Research in Astronomy and Astrophysics最新文献_第5页

Morphology Study for GeV Emission of the Nearby Supernova Remnant G332.5-5.6 邻近超新星剩余物 G332.5-5.6 的 GeV 发射形态研究

Research in Astronomy and Astrophysics Pub Date : 2024-03-09 DOI: 10.1088/1674-4527/ad3287

Ming-Hong Luo, Qing-Wen Tang, Xiu-Rong Mo

引用次数: 0

Four late-type galaxies with double radio lobes and properties of such galaxies 四个具有双射电叶的晚期类型星系及其特性

Research in Astronomy and Astrophysics Pub Date : 2024-03-05 DOI: 10.1088/1674-4527/ad304c

Z. Yuan, XuYang Gao, Z. L. Wen, Jinlin Han

{"title":"Four late-type galaxies with double radio lobes and properties of such galaxies","authors":"Z. Yuan, XuYang Gao, Z. L. Wen, Jinlin Han","doi":"10.1088/1674-4527/ad304c","DOIUrl":"https://doi.org/10.1088/1674-4527/ad304c","url":null,"abstract":"\u0000 Triggering mechanism for radio lobes from late-type galaxies is not fully understood. More samples are desired for a thorough investigation and statistics. By utilizing the optical data from the newly released Dark Energy Spectroscopic Instrument imaging surveys and the radio sources from the NRAO VLA Sky Survey and the Faint Images of the Radio Sky at Twenty-centimeter, we identify four Late-type Galaxies with double Radio Lobes (LaGRLs): J0217-3645, J0947+6220, J1412+3723 and J1736+5108. Including previously known LaGRLs, we confirm the correlation between radio power P1.4GHz and stellar mass M∗ of host galaxies. Most (25/35) LaGRLs belong to the blue cloud galaxies, while the newly-identified cases in this work are located within the region of red sequence. We find a clear correlation between the differential radio power, i.e., the offset from the P1.4GHz-M∗ relation, and the galaxy color, indicating that bluer galaxies at a fixed M∗ tend to host more powerful radio lobes. Furthermore, majority (31/36) LaGRLs are either located in a galaxy group or display a disturbed morphology. We suggest that all of the galaxy mass, color and surrounding environment could play important roles in triggering radio lobes in late-type galaxies.","PeriodicalId":509923,"journal":{"name":"Research in Astronomy and Astrophysics","volume":"113 25","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-03-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140079305","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

BSN: Photometric Light Curve Analysis of Two Contact Binary Systems LS Del and V997 Cyg BSN：两个接触双星系统 LS Del 和 V997 Cyg 的光度光曲线分析

Research in Astronomy and Astrophysics Pub Date : 2024-03-04 DOI: 10.1088/1674-4527/ad30b2

A. Poro, M. Tanrıver, Elham Sarvari, Shayan Zavvarei, Hossein Azarara, Laurent Corp, Sabrina Baudart, Asma Ababafi, Nazanin Kahali Poor, Fariba Zare, Ahmet Bulut, Ahmet Keskin

{"title":"BSN: Photometric Light Curve Analysis of Two Contact Binary Systems LS Del and V997 Cyg","authors":"A. Poro, M. Tanrıver, Elham Sarvari, Shayan Zavvarei, Hossein Azarara, Laurent Corp, Sabrina Baudart, Asma Ababafi, Nazanin Kahali Poor, Fariba Zare, Ahmet Bulut, Ahmet Keskin","doi":"10.1088/1674-4527/ad30b2","DOIUrl":"https://doi.org/10.1088/1674-4527/ad30b2","url":null,"abstract":"\u0000 The light curve analyses and orbital period variations for two W Ursae Majoris (W UMa) binary stars, LS Del and V997 Cyg, were presented in this work which was conducted in the frame of the Binary Systems of South and North (BSN) Project. Ground-based photometric observations were performed at two observatories in France. We used TESS (The Transiting Exoplanet Survey Satellite) data for extracting times of minima and light curve analysis of the target systems. The O-C diagram for both systems displays a parabolic trend. LS Del and V997 Cyg's orbital periods are increasing at a rate of $dP/dt= 7.20times10^{-08}$ $d yr^{-1}$ and $dP/dt= 2.54times10^{-08}$ $d yr^{-1}$, respectively. Therefore, it can be concluded that the mass is being transferred from the less massive star to the more massive component with a rate of $dM/dt=-1.96times10^{-7}$ $M_odot$ $yr^{-1}$ for LS Del system, and $dM/dt=-3.83times10^{-7}$ $M_odot$ $yr^{-1}$ for V997 Cyg. The parameters of the third possible object in the system were also considered. The PHysics Of Eclipsing BinariEs (PHOEBE) Python code was used to analyze the light curves. The light curve solutions needed a cold starspot due to the asymmetry in the LS Del system's light curve maxima. The mass ratio, fill-out factor, and star temperature all indicate that both systems are contact binary types in this investigation. Two methods were used to estimate the absolute parameters of the systems: one method used the parallax of Gaia Data Release 3 (EDR3), and the other used a $P-M$ relationship. The positions of the systems were also depicted on the $M-L$, $M-R$, $q-L_{ratio}$, and $logM_{tot}-logJ_0$ diagrams.","PeriodicalId":509923,"journal":{"name":"Research in Astronomy and Astrophysics","volume":"15 S1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-03-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140266188","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Inverse Calculation and Regularization Process for the Solar Aspect System (SAS) of HXI Payload on ASO-S Spacecraft ASO-S 航天器上 HXI 有效载荷的太阳视角系统 (SAS) 的逆计算和正则化过程

