67 results about "Radio astronomy" patented technology

The application discloses a kind of deep learning methods for low-frequency SKA broadband effect and synthetic beam effect elimination, belong to radio astronomy image processing field, including steps: S1, establish FSAS, FERM and FGFN;S2, based on the FSAS, FERM and FGFN of S1 establishment establishes IFS-Transformer network model;S3, two FERM modules are applied to obtain dirty image I ∈ R H×W×C Low-level features F0 ∈ R H×W×C ;S4, F0 is input FGFN module, and coding part is completed after twice downsampling operation;S5, the feature obtained by coding part is passed through 3 FSAS and twice upsampling, realizes feature learning and decoding operation;S6, after being processed by two FERM, final recovered image is obtained.The effect elimination method based on deep learning can more effectively eliminate the joint of broadband effect and synthetic beam effect, and can greatly reduce the time of effect elimination to a greater extent to restore and reconstruct original sky brightness;The manual operation process of the method of the patent can be greatly simplified by using deep learning technology.

The invention discloses a deep learning method for eliminating a low-frequency SKA broadband effect and a synthetic beam effect, and belongs to the field of radio astronomical image processing, and the method comprises the steps: S1, building an FSAS, an FERM and an FGFN; s2, establishing an IFS-Transform network model based on the FSAS, the FERM and the FGFN established in the step S1; s3, using two FERM modules to obtain low-level features F0 of the dirty image I belonging to RH * W * C, wherein the low-level features F0 belong to RH * W * C; s4, inputting the F0 into an FGFN module, and completing a coding part through two times of down-sampling operation; s5, performing three FSAS and two times of up-sampling on the features obtained by the coding part to realize feature learning and decoding operation; and S6, after two FERM processing, a final restored image is obtained. According to the effect elimination method based on deep learning, the broadband effect and the synthetic beam effect can be more effectively and jointly eliminated, the original sky brightness can be recovered and reconstructed to a greater extent, and the effect elimination time can be greatly shortened; according to the method, the manual operation process of effect elimination can be greatly simplified by adopting the deep learning technology.

The invention discloses a radio astronomical real-time data stream processing method and system based on a distributed acquisition component, and the method comprises the steps: S1, data transmission: a server receives a user datagram protocol UDP data packet transmitted by a radio astronomical telescope through a network card, and carries out the data transmission through an open-source pulsar distributed acquisition component and a data analysis system PSRDADA; creating and managing annular buffers, and transmitting data streams among the annular buffers; s2, data processing: using a CUDA (Unified Computing Device Architecture) parallel computing platform and a programming model of a GPU (Graphics Processing Unit) to write a computing and unpacking program so as to realize parallel processing and data extraction of large-scale data; and S3, writing data into a disk, writing the data blocks into the disk by using a data storage client of the PSRDADA, and dividing the data into files with any length. According to the invention, high-speed radio data streams can be received efficiently and stably, real-time processing of data is realized, and a reliable solution is provided for high-bandwidth signal transmission and processing in radio astronomical observation.

The invention provides a transient source positioning method, device and equipment based on multi-beam imaging and a storage medium, and relates to the technical field of radio astronomy observation and data processing. The method comprises the following steps: acquiring voltage data acquired by each receiving station of a radio array; constructing a beam weight tensor according to a plurality of preset target directions and the geometric structure of the radio array; and carrying out complex number tensor multiplication on the voltage data and the beam weight tensor, and synthesizing digital beams in one-to-one correspondence with all target directions in parallel. Obtaining a beam intensity sequence according to the digital beam, and mapping the beam intensity sequence to generate a two-dimensional image; and carrying out detection processing on the two-dimensional image, and identifying and positioning a temporary source. The method is used for achieving the effect of improving the positioning efficiency of the transient source according to multi-beam imaging.

The invention discloses an ultra-wideband low-profile feed source loaded with a step medium, and relates to the field of ultra-wideband feed sources. The antenna comprises four log-periodic antennas, four groups of step dielectrics, dielectric cylinders, a reflection floor, a metal cavity and two feed baluns, the four log-periodic antennas are divided into two pairs which are orthogonally arranged, each pair comprises two log-periodic antennas which are oppositely arranged, the log-periodic antennas are fixed on the dielectric cylinder through screws, and an included angle is formed between the log-periodic antennas and the reflection floor; each group of stepped dielectric is formed by arranging twelve dielectric blocks in height stepped distribution, is positioned between the log-periodic antenna and the reflection floor, and clings to the reflection floor; the two feed baluns are orthogonally arranged, and each balun comprises a dielectric substrate, an index gradient microstrip line and a one-to-two power divider. The antenna is wide in frequency band, low in profile and suitable for serving as a primary radiator of a reflector antenna in the fields of satellite communication, radar detection, radio astronomy and the like.

