Physics
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21741302k&link_type=abstract
American Astronomical Society, AAS Meeting #217, #413.02; Bulletin of the American Astronomical Society, Vol. 43, 2011
Physics
Scientific paper
An optimization algorithm designed by Leonid Kogan ( L. Kogan, Optimizing a Large Array Configuration to Minimize the Side lobes, IEEE Transactions on Antennas and Propagation, vol 48, NO 7, July 2000, p 1075) to minimize side-lobes in the point-spread response has been applied in the design of two new radio-interferometric arrays: (1) the most compact (E) configuration of EVLA and (2) the phased-array station for the Long Wavelength Array (LWA). Scientific programs for the EVLA's E-configuration includes galactic and Local HII, molecular gas, cosmic web, radio continum, radio lobes, SZ effect, cosmology and pulsar searches. The LWA will operate at frequencies from 10-88 MHz and will study a wide range of scientific programs including clusters of galaxies, high-redshift radio galaxies, pulsars, SNR's, extra-solar planets, solar physics and ionospheric physics. Both arrays need to be compact and to have the smallest side lobes possible. The E-configuration was designed to minimizes cost by requiring only one new railroad track in addition to the existing EVLA infrastructure. The shadowing factor achieved is reasonably good for a wide range of hour angles and declinations. The achieved side-lobe levels in the synthesized beam are no greater than 12% within the antenna primary beam for any operating VLA wavelength. For comparison, the VLA-D configuration has side-lobes near 60%. For the LWA station configuration, the sidelobes are never greater than 1.6% at any point in the sky regardless of phased direction or operating wavelength. Such small sidelobes for both arrays promise very high image fidelity for maximum scientific results.
Cohen Albert
Kogan Leonid
Ott Jorgen
Owen Frazer
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