Research in Astronomy and Astrophysics Pub Date : 2024-02-10 DOI: 10.1088/1674-4527/ad283b

Jirui Yu, Ping Ruan, Yang Su, Yi-Jing He, Jin-you Tao, Zhe Zhang, Song Guo, Bin Xue, Jian Feng Yang

{"title":"Inverse Calculation and Regularization Process for the Solar Aspect System (SAS) of HXI Payload on ASO-S Spacecraft","authors":"Jirui Yu, Ping Ruan, Yang Su, Yi-Jing He, Jin-you Tao, Zhe Zhang, Song Guo, Bin Xue, Jian Feng Yang","doi":"10.1088/1674-4527/ad283b","DOIUrl":"https://doi.org/10.1088/1674-4527/ad283b","url":null,"abstract":"\u0000 For the ASO-S/HXI payload, the accuracy of the flare reconstruction is reliant on important factors such as the alignment of the dual grating and the precise measurement of observation orientation. To guarantee optimal functionality of the instrument throughout its life cycle, the SAS is imperative to ensure that measurements are accurate and reliable. This is achieved by capturing the target motion and utilizing a physical model-based inversion algorithm. However, the SAS optical system's inversion model is a typical ill-posed inverse problem due to its optical parameters, which results in small target sampling errors triggering unacceptable shifts in the solution. To enhance inversion accuracy and make it more robust against observation errors, we suggest dividing the inversion operation into two stages based on the SAS spot motion model. Firstly, the as-rigid-as-possible (ARAP) transformation algorithm calculates the relative rotations and an intermediate variable between the substrates. Secondly, we solve an inversion linear equation for the relative translation of the substrates, the offset of the optical axes, and the observation orientation. To address the ill-posed challenge, the Tikhonov method grounded on the discrepancy criterion and the maximum a posteriori (MAP) method founded on the Bayesian framework are utilized. The simulation results exhibit that the ARAP method achieves a solution with a rotational error of roughly ±3.5 arcsec (1/2-quantile); both regularization techniques are successful in enhancing the stability of the solution, the variance of error in the MAP method is even smaller - it achieves a translational error of approximately ±18μm (1/2-quantile) in comparison to the Tikhonov method's error of around ±24μm (1/2-quantile). Furthermore, the SAS practical application data indicates the method's usability in this study. Lastly, this paper discusses the intrinsic interconnections between the regularization methods.","PeriodicalId":509923,"journal":{"name":"Research in Astronomy and Astrophysics","volume":" 515","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139787370","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Inverse Calculation and Regularization Process for the Solar Aspect System (SAS) of HXI Payload on ASO-S Spacecraft ASO-S 航天器上 HXI 有效载荷的太阳视角系统 (SAS) 的逆计算和正则化过程

Research in Astronomy and Astrophysics Pub Date : 2024-02-10 DOI: 10.1088/1674-4527/ad283b

Jirui Yu, Ping Ruan, Yang Su, Yi-Jing He, Jin-you Tao, Zhe Zhang, Song Guo, Bin Xue, Jian Feng Yang

