be set to: configure the clock source and lock the clock of the digital part of the USRP X410 to ensure that the sampling operation of the USRP X410 and the operation of the data acquisition module to receive sample data are synchronized, thereby ensuring the stability and accuracy of the received data.

[0057] The data preprocessing module is configured to: read the sample data received by the data acquisition module, calibrate the sample data, extract the antenna position data, and linearly interpolate the antenna position data according to the calibrated data to obtain preprocessed data. The antenna position data is stored in the local control terminal.

[0058] The data preprocessing module can also be set to: determine whether pointing correction is needed; if necessary, perform Gaussian fitting on the preprocessed data to obtain pointing errors in the right ascension and / or declination directions; convert the pointing errors in the right ascension and / or declination directions into pointing errors in the azimuth and / or pitch directions to achieve pointing correction.

[0059] The data post-processing module is set to: calculate the pre-processed data and obtain the target source flow.

[0060] Specifically, the data post-processing module includes:

[0061] The baseline correction module is configured to remove background noise from the preprocessed data and correct the angle deviation between the sample data and the preset target. This module is used to remove the baseline, thereby eliminating low-frequency noise and system errors in the sample data, so as to more accurately analyze the real signal of the target source.

[0062] The parameter calculation module is set to: extract the amplitude of the target source signal, calculate the half-power beam width and the root mean square of the preprocessed data. Among them, the calculation of the half-power beam width can measure the temperature of the target source to evaluate the directivity and resolution of the antenna; calculate the noise level in the root mean square evaluation data as the basis for subsequent signal-to-noise ratio analysis.

[0063] The gain curve drawing module is configured to: analyze the relationship between antenna gain and elevation / azimuth angle based on the preprocessed data and generate a gain curve graph. The gain curve graph shows the gain variation of the antenna at different angles, which helps to identify and correct any anomalies in the antenna directivity.

[0064] The target source flow calculation module is set to: obtain the relative error (measurement error and noise error) related to the target source signal amplitude according to the calculation results obtained by the parameter calculation module, and convert the observed temperature (K) of the target source into flow (Jy) to obtain the target source flow. Among them, the relative error related to the target source signal amplitude is used to evaluate the accuracy and reliability of the measurement results, that is, to help identify the impact of measurement errors and noise on the final results, thereby ensuring data quality.

[0065] The target source flow calculation module can be further configured to obtain the maximum amplitude and standard deviation of the target source signal according to the amplitude of the target source signal, and calculate the correction factor by fitting, and combine the maximum amplitude of the target source signal with the correction factor to obtain the observed temperature of the target source. Among them, the standard deviation is used to calculate the full width half maximum value (indicating the width of the signal), reflecting the extension degree of the signal in frequency or position, and the correction factor is used to eliminate the influence of the signal width on the amplitude. This process comprehensively considers the strength of the signal and its characteristic width to provide a more accurate temperature estimate.

[0066] Embodiment 2

[0067] Embodiment 2 of the present invention provides a method for observing a continuous spectrum of a Tianma telescope, the method comprising the following steps:

[0068] Step S1, providing the above-mentioned Tianma telescope continuous spectrum observation system, the data processing module configures the sampling frequency, center frequency and required total number of samples of the continuous spectrum terminal, and configures the clock source to synchronize the sampling operation of the continuous spectrum terminal and the operation of the data processing module receiving sample data. In this embodiment, USRP X410 is used as the Tianma telescope continuous spectrum terminal.

[0069] In actual observations, radio sources with different fluxes are used for observations to verify the effectiveness of the continuous spectrum observation system. USRP X410 requires the UHD driver version 4.1 or higher to operate normally. Therefore, to ensure that all functions are supported and work properly, install UHD before observation and select the UHD driver version 4.6.

[0070] Using USRP X410 as the terminal of the continuous spectrum, this method uses the UHD library to implement signal down-conversion and AD sampling. The down-conversion process involves multiplying the received signal with the local oscillator signal generated by the local oscillator, and then extracting the converted signal through a low-pass filter. This process can be described in real or complex form, called real mixing and complex mixing, respectively. In addition, the ADC quantizer of the device is 12 bits, and the sampling rate can reach up to 500MS / s. After USRPX410 performs AD sampling on the radio signal, it transmits the collected data to the host through the QSFP28 (Quad Small Form-factor Pluggable 28) port. The network transmission rate of the QSFP28 port is related to the FPGA image, as shown in the following table: FPGA Image Style Number of channels Bandwidth per channel QSFP2 Port 0 Interface QSFP2 Port 1 Interface X4_200 4(2 per ZBX) 200MHz 4×10GbE(AllLanes) Not used UC_200 4(2 per ZBX) 200MHz Not used 100GbE CG_400 4(2per ZBX) 400MHz 100GbE 100GbE

[0071] In actual observation, the FPGA image used is UC_200, so the QSFP28 optical module can support the network transmission rate of 100GbE.

