2004/12/13 by Huib Jan van Langevelde, H. J. van Langevelde, H. Verkouter +13
Engineering · Physics and Astronomy · #Adaptive optics and wavefront sensing #Astronomical Observations and Instrumentation #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #FOS: Physical sciences #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0412292
2 pages, 1 figure. 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. 249-251. Needs evn2004.cls
arxiv created 2004/12/13 · openalex publication_date 2004/12/13 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The EVN MkIV data processor is being equipped with a high data output capability, called PCInt. In its next phase it will allow very high data output rates, up to 160 Mb/s. This functionality is required for the high spectral resolution that will be offered with recirculation. Moreover, VLBI observations traditionally focus on a small patch of sky and image typically a few 100 mas around a bright source. High spectral and time resolution is needed to image a larger area of the sky, up to the primary beam of the individual telescopes. After the upgrade such high resolution data will become the standard product. From the archive of high resolution data it will be possible to image many sources in each field of view around the original targets.