The invention relates to a radio astronomical electromagnetic environment simulation and construction method and system and computer equipment, and is applied to a radio astronomical electromagnetic environment simulation system, and the method comprises the steps: obtaining electromagnetic environment simulation parameters and a target environment simulation mode; determining a target simulation mode corresponding to the target environment simulation mode according to a preset corresponding relation; based on the electromagnetic environment simulation parameters, performing simulation according to a target simulation mode, and determining a target radio astronomical signal corresponding to the target environment simulation mode; obtaining a target radio frequency interference signal determined according to the electromagnetic environment simulation parameter; performing superposition processing on the target radio astronomical signal and the target radio frequency interference signal to obtain a target environment simulation signal; constructing a radio astronomical electromagnetic environment according to the target environment simulation signal; high restoration of the complex radio astronomical electromagnetic environment is achieved, and the flexibility and adaptability of simulation and construction of the radio astronomical electromagnetic environment are improved.

The invention relates to a design method and system of a small radio telescope antenna electromechanical device, and relates to the technical field of radio astronomy, and the design method comprises mechanical structure design, communication control design and man-machine interaction design, and comprises the design methods of structure optimization design, finite element analysis, manufacturing process optimization, modular virtual assembly and the like. The structural stability and the manufacturing and assembling efficiency of the antenna are effectively improved; data transmission among the servo motor driver, the azimuth pitching encoder and the motion controller is achieved through serial communication, data transmission between the motion controller and the main control computer is achieved through the Ethernet, and data transmission between the main control computer and the mobile terminal is achieved through the Internet of Things and the cloud server. By designing and optimizing control software interfaces of the fixed terminal and the mobile terminal, multi-terminal remote convenient control of the antenna is finally realized.

The present invention discloses a method and system for accelerating a radio astronomy cross-correlator based on FPGA, which relates to the field of radio astronomy. The technical solution provided by the present invention is used for the cross-correlation operation of radio array signals, stores antenna signal data on-chip and performs multi-channel segmentation in the time window dimension to achieve multi-channel parallel accumulation, improve the calculation efficiency, and adopts a streaming transmission structure and a method for reducing the data storage amount to enhance the scalability.

The utility model discloses a PCIe-based radio astronomy band-pass signal power spectrum estimation operation card, which is characterized by comprising a PPS (pulse per second) module used for receiving an input pulse per second synchronizing signal and locking the pulse per second synchronizing signal and a reference clock signal provided by a CLK clock module in a phase-locked loop mode, a clock synchronization signal of the second pulse reference is generated, and synchronous control is carried out on the DDC band-pass signal down-conversion module; the DDC band-pass signal down-conversion module is used for sequentially processing the sampling data output by the ADC sampling module according to the clock synchronization signal of the second pulse reference and then outputting the sampling data to the PFB channelization and power spectrum estimation operation module; and the PFB channelization and power spectrum estimation operation module is used for performing PFB channelization and power spectrum estimation operation on the input data to obtain a power spectrum estimation result, and transmitting the power spectrum estimation result to the PCIe interface module or the network port module for outputting. According to the invention, the flexibility of band-pass data processing is improved.

The application discloses a FAST core array broadband beam effect elimination method based on deep learning, relates to the technical field of radio astronomy image processing, and constructs an end-to-end image restoration system, which comprises the following five steps: acquiring an observation image containing a broadband beam effect; extracting multi-scale features and introducing a spatial perception mechanism; performing feature frequency domain enhancement processing and multi-scale context fusion; and outputting a multi-scale prediction image and a restored image from which the broadband beam effect is removed. The application realizes the function of improving imaging quality by constructing a deep learning model, avoids cumulative errors caused by step-by-step processing, can effectively remove broadband beam distortion, and makes the reconstructed image more close to the real sky brightness distribution in overall fidelity and structural details, and has higher physical consistency.