{"title":"Inverse Calculation and Regularization Process for the Solar Aspect System (SAS) of HXI Payload on ASO-S Spacecraft","authors":"Jirui Yu, Ping Ruan, Yang Su, Yi-Jing He, Jin-you Tao, Zhe Zhang, Song Guo, Bin Xue, Jian Feng Yang","doi":"10.1088/1674-4527/ad283b","DOIUrl":"https://doi.org/10.1088/1674-4527/ad283b","url":null,"abstract":"\u0000 For the ASO-S/HXI payload, the accuracy of the flare reconstruction is reliant on important factors such as the alignment of the dual grating and the precise measurement of observation orientation. To guarantee optimal functionality of the instrument throughout its life cycle, the SAS is imperative to ensure that measurements are accurate and reliable. This is achieved by capturing the target motion and utilizing a physical model-based inversion algorithm. However, the SAS optical system's inversion model is a typical ill-posed inverse problem due to its optical parameters, which results in small target sampling errors triggering unacceptable shifts in the solution. To enhance inversion accuracy and make it more robust against observation errors, we suggest dividing the inversion operation into two stages based on the SAS spot motion model. Firstly, the as-rigid-as-possible (ARAP) transformation algorithm calculates the relative rotations and an intermediate variable between the substrates. Secondly, we solve an inversion linear equation for the relative translation of the substrates, the offset of the optical axes, and the observation orientation. To address the ill-posed challenge, the Tikhonov method grounded on the discrepancy criterion and the maximum a posteriori (MAP) method founded on the Bayesian framework are utilized. The simulation results exhibit that the ARAP method achieves a solution with a rotational error of roughly ±3.5 arcsec (1/2-quantile); both regularization techniques are successful in enhancing the stability of the solution, the variance of error in the MAP method is even smaller - it achieves a translational error of approximately ±18μm (1/2-quantile) in comparison to the Tikhonov method's error of around ±24μm (1/2-quantile). Furthermore, the SAS practical application data indicates the method's usability in this study. Lastly, this paper discusses the intrinsic interconnections between the regularization methods.","PeriodicalId":509923,"journal":{"name":"Research in Astronomy and Astrophysics","volume":"56 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139846908","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

All-Sky Guide Star Catalog For CSST CSST 全天空导星目录

Research in Astronomy and Astrophysics Pub Date : 2024-02-06 DOI: 10.1088/1674-4527/ad26b6

HuiMei Feng, Zi-Huang Cao, Man I Lam, Ran Li, Chao Liu

{"title":"All-Sky Guide Star Catalog For CSST","authors":"HuiMei Feng, Zi-Huang Cao, Man I Lam, Ran Li, Chao Liu","doi":"10.1088/1674-4527/ad26b6","DOIUrl":"https://doi.org/10.1088/1674-4527/ad26b6","url":null,"abstract":"\u0000 The China Space Station Telescope (CSST) is a 2-meter space telescope with multiple back-end instruments. The Fine Guidance Sensor (FGS) is an essential subsystem of the CSST Precision Image Stability System (PISS) to ensure the required absolute pointing accuracy and line-of-sight stabilization. In this study, we construct the Main Guide Star Catalog for FGS. To accomplish this, we utilize the information about the FGS and object information from the Gaia Data Release 3. We provide an FGS instrument magnitude and exclude variables, binaries, and high proper motion stars from the catalog to ensure uniform FGS guidance capabilities. Subsequently, we generate a HEALPix index, which provides a hierarchical tessellation of the celestial sphere, and employ the Voronoi algorithm to achieve a homogeneous distribution of stars across the catalog. This distribution ensures adequate coverage and sampling of the sky. The performance of the CSST guide star catalog was assessed by simulating the field of view of the FGS according to the CSST mock survey strategy catalog. The analysis of the results indicates that this catalog provides adequate coverage and accuracy. The catalog’s performance meets the FGS requirements, ensuring the functioning of the FGS and its guidance capabilities.","PeriodicalId":509923,"journal":{"name":"Research in Astronomy and Astrophysics","volume":"48 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139859801","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

All-Sky Guide Star Catalog For CSST CSST 全天空导星目录

Research in Astronomy and Astrophysics Pub Date : 2024-02-06 DOI: 10.1088/1674-4527/ad26b6

