2004/12/30 by R. G. Strom, Strom, R. G.
Computer Science · Engineering · Physics and Astronomy · #Adaptive optics and wavefront sensing #Advanced Measurement and Metrology Techniques #Astronomical Observations and Instrumentation #Astrophysics (astro-ph) #FOS: Physical sciences #Optical measurement and interference techniques #Particle Accelerators and Free-Electron Lasers #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0412687
2 pages. no figures. Proceedings of the 7th European VLBI Network Symposium held in Toledo, Spain on October 12-15, 2004. Editors: R. Bachiller, F. Colomer, J.-F. Desmurs, P. de Vicente (Observatorio Astronomico Nacional), p. 273-274. Needs evn2004.cls
arxiv created 2004/12/30 · openalex publication_date 2004/12/30 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The EVN stations encompass elements with a range of diameters, even including\nan interferometer (the Westerbork Telescope, with up to 14 elements used\ntogether as a tied array). In combination, the various station pairs will each\nproduce their own primary beam envelopes, with which the interferometer pattern\nis modulated. People sometimes forget that in the case of unequal elements,\nthis combined primary beam envelope is different from the beam of each element\nseparately. The reason for this is reviewed, the results for a number of\nstation pairs are summarized, and some of the practical consequences are\ndiscussed. The increased interest in wide-field applications, as illustrated by\nseveral recent results, underlines the need for a proper determination of the\ninterferometer beam envelope.\n