The HERA-19 Commissioning Array: Direction Dependent Effects
Saul A. Kohn, James E. Aguirre, Paul La Plante, Tashalee S. Billings, Paul M. Chichura, Austin F. Fortino, Amy S. Igarashi, Roshan K. Benefo, Samavarti Gallardo… 展开作者
Saul A. Kohn, James E. Aguirre, Paul La Plante, Tashalee S. Billings, Paul M. Chichura, Austin F. Fortino, Amy S. Igarashi, Roshan K. Benefo, Samavarti Gallardo, Zachary E. Martinot, Chuneeta D. Nunhokee, Nicholas S. Kern, Philip Bull, Adrian Liu, Paul Alexander, Zaki S. Ali, Adam P. Beardsley, Gianni Bernardi, Judd D. Bowman, Richard F. Bradley, Chris L. Carilli, Carina Cheng, David R. DeBoer, Eloy de Lera Acedo, Joshua S. Dillon, Aaron Ewall-Wice, Gcobisa Fadana, Nicolas Fagnoni, Randall Fritz, Steven R. Furlanetto, Brian Glendenning, Bradley Greig, Jasper Grobbelaar, Bryna J. Hazelton, Jacqueline N. Hewitt, Jack Hickish, Daniel C. Jacobs, Austin Julius, MacCalvin Kariseb, Matthew Kolopanis, Telalo Lekalake, Anita Loots, David MacMahon, Lourence Malan, Cresshim Malgas, Matthys Maree, Nathan Mathison, Eunice Matsetela, Andrei Mesinger, Miguel F. Morales, Abraham R. Neben, Bojan Nikolic, Aaron R. Parsons, Nipanjana Patra, Samantha Pieterse, Jonathan C. Pober, Nima Razavi-Ghods, Jon Ringuette, James Robnett, Kathryn Rosie, Raddwine Sell, Craig Smith, Angelo Syce, Max Tegmark, Nithyanandan Thyagarajan, Peter K. G. Williams, Haoxuan Zheng
Foreground power dominates the measurements of interferometers that seek a statistical detection of highly-redshifted HI emission from the Epoch of Reionization (EoR). The chromaticity of the instrument creates a boundary in the Fourier transform of frequency (proportional to $k_\parallel$) between spectrally smooth emission, characteristic of the strong synchrotron foreground (the "wedge"), and the spectrally structured emission from HI in the EoR (the "EoR window"). Faraday rotation can inject spectral structure into otherwise smooth polarized foreground emission, which through instrument effects or miscalibration could possibly pollute the EoR window. Using data from the HERA 19-element commissioning array, we investigate the polarization response of this new instrument in the power spectrum domain. We perform a simple image-based calibration based on the unpolarized diffuse emission of the Global Sky Model, and show that it achieves qualitative redundancy between the nominally-redundant baselines of the array and reasonable amplitude accuracy. We construct power spectra of all fully polarized coherencies in all pseudo-Stokes parameters. We compare to simulations based on an unpolarized diffuse sky model and detailed electromagnetic simulations of the dish and feed, confirming that in Stokes I, the calibration does not add significant spectral structure beyond the expected level. Further, this calibration is stable over the 8 days of observations considered. Excess power is seen in the power spectra of the linear polarization Stokes parameters which is not easily attributable to leakage via the primary beam, and results from some combination of residual calibration errors and actual polarized emission. Stokes V is found to be highly discrepant from the expectation of zero power, strongly pointing to the need for more accurate polarized calibration.