[0072] When collecting sample data, the user configuration is received through command line parameters, including relevant parameters of the USRP device (such as sampling rate, center frequency, gain, etc.) and the server's IP address and UDP port. Then, a USRP device instance is created and relevant parameters are set, and the clock source (such as internal, external, MIMO or GPSDO) is configured. The RF sample data received from the USRP device is stored in the buffer. After each batch of samples is received, the error information in the metadata is checked to handle problems such as timeout or packet loss. The received sample data is sent to the target server address and port through the network using the UDP protocol. During the receiving process, if an error is detected, the system exits the receiving loop and outputs the corresponding error information.

[0073] Step S2, receiving sample data and detecting whether there is error information in the sample data. If error information is detected, the sample data is received again; if no error information is detected, the sample data is stopped from being received after the total number of samples is reached.

[0074] Step S3, calibrating the sample data, reading the antenna position data, and performing linear interpolation on the antenna position data according to the calibrated data to obtain pre-processed data.

[0075] In this embodiment, the sample data is calibrated by using a fast periodic noise injection calibration method, that is, the sample data contains two sets of data: one set is the observation data with noise injection The other set is observation data without noise injection The calibrated data S(t) is calculated according to the following formula:

[0076]

[0077] In the formula, is the average noise calibration value within the bandwidth, and <> means taking the average value.

[0078] In this embodiment, the method for linear interpolation of the antenna position data is: according to the time value t in S(t), the antenna position data L a (t) is linearly interpolated to obtain the position value of S(t), thereby obtaining the preprocessed data S(I), where I is the position data of right ascension or declination.

[0079] Step S3 may also include: determining whether pointing correction is required; if necessary, performing Gaussian fitting on the preprocessed data to obtain pointing errors in the right ascension and / or declination directions; converting the pointing errors in the right ascension and / or declination directions into pointing errors in the azimuth and / or pitch directions, and then implementing pointing correction.

[0080] Among them, Gaussian fitting of preprocessed data is performed according to the following formula:

[0081]

[0082] Where K is the baseline slope, c is the baseline constant, a is the Gaussian function amplitude, and HPBW is the half-power beamwidth.

[0083] Step S4, calculate the preprocessed data to obtain the target source flow.

[0084] Specifically, step S4 includes:

[0085] Step S41, removing background noise in the preprocessed data and correcting the angle deviation between the observed data and the preset target.

[0086] Step S42, extracting the signal amplitude of the target source, calculating the half-power beam width and the root mean square of the pre-processed data.

[0087] Step S43: Analyze the relationship between antenna gain and elevation angle / azimuth angle based on the preprocessed data to generate a gain curve graph.

[0088] Step S44, according to the calculation results obtained by the parameter calculation module, the measurement error and noise error of the target source signal amplitude are obtained, and the observed temperature (K) of the target source is converted into flow (Jy) to obtain the target source flow.

[0089] The present invention has the following beneficial effects:

[0090] (1) Significantly improved measurement accuracy: The present invention uses the USRP X410 hardware device and installs it in the feed cabin, effectively avoiding the signal passing through optical fiber transmission, down-conversion system and long-distance link. This greatly reduces radio frequency interference and signal transmission loss, so that the flow measurement accuracy of the radio source can be doubled, and the continuous spectrum data of celestial bodies can be captured more accurately.

[0091] (2) Easier maintenance and troubleshooting: Compared to the DIBAS system, the USRP X410 device used in the present invention has higher maintainability. It supports software-defined system configuration, allowing rapid self-diagnosis and fault detection, thereby greatly simplifying the maintenance and repair process. This improvement reduces dependence on external support and reduces the cost and time of equipment maintenance.

[0092] (3) Enhanced system flexibility and scalability: The present invention utilizes the programmable features of the USRP X410 to achieve a modular design of the system. This flexibility allows the system to be easily upgraded and optimized, and can quickly integrate new functions or adapt to new observation requirements. This feature not only supports current scientific tasks, but also provides expansion space for future technological development.

[0093] (4) Improved reliability and stability: By reducing radio frequency interference and link loss, the present invention significantly improves the reliability of the system and ensures high-quality observation data.

[0094] (5) Faster response speed: The system architecture of the present invention enables faster response to new observation requirements. Using software-defined radio technology, the system can be reconfigured and adjusted in a short period of time to quickly adapt to new scientific goals and operating environments, thereby improving the operating efficiency of the Tianma Telescope.

[0095] The above is only a preferred embodiment of the present invention, and is not intended to limit the scope of the present invention. The above embodiment of the present invention can also be modified in various ways. That is, all simple, equivalent changes and modifications made according to the claims and the description of the present invention fall within the scope of protection of the claims of the present invention. The contents not described in detail in the present invention are all conventional technical contents.

