Full-polarization primary beam patterns of MeerKAT antennas have been measured in L-band (856 to 1711 MHz) by means of radio holography using celestial targets. This paper presents the observed frequency dependent properties of these beams, and guides users of this 64 antenna radio telescope that are concerned by its direction dependent polarization effects. In this work the effects on the primary beams due to modeling simplifications, bandwidth averaging, gravitational loading and ambient temperature are quantified within the half power region of the beam. A perspective is provided on the level of significance of typical use case effects. It is shown that antenna pointing is a leading cause of inaccuracy for telescope users in the presumed beam shape, introducing errors exceeding 1% in power near the half power point of beams, owing to a telescope pointing accuracy of $σ\approx 0.6$ arcminutes. Disregarding these pointing errors, variability in the Stokes I beam shape relative to the array average is most commonly around 0.3% in power; however, the impact above 1500 MHz is on average triple that of the lower half of the band. This happens because the proportion of higher order waveguide modes that are activated and propagate is sensitive to small manufacturing differences in the orthomode transducer for each receiver. Primary beam correction verification test results for an off-axis spectral index measurement experiment are included.
Breakthrough Listen's Automated Commensal Technosignature Survey with MeerKAT
University of Oxford（牛津大学）；Berkeley SETI Research Center, University of California, Berkeley（加州大学伯克利分校伯克利SETI研究中心）；SETI Institute（SETI研究所）；Department of Physics and Astronomy, University of New Mexico（新墨西哥大学物理与天文学系）；LPC2E, OSUC, Univ Orleans, CNRS, CNES, Observatoire de Paris（奥尔良大学、CNRS、CNES、巴黎天文台 LPC2E 联合实验室）；South African Radio Astronomy Observatory（南非射电天文观测站）
A direction-dependent framework for visibility plane mosaicing and primary beam correction
Centre for Radio Astronomy Techniques and Technologies (RATT), Department of Physics and Electronics, Rhodes University（罗德岛大学物理与电子学院射电天文技术与理论中心）；INAF – Istituto di Radioastronomia（意大利国家天体物理研究所射电天文研究所）；GEPI & USN, Observatoire de Paris, CNRS, Université Paris Diderot（巴黎天文台GEPI与USN实验室，CNRS，巴黎第七大学）；South African Radio Astronomy Observatory（南非射电天文观测台）
The MeerKLASS On-the-Fly continuum survey: pipeline design and validation
University of the Western Cape（西开普大学）；South African Radio Astronomy Observatory（南非射电天文台）；LMU Faculty of Physics（慕尼黑大学物理学院）；The University of Manchester（曼彻斯特大学）；Victoria University of Wellington（惠灵顿维多利亚大学）；Rhodes University（罗德斯大学）；National Institute of Astrophysics (INAF IRA)（意大利国家天体物理研究所）
State Key Laboratory of Radio Astronomy and Technology, National Astronomical Observatories, CAS（中国科学院国家天文台射电天文与技术重点实验室）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文学与空间科学学院）
Direct Primary Beam Correction: Untangling Mutual Coupling in 21-cm Cosmological Experiments with the SKA-Low Radio Telescope
University of Cambridge（剑桥大学）；Kavli Institute for Cosmology in Cambridge, University of Cambridge（剑桥卡弗里宇宙学研究所）；Queen Mary, University of London（伦敦大学玛丽女王学院）；University of Manchester（曼彻斯特大学）；KTH Royal Institute of Technology（瑞典皇家理工学院）
Measurement of the Primary Beam of the Tianlai Cylindrical Antenna Using an Unmanned Aerial Vehicle
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；State Key Laboratory of Radio Astronomy and Technology（射电天文技术国家重点实验室）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）
Full Characterisation of the Polarisation Primary Beam of the GRAO 32-m Telescope
Ghana Space Science and Technology Institute Ghana Atomic Energy Commission（加纳空间科学与研究所 加纳原子能委员会）；University of California Santa Cruz（加州大学圣克鲁兹分校）；University of Nigeria Nsukka（尼日利亚恩苏卡大学）