Design and Commissioning of an LWA Swarm Station: The Long Wavelength Array -- North Arm
University of New Mexico（新墨西哥大学）；Air Force Research Laboratory, Space Vehicles Directorate（空军研究实验室空间飞行器管理局）；Curtin Institute of Radio Astronomy, Curtin University（科廷大学射电天文研究所）；United States Naval Observatory（美国海军天文台）；Hillsdale College（希尔斯代尔学院）
DragonflyPol: Wide-Field Optical Linear Polarimetry with the Dragonfly Telephoto Array (Instrument Description and Commissioning)
University of South Carolina（南卡罗来纳大学）；Stanford University（斯坦福大学）；Chiba Institute of Technology（千叶工业大学）；Hiroshima University（广岛大学）；Kyung Hee University（庆熙大学）；NRC Herzberg Astronomy & Astrophysics Research Centre（加拿大国家研究委员会赫茨伯格天文学与天体物理学研究中心）；University of Toronto（多伦多大学）
Performance of the INFN Camera calibration device of the first Large Size Telescope in the Cherenkov Telescope Array
$10^{\rm th}$ 2018年10月，在西班牙拉帕尔马加那利岛Observatorio del Roque de los Muchachos的切伦科夫望远镜阵列（CTA）北部站点开始调试第一台大尺寸望远镜（LST）原型。对于精确的事件能量重建，LST相机需要在大的动态范围内进行均匀且恒定的校准，直到$10^{4}$光电子（p.e.），对于每个摄像机光电倍增管（PMT）。本文介绍了LST-1相机标定系统（CaliBox）在第一次调试期间的性能，并提供了光平场测量的初步结果
The CHIME/FRB Outriggers: Commissioning the Hat Creek Outrigger and an Updated Calibration Scheme for Mitigating RFI
ASTRON, Netherlands Institute for Radio Astronomy（荷兰射电天文研究所）；Anton Pannekoek Institute for Astronomy, University of Amsterdam（阿姆斯特丹大学安东·潘内科克天文学研究所）；MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理学与空间研究研究所）；Department of Physics, Massachusetts Institute of Technology（麻省理工学院物理学系）
本文介绍 CHIME/FRB Outrigger 中 Hat Creek Outrigger 的调试，采用高斯过程回归校准方案缓解射频干扰，将点源灵敏度提升约 1.69-1.87 倍，并验证了该框架对大型干涉阵列的适用性。
A Python/CuPy Software Correlator for QUEST: Real-Time Performance and Initial Imaging
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；University of Chinese Academy of Sciences（中国科学院大学）；School of Arts and Sciences, Shanghai Dianji University（上海电机学院文理学院）；College of Physics and Electronic Engineering, Qilu Normal University（齐鲁师范学院物理与电子工程学院）
Commissioning An All-Sky Infrared Camera Array for Detection Of Airborne Objects
Harvard-Smithsonian Center for Astrophysics（哈佛-史密森天体物理中心）；Galileo Project（伽利略计划）；Scientific Coalition for UAP Studies（不明异常现象研究科学联盟）；Atlas Lens Co.（阿特拉斯透镜公司）
A Fast Direct Solver for Mutual Coupling Analysis of Large Arrays of Reflector Antennas
University of Cambridge（剑桥大学）；Kavli Institute for Cosmology, Cavendish Laboratory, University of Cambridge（剑桥大学卡文迪许实验室可夫利宇宙学研究所）；Queen Mary University of London（伦敦大学玛丽女王学院）；University of Manchester（曼彻斯特大学）
QUIJOTE scientific results - XX. Commissioning and First Results from the Thirty and Forty Gigahertz Instrument (TFGI)
Laboratoire de Physique Subatomique et de Cosmologie, Université Grenoble Alpes, CNRS/IN2P3（亚原子物理与宇宙学实验室，格勒诺布尔阿尔卑斯大学，法国国家科学研究中心/法国国家粒子物理研究所）；Instituto de Astrofísica de Canarias（加那利群岛天体物理研究所）；Departamento de Astrofísica, Universidad de La Laguna（拉帕尔马大学天体物理学系）；Universidade da Coruña, CITIC（科鲁尼亚大学，信息技术创新中心）；Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), UTIAS, The University of Tokyo（Kavli宇宙物理与数学研究所（ Kavli IPMU, WPI），UTIAS，东京大学）；Instituto de Fisica de Cantabria (IFCA, CSIC-UC)（坎塔布里亚物理研究所（ IFCA, 西班牙国家研究委员会-坎塔布里亚大学））