The present invention discloses a method and system for processing real-time radio astronomy data streams based on distributed acquisition components, including: S1. Data transmission, the server receives User Datagram Protocol (UDP) data packets transmitted by a radio astronomy telescope through a network card, uses the open-source pulsar distributed acquisition component and data analysis system PSRDADA to create and manage a circular buffer, and transfers data streams between each circular buffer; S2. Data processing, utilize the unified computing device architecture (CUDA) parallel computing platform and programming model of a graphics processing unit (GPU) to write a calculation and unpacking program, thereby realizing parallel processing and data extraction of large-scale data; S3. Data writing to disk, use the data storage client of PSRDADA to write data blocks to the disk and split the data into files of arbitrary length. The present invention can efficiently and stably receive high-speed radio data streams, realize real-time processing of data, and provide a reliable solution for high-bandwidth signal transmission and processing in radio astronomy observations.

The present invention relates to a monolithic low-noise amplifier with externally matched input port for liquid helium temperature zone, including an input matching circuit and a wide-band monolithic low-noise amplifier circuit. The input matching circuit is cascaded with the monolithic low-noise amplifier circuit, and the input port of the monolithic amplifier circuit is matched mainly through capacitors C1, C2, inductor L1 and resistor R1 to optimize the performance of the amplifier such as noise and port return loss; the monolithic low-noise amplifier circuit includes a three-level strained high electron mobility transistor, a matching circuit and a bias circuit. By adopting the low-noise amplifier disclosed in the present invention, it can be stably used in the ultra-low temperature liquid helium temperature zone, and within the wide frequency band range of 2GHz to 15GHz, the gain is greater than 32dB and the noise temperature is less than 10K. By changing the external input matching circuit, more excellent narrowband performance can be achieved. The device has the characteristics of low noise, small size, and convenient matching, and can be applied to receiving systems in the fields of deep space exploration and radio astronomy.

The invention discloses an intelligent staged compression method and system for radio astronomical data based on deep learning. The method comprises the following steps: 1) constructing a celestial body signal frequency domain template library according to observation data in the radio astronomy field; 2) mapping current observation data to be processed to a frequency domain to generate a frequency point matrix; 3) extracting a frequency domain feature of each frequency point from the frequency point matrix, performing similarity calculation on the frequency domain feature and a feature corresponding to each template, if the similarity is greater than a set threshold value, determining that the corresponding frequency point is an effective frequency point, otherwise, determining that the corresponding frequency point is an invalid frequency point; (3) the effective frequency points are analyzed and processed according to channel dimensions, and if the difference between the adjacent channel data is smaller than or equal to a difference threshold value, the difference value between the adjacent channel data is recorded in a difference coding mode; 4) performing secondary compression on the output data in the step 3); and 5) generating a standard Fits format file from the secondary compressed coding data and adding metadata parameters. According to the method, the bottleneck problem of mass data storage and transmission caused by multi-beam observation is effectively solved.

The application discloses a feed horn for radio astronomy, which comprises a first ridge and a second ridge, the first ridge and the second ridge are cross arranged; a reflection plate is arranged at the bottom of the first ridge and the second ridge, used for positioning the first ridge and the second ridge, and reflecting back radiation; a loading medium rod is arranged at the center upper part of the cross of the first ridge and the second ridge; a support plate is arranged at the top of the first ridge and the second ridge, used for mounting the loading medium rod, and further fixing the first ridge and the second ridge. The matching structure of the specially designed ridge, the reflection plate, the loading medium rod and the support plate makes the feed horn realize higher performance in a wider frequency band. The coaxial feed is adopted, which has the advantages of simple structure, low cost, small size, light weight and easy impedance matching, and meets the needs of wide frequency band radio astronomy scientific observation of 2-16GHz.

The invention relates to the technical field of radio astronomy, and discloses monopulse candidate recognition based on deep learning, comprising the following steps: S1, using Sigproc to convert a Fits file in CRAFTS data into a file in a Filterbank format; s2, generating a group of Cand files by utilizing the Heimdall; s3, converting the signal information in the Cand file into a file in an H5 format by utilizing a Python packet Your; s4, performing feature fusion on two features of frequency-time and DM-time in the H5 file; and S5, inputting the fused features into a model combined with a CNN (Convolutional Neural Network) and a Transform for identification. According to the monopulse candidate body recognition based on deep learning, CRAFTS data are preprocessed through Sigproc, Heimdall and Your tools, an optimized C-C-T-T architecture model is used for recognition, experimental results show that the accuracy rate of 99.59%, the false positive rate of 0.42% and the recall rate of 99.6% are achieved through the method, and the method is remarkably superior to an existing method; according to the method, the accuracy and recall ability of monopulse candidate body identification are improved, and an efficient and accurate research tool is provided for radio astronomy.