Claims

1. A Tianma telescope continuous spectrum observation system, characterized in that: include: The Tianma telescope is set up to: receive radio signals from deep in the universe; The receiver module is configured to: amplify and process the radio signal received by the Tianma telescope and output an intermediate frequency signal; An intermediate frequency transmission module is configured to: receive the intermediate frequency signal output by the receiver module; A continuous spectrum terminal is installed in the feed cabin of the Tianma telescope and is configured to: receive the intermediate frequency signal from the intermediate frequency transmission module, and perform digital down-conversion and AD sampling on the intermediate frequency signal to obtain a baseband signal; The data processing module is configured to: receive a baseband signal from the continuous spectrum terminal, and process the baseband signal to obtain a measurement result of the radio source flow, and complete the continuous spectrum observation of the Tianma telescope.

2. The Tianma telescope continuous spectrum observation system according to claim 1, characterized in that: The continuous spectrum terminal adopts USRP X410 device.

3. The Tianma telescope continuous spectrum observation system according to claim 1, characterized in that: The data processing module comprises: The data acquisition module is configured to: configure the sampling frequency, center frequency and required total number of samples of the continuous spectrum terminal, and after the configuration is completed, receive sample data from the continuous spectrum terminal, and detect whether there is error information in the sample data, if error information is detected, re-receive the sample data; if no error information is detected, stop receiving sample data after the total number of samples is reached; The data preprocessing module is configured to: perform calibration processing on the sample data, read the antenna position data at the same time, and perform linear interpolation on the antenna position data according to the calibrated data to obtain preprocessed data; The data post-processing module is configured to: calculate the pre-processed data to obtain the target source flow.

4. The Tianma telescope continuous spectrum observation system according to claim 1, characterized in that: The data acquisition module may also be configured to: configure a clock source so as to synchronize the sampling operation of the continuous spectrum terminal with the operation of the data acquisition module receiving sample data.

5. The Tianma telescope continuous spectrum observation system according to claim 1, characterized in that: The data preprocessing module can also be configured to determine whether pointing correction is required; if necessary, perform Gaussian fitting on the preprocessed data to obtain pointing errors in the right ascension and / or declination directions, convert the pointing errors in the right ascension and / or declination directions into pointing errors in the azimuth and / or pitch directions, and then implement pointing correction.

6. The Tianma telescope continuous spectrum observation system according to claim 3, characterized in that: The data post-processing module comprises: A baseline correction module, configured to: remove background noise in the preprocessed data, and correct the angle deviation between the sample data and a preset target; A parameter calculation module is configured to: extract the amplitude of the target source signal, calculate the half-power beam width and the root mean square of the preprocessed data; A gain curve drawing module is configured to: analyze the relationship between antenna gain and elevation angle / azimuth angle according to the preprocessed data to generate a gain curve graph; The target source flow calculation module is configured to obtain the relative error related to the target source signal amplitude according to the calculation result obtained by the parameter calculation module, and convert the observed temperature of the target source into flow to obtain the target source flow.

7. The Tianma telescope continuous spectrum observation system according to claim 6, characterized in that: The target source flow calculation module is configured to obtain the maximum amplitude and standard deviation of the target source signal according to the amplitude of the target source signal, calculate the correction factor by fitting, and obtain the observed temperature of the target source after combining the maximum amplitude of the target source signal with the correction factor.

8. A method for observing the continuous spectrum of the Tianma telescope, characterized in that: include: Step S1, providing the Tianma telescope continuous spectrum observation system as described in any one of claims 1 to 7, wherein the data processing module configures the sampling frequency, center frequency and required total number of samples of the continuous spectrum terminal, and configures the clock source to synchronize the sampling operation of the continuous spectrum terminal with the operation of the data processing module receiving sample data; Step S2, receiving sample data, and detecting whether there is error information in the sample data, and if error information is detected, receiving the sample data again; If no error information is detected, the receiving of sample data stops after the total number of samples is reached; Step S3, calibrating the sample data, reading the antenna position data, and performing linear interpolation on the antenna position data according to the calibrated data to obtain preprocessed data; Step S4, calculating the preprocessed data to obtain the target source flow.

9. The Tianma telescope continuous spectrum observation method according to claim 8, characterized in that: The step S4 also includes: determining whether pointing correction is required, and if required, performing Gaussian fitting on the preprocessed data to obtain pointing errors in the right ascension and / or declination directions, converting the pointing errors in the right ascension and / or declination directions into pointing errors in the azimuth and / or pitch directions, and then implementing the pointing correction.

10. The Tianma telescope continuous spectrum observation method according to claim 8, characterized in that: The step S4 comprises: Step S41, removing background noise in the preprocessed data and correcting the angle deviation between the observed data and the preset target; Step S42, extracting the amplitude of the target source signal, calculating the half-power beam width and the root mean square of the pre-processed data; Step S43, analyzing the relationship between antenna gain and elevation angle / azimuth angle according to the preprocessed data, and generating a gain curve graph; Step S44, according to the calculation result obtained in step S42, the relative error related to the target source signal amplitude is obtained, and the observed temperature of the target source is converted into flow rate to obtain the target source flow rate.

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