Figure 4 from The Radio Sky at Meter Wavelengths: m-mode Analysis Imaging with the OVRO-LWA

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The Radio Sky at Meter Wavelengths: m-mode Analysis Imaging with the OVRO-LWA

Authors: Michael W. Eastwood, Marin M. Anderson, Ryan M. Monroe, Gregg Hallinan, Benjamin R. Barsdell, Stephen A. Bourke, M. A. Clark, Steven W. Ellingson, Jayce Dowell, Hugh Garsden, Lincoln J. Greenhill, Jacob M. Hartman, Jonathon Kocz, T. Joseph W. Lazio, Danny C. Price, Frank K. Schinzel, Gregory B. Taylor, Harish K. Vedantham, Yuankun Wang, and David P. Woody

2018 The Astronomical Journal 156 32.

Provider: AAS Journals

Caption: Figure 4.

Empirical fits to the OVRO-LWA Stokes I primary beam (the response of the x and y dipoles has been summed) at three frequencies: 36.528 MHz (left panel), 52.224 MHz (middle panel), and 73.152 MHz (right panel). The source tracks used to measure the beam model are overlaid. From north to south, these tracks correspond to Cas A, Cyg A, 3C 123, Tau A, Vir A, Her A, 3C 353, and Hya A. The fitting process is described in Section 3.3, and residuals for Cyg A and Cas A are in Figure 5.

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