The invention belongs to the field of radio astronomy, and provides a monopulse signal identification system and method based on a SW architecture, and the method comprises the steps: obtaining astronomical observation original data, and carrying out the preprocessing, and obtaining the preprocessed astronomical observation data; and generating an original candidate body pulse signal list from the preprocessed astronomical observation data, visualizing the original candidate body pulse signal list to obtain a pulse image, and performing classification and recognition by using a deep neural network model optimized and trained by a SW architecture to obtain a classification result. Based on the classification result, screening a pulse image corresponding to a real classification result, and analyzing the pulse image to obtain a real candidate body pulse signal list; and a drawing sub-process is allocated for each candidate body based on the real candidate body pulse signal list, each drawing sub-process generates a dynamic spectrogram and a pulse fitting graph and then combines the dynamic spectrogram and the pulse fitting graph to obtain a candidate body graph, and the real candidate body pulse signal list and the candidate body graph are fused to obtain a pulse signal identification result.

The invention provides a radio astronomy electromagnetic interference data extraction and storage method. The method comprises the steps of obtaining original baseband data and storing the original baseband data in a PSRFITS format; defining a storage data structure; according to the original baseband data, the basic observation attribute and the file path of the PSRFITS format file, extracting to obtain an original electromagnetic interference data matrix and attribute data; the method comprises the following steps of: extracting and grouping an original electromagnetic interference data matrix to obtain a denoised data matrix with a frequency index and a time index and an attribute data key value pair set, wherein the denoised data matrix is divided into polarization and interference service frequency bands; enabling each HDF5 file to correspond to a combination of a polarization mode POL and an interference service frequency band; and storing the logic group matrix, the time index vector and the attribute data key value pair set in an HDF5 file. According to the method disclosed by the invention, the conversion from original baseband data to standardized storage is realized, and the access speed, the analysis flexibility and the long-term maintainability are considered while the data volume is obviously reduced.

The invention discloses a feed source horn for radio astronomy, and the horn comprises a first ridge piece and a second ridge piece, and the first ridge piece and the second ridge piece are disposed in a crossed manner. The reflecting plate is arranged at the bottoms of the first ridge piece and the second ridge piece and used for positioning the first ridge piece and the second ridge piece and reflecting back radiation at the same time; the loading medium rod is arranged at the upper part of the center of the intersection of the first ridge piece and the second ridge piece; the supporting plate is arranged at the top of the first ridge piece and the top of the second ridge piece and used for installing the loading medium rod and further fixing the first ridge piece and the second ridge piece at the same time. Through the specially designed matching structure of the ridge piece, the reflecting plate, the loading medium rod and the supporting plate, the feed source horn achieves higher performance in a wider frequency band. With the adoption of coaxial feed, the antenna has the advantages of simple structure, low cost, small size, light weight and easiness in impedance matching, and meets the requirements of 2-16GHz wide-band radio astronomical scientific observation.

This invention discloses a real-time imaging method and system for low-frequency radio interferometer arrays based on deep learning. The method includes: constructing a solar radio burst simulation dataset for low-frequency interferometer arrays, wherein the solar radio burst simulation dataset includes a clean target image and a simulated dirty observation image; constructing a deep learning imaging model, and performing supervised training using the simulated dirty observation image from the solar radio burst simulation dataset to obtain a trained deep learning imaging model; and performing forward propagation on the real-time observational visibility data acquired by the target low-frequency interferometer array based on the trained deep learning imaging model to obtain a reconstructed high-fidelity radio image. This invention can shorten the imaging time and improve the fidelity of the imaging results. As a real-time imaging method and system for low-frequency radio interferometer arrays based on deep learning, this invention can be widely applied in the field of radio astronomy image processing technology.

