Array Configuration for the Long Wavelength Array

Details Array Configuration for the Long Wavelength Array Array Configuration for the Long Wavelength Array

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...20713606c&link_type=abstract

American Astronomical Society Meeting 207, #136.06; Bulletin of the American Astronomical Society, Vol. 37, p.1389

Astronomy and Astrophysics

Astronomy

Scientific paper

The Long Wavelength Array (LWA) is a next-generation low-frequency telescope being built in New Mexico by the Southwest Consortium (UNM, UT-ARL, NRL, LANL). The LWA will operate at any frequency between 20 to 80 MHz. It will consist of 52 phased array-dipole stations, each acting in an equivalent way to an antenna in an interferometric array. Here, we describe a proposed array configuration and discuss its properties. Among the many considerations are: (1) adequate snapshot UV-coverage for calibration (2) sensitivity to large scale diffuse structure (3) achieving high resolution with up to 400 km baselines and (4) high imaging fidelity. Unlike the VLA, the LWA stations are not movable, so each of these goals must be achieved simultaneously with a single array configuration. The LWA is being constructed in phases, and we discuss the capabilities and considerations of each phase. Basic research in radio astronomy at the Naval Research Laboratory is supported by the Office of Naval Research.

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