HuiMei Feng, Zi-Huang Cao, Man I Lam, Ran Li, Chao Liu

{"title":"All-Sky Guide Star Catalog For CSST","authors":"HuiMei Feng, Zi-Huang Cao, Man I Lam, Ran Li, Chao Liu","doi":"10.1088/1674-4527/ad26b6","DOIUrl":"https://doi.org/10.1088/1674-4527/ad26b6","url":null,"abstract":"\u0000 The China Space Station Telescope (CSST) is a 2-meter space telescope with multiple back-end instruments. The Fine Guidance Sensor (FGS) is an essential subsystem of the CSST Precision Image Stability System (PISS) to ensure the required absolute pointing accuracy and line-of-sight stabilization. In this study, we construct the Main Guide Star Catalog for FGS. To accomplish this, we utilize the information about the FGS and object information from the Gaia Data Release 3. We provide an FGS instrument magnitude and exclude variables, binaries, and high proper motion stars from the catalog to ensure uniform FGS guidance capabilities. Subsequently, we generate a HEALPix index, which provides a hierarchical tessellation of the celestial sphere, and employ the Voronoi algorithm to achieve a homogeneous distribution of stars across the catalog. This distribution ensures adequate coverage and sampling of the sky. The performance of the CSST guide star catalog was assessed by simulating the field of view of the FGS according to the CSST mock survey strategy catalog. The analysis of the results indicates that this catalog provides adequate coverage and accuracy. The catalog’s performance meets the FGS requirements, ensuring the functioning of the FGS and its guidance capabilities.","PeriodicalId":509923,"journal":{"name":"Research in Astronomy and Astrophysics","volume":"88 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139799849","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

A Quick Calculation Method for Radiation Pattern of Submillimeter Telescope with Deformation and Displacement 具有形变和位移的亚毫米波望远镜辐射模式的快速计算方法

Research in Astronomy and Astrophysics Pub Date : 2024-02-02 DOI: 10.1088/1674-4527/ad256e

Jia You, Yiwei Yao, Zheng Wang

{"title":"A Quick Calculation Method for Radiation Pattern of Submillimeter Telescope with Deformation and Displacement","authors":"Jia You, Yiwei Yao, Zheng Wang","doi":"10.1088/1674-4527/ad256e","DOIUrl":"https://doi.org/10.1088/1674-4527/ad256e","url":null,"abstract":"\u0000 Radiation pattern captures the electromagnetic performance of reflector antennas, which is significantly affected by the deformation of the primary reflector due to gravity and the displacement of the secondary reflector. During the design process of large reflector antennas, a substantial amount of time is often dedicated to iteratively adjusting structural parameters and validating electromagnetic performance. To improve the efficiency of the de- sign process, we first propose an approximate calculation method of optical path difference (OPD) for the deformation of the primary reflector under gravity and the displacement of the secondary reflector. Then an OPD fitting function based on the modified Zernike poly- nomials is proposed to capture the phase difference of radiation over the aperture plane, based on which the radiation pattern will be obtained quickly by the aperture field integration method. Numerical experiments demonstrate the effectiveness of the proposed quick calcula- tion method for analyzing the radiation pattern of a 10.4-m submillimeter telescope antenna at its highest operating frequency of 856 GHz. In comparison with the numerical simula- tion method based on GRASP (which is an antenna electromagnetic analysis tool combining physical optics (PO) and physical theory of diffraction (PTD)), the quick calculation method reduces the time for radiation pattern analysis from more than one hour to less than two min- utes. Furthermore, the quick calculation method exhibits excellent accuracy for the figure of merit (FOM) of the radiation pattern. Therefore, the proposed quick calculation method can obtain the radiation pattern with high speed and accuracy. Compared to the time-consuming numerical simulation method (PO and PTD), it can be employed for quick analysis of the radiation pattern for the lateral displacement of the secondary reflector and the deformation of the primary reflector under gravity in the design process of the reflector antenna.","PeriodicalId":509923,"journal":{"name":"Research in Astronomy and Astrophysics","volume":"18 S14","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139810423","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

A Quick Calculation Method for Radiation Pattern of Submillimeter Telescope with Deformation and Displacement 具有形变和位移的亚毫米波望远镜辐射模式的快速计算方法

Research in Astronomy and Astrophysics Pub Date : 2024-02-02 DOI: 10.1088/1674-4527/ad256e