The invention relates to a beam gain constraint method for a phased array receiver, and the method comprises the steps: placing the phased array receiver in a far-field region as a receiving array, and obtaining the response of each port of the array to a reference signal and background noise through opening or closing a signal generator; a beam forming weighting coefficient is solved in combination with the steering vector and the noise correlation matrix, a corresponding beam forming network is built, a directional diagram and gain of each beam of the array after weighting are measured, a target gain is selected, a corresponding scaling factor is solved in combination with the relation between the target gain and the actually measured gain of each beam, and the beam forming network is built; and correcting the weighting coefficient of each beam by using the scaling factor, and finally achieving the purpose that the gain of each beam is constrained to the target gain. According to the method, an independent beam gain constraint unit does not need to be established, and correction of the weighting coefficient can be realized only by using an original beam calibration system, so that homogenization of each beam gain in a field range of the phased array receiver is met, and convenience is provided for the phased array receiver to realize high-resolution imaging in radio astronomical observation.

The application relates to the field of radio astronomy signal processing, and discloses a radio frequency interference reduction method and device for a phased array radio telescope, wherein the method comprises the following steps: acquiring relative position information of a plurality of navigation satellites, determining potential interference satellites from the plurality of navigation satellites according to the relative position information; acquiring a wideband signal collected by the phased array radio telescope, and determining a plurality of interfered subbands in the wideband signal; matching the interfered subbands with the potential interference satellites, and determining subband interference information of the interfered subbands according to a matching result; acquiring a signal subspace and an interference subspace of the interfered subbands, and then determining a skew projection matrix of the interfered subbands; and simultaneously performing interference reduction and digital beam forming on the interfered subbands according to the skew projection matrix and the signal subspace. The technical scheme provided by one or more embodiments of the application can realize continuous interference reduction of the phased array radio telescope on the in-orbit satellites.

The invention discloses a system and a method for measuring celestial body radiation noise based on an idle channel of a GNSS (Global Navigation Satellite System) receiver, relates to the crossing field of satellite navigation and radio astronomy detection, fully utilizes the idle channel in the receiver, realizes function expansion through firmware and algorithm upgrading, and does not need to add radio frequency hardware. This means that the idle channel and the navigation channel share the same radio frequency link in the links of the antenna, the feeder line, the low noise amplifier, the down-conversion and the like, so that the noise measurement result is consistent with the real observation condition. The deep fusion of navigation and scientific detection is realized, the baseband output is converted into a real-time radio radiation detector through statistical analysis, and the time sequence data of the equivalent noise temperature of the antenna can be continuously acquired. The data can be directly used for tasks such as sun storm monitoring, moon brightness temperature measurement, space background radiation change analysis and the like, and a real-time data source is provided for radio astronomy, space weather monitoring and planetary scientific detection.

The invention provides an image reconstruction method and device for very long baseline interference measurement data, and relates to the technical field of radio astronomy observation, and the method comprises the steps: processing the very long baseline interference measurement data of a target observation object in batches, reading the visibility data of each observation baseline, and processing the abnormal data, obtaining target visibility data; performing image deconvolution on a dirty image corresponding to the target visibility data to obtain a clean image and a clean model of the target observation object with dirty lobe interference removed; based on a target antenna gain factor corresponding to the observation baseline solved by the cleaning model, correcting observation data of the target observation object, and iteratively optimizing the cleaning model to determine a target cleaning model and correction parameters; and on the basis of the preset parameters and the target cleaning model of the at least one target observation object determined by the nonlinear least square method, the target cleaning model and the correction parameters, automatic image reconstruction is carried out, and the insufficient capacities of VLBI data batch processing, visual output and the like are relieved.

The invention relates to a linear drive unit comprising a first and second actuator element, a guiding unit configured to enable a linear relative movement between both actuator elements, a first and second power unit, each attached to the first actuator element and configured to provide the second actuator element with a respective first and second driving force, and a control unit for controlling both power units and configured to control the first and second driving force such that the first driving force can be different from the second driving force. The invention further relates to a telescope comprising a linear drive unit as well as to a method of aligning such telescope.

The invention provides a temporary source synchronous positioning method, device and equipment and a storage medium, and relates to the technical field of radio astronomical data processing. The method comprises the following steps: acquiring time domain original voltage data and image domain long-time data under the same astronomical observation scene; and carrying out parallel monitoring on the time domain original voltage data and the image domain long-time data. If a temporary source signal is monitored in any data, generating a trigger signal, and determining an imaging mode based on the trigger signal; and executing data interception according to the imaging mode to obtain short-period data. And extracting calibration information in the long-time data of the image domain, calibrating the short-time data according to the calibration information, generating a calibrated temporary source image, and outputting a positioning result of a temporary source in the temporary source image. The method is used for achieving the effect of considering the time resolution, the imaging sensitivity and the positioning precision while positioning the transient source.

The invention relates to a drive system for sensitive devices, in particular for radio astronomical devices, the drive system comprising an electric motor, a converter configured to supply a drive power to the electric motor and to control a rotational speed and / or rotational position of the electric motor, a power supply line for providing the electric motor with a drive power, and a signal line for providing the converter with a signal indicating a measured rotational speed and / or rotational position of the electric motor, wherein the drive system further comprises a shaft grounding element for grounding a drive shaft of the electric motor and wherein at least one of the power supply line and the signal line further comprises a line filter unit for filtering electromagnetic interference (EMI) signals.

The invention discloses an RDMA-based phased array radio astronomical real-time data stream transmission processing method and system, and the method comprises the steps: S1, data receiving preparation: creating a queue pair of an original data packet type at a receiving end server through the RDMA, and constructing an annular receiving buffer area; s2, flow rule configuration and data capture: creating a flow filtering rule by using an InfiniBand flow control interface, directly writing a matched data flow into an annular receiving buffer area, and bypassing an operating system kernel protocol stack; s3, real-time signal processing: performing fast Fourier transform and spectrum accumulation processing on the extracted time domain signal to generate spectrum data; and S4, data persistent storage: transmitting the processed spectrum data to a host memory, and writing the spectrum data into a disk file in batches through a buffer mechanism. According to the invention, ultra-high-speed data transmission is realized by using zero copy of the RDMA and a kernel bypass mechanism, the end-to-end delay is reduced to a microsecond level, and the throughput, real-time performance and reliability of phased array radio astronomical observation data are remarkably improved.

The present invention discloses a method for embedding U 2 The method for segmenting radio frequency interference using the ‑Net method belongs to the field of radio astronomy image segmentation technology based on deep learning. The invention comprises: simultaneously inputting the time-frequency image of radio observation data into the trained ST‑U 2 The main encoder and auxiliary encoder in the Net model extract local detail features and global context information, respectively. The intermediate feature maps of the auxiliary encoder output at each stage are fused with the intermediate feature maps of the main encoder output at each stage through the relationship aggregation module in the main encoder and then input into the decoder. The decoder then outputs a predicted segmentation mask image containing the RFI area and the non-interference area. Compared to existing deep learning RFI segmentation methods, this method has significant advantages in segmenting narrowband RFI and overall segmentation accuracy.

The invention discloses a radio astronomy radio frequency interference suppression method and system, and the method is realized based on adaptive digital filtering and spatial domain-frequency domain combined filtering, and comprises the following steps: S1, a feed source cabin receives an antenna surface reflection signal, divides the antenna surface reflection signal into two polarization signals in a vertical direction and a horizontal direction, carries out the filtering processing, and converts the polarization signals into optical signals; s2, optimizing the optical signal through an adaptive digital filtering suppression radio frequency interference algorithm in combination with the characteristics of an antenna array; s3, processing the signal through a spatial domain-frequency domain combined filtering algorithm, and suppressing interference and noise in other directions; s4, the processed astronomical signals are used for real-time observation on a display terminal of the man-machine interaction module or stored in a server for subsequent processing and analysis. According to the method and the system, ground communication signal interference is dynamically suppressed, and the directional gain of a target astronomical signal is improved, so that the problem of insufficient signal-to-noise ratio (SNR) caused by radio frequency interference (RFI) and noise in a traditional observation system is solved.

The invention discloses a radio astronomy wide temperature range adaptive beamforming method, which comprises the following steps of: 1) setting a phase temperature coefficient (ai, bi) and an amplitude temperature coefficient (ci, di) for each frequency point fi, and monitoring the environment temperature in real time; 2) generating a shared real-time temperature T real-time according to the temperature information, establishing a phase error model delta phi = ai * T real-time + bi and an amplitude error model delta A = ci * T real-time + di for each frequency point fi, and calculating phase and amplitude errors of the corresponding frequency point fi; wherein all frequency points of each channel share the real-time temperature T real-time; 3) performing DDC down-conversion on the radio frequency signal of each channel of the PAF to intermediate frequency, and converting the intermediate frequency into frequency domain data; then correcting the amplitude and phase of each frequency point in the frequency domain data; and 4) performing multi-beam synchronous output on the correction data. According to the invention, the detection requirements of a telescope on a transient celestial body, an extension source and a fine spectral line can be met.