Jia You, Yiwei Yao, Zheng Wang

{"title":"A Quick Calculation Method for Radiation Pattern of Submillimeter Telescope with Deformation and Displacement","authors":"Jia You, Yiwei Yao, Zheng Wang","doi":"10.1088/1674-4527/ad256e","DOIUrl":"https://doi.org/10.1088/1674-4527/ad256e","url":null,"abstract":"\u0000 Radiation pattern captures the electromagnetic performance of reflector antennas, which is significantly affected by the deformation of the primary reflector due to gravity and the displacement of the secondary reflector. During the design process of large reflector antennas, a substantial amount of time is often dedicated to iteratively adjusting structural parameters and validating electromagnetic performance. To improve the efficiency of the de- sign process, we first propose an approximate calculation method of optical path difference (OPD) for the deformation of the primary reflector under gravity and the displacement of the secondary reflector. Then an OPD fitting function based on the modified Zernike poly- nomials is proposed to capture the phase difference of radiation over the aperture plane, based on which the radiation pattern will be obtained quickly by the aperture field integration method. Numerical experiments demonstrate the effectiveness of the proposed quick calcula- tion method for analyzing the radiation pattern of a 10.4-m submillimeter telescope antenna at its highest operating frequency of 856 GHz. In comparison with the numerical simula- tion method based on GRASP (which is an antenna electromagnetic analysis tool combining physical optics (PO) and physical theory of diffraction (PTD)), the quick calculation method reduces the time for radiation pattern analysis from more than one hour to less than two min- utes. Furthermore, the quick calculation method exhibits excellent accuracy for the figure of merit (FOM) of the radiation pattern. Therefore, the proposed quick calculation method can obtain the radiation pattern with high speed and accuracy. Compared to the time-consuming numerical simulation method (PO and PTD), it can be employed for quick analysis of the radiation pattern for the lateral displacement of the secondary reflector and the deformation of the primary reflector under gravity in the design process of the reflector antenna.","PeriodicalId":509923,"journal":{"name":"Research in Astronomy and Astrophysics","volume":"13 10","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139870161","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Development of a Front End Array for Broadband Phased Array Receiver 为宽带相控阵接收器开发前端阵列

Research in Astronomy and Astrophysics Pub Date : 2024-02-01 DOI: 10.1088/1674-4527/ad24f6

Kai Wang, Liang Cao, Jun Ma, X. Duan, Hao Yan, Mao-zheng Chen, Yun-Wei Ning

{"title":"Development of a Front End Array for Broadband Phased Array Receiver","authors":"Kai Wang, Liang Cao, Jun Ma, X. Duan, Hao Yan, Mao-zheng Chen, Yun-Wei Ning","doi":"10.1088/1674-4527/ad24f6","DOIUrl":"https://doi.org/10.1088/1674-4527/ad24f6","url":null,"abstract":"\u0000 The receiver is a signal receiving device placed at the focus of the telescope. In order to improve the observation efficiency, the concept of phased array receiver has been proposed in recent years, which places a small phased array at the focal plane of the reflector, and flexible pattern and beam scanning functions can be achieved through a beamforming network. If combined with the element multiplexing, all beams within the entire field of view can be observed simultaneously to achieve continuous sky coverage. This article focuses on the front-end array of phased array receiver at 0.7-1.8 GHz for QiTai Telescope, and designs a Vivaldi antenna array of PCB structure with dual line polarization. Each polarization antenna is designed to arrange in a rectangle manner by 11 × 10. Based on the simulation results of the focal field, 32, 18 and 8 elements were selected to form one beam at 0.7, 1.25 and 1.8 GHz. A analog beamforming network was constructed, and the measured gains of axial beam under uniform weighting were 19.32, 13.72 and 15.22 dBi. Combining the beam scanning method of reflector antenna, the pattern test of different position element sets required for PAF beam scanning was carried out under independent array. The pattern optimization at 1.25 GHz was carried out by weighting method of conjugate field matching. Compared with uniform weighting, the gain, sidelobe level, and main beam direction under conjugate field matching have been improved. Although the above test and simulation results are slightly different, which is related to the passive array and laboratory testing condition, the relevant work has accumulated experience in the development of front-end array for phased array receiver, and has good guiding significance for future performance verification after the array is installed on the telescope.","PeriodicalId":509923,"journal":{"name":"Research in Astronomy and Astrophysics","volume":"10 4","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139817213","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0