Capabilities of the Expanded Very Large Array (EVLA) for Astronomical Surveys.

Details Capabilities of the Expanded Very Large Array (EVLA) for Astronomical Surveys. Capabilities of the Expanded Very Large Array (EVLA) for Astronomical Surveys.

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21535703m&link_type=abstract

American Astronomical Society, AAS Meeting #215, #357.03; Bulletin of the American Astronomical Society, Vol. 42, p.541

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Scientific paper

The Expanded Very Large Array (EVLA, Perley et al. 2009, arXiv:0909.1585) is a program to significantly upgrade the capabilities of the VLA through replacement of the receivers, electronics, signal paths, and correlator with cutting-edge technology. This has significant impact upon the capabilities of the VLA for carrying out large continuum and lines surveys from 1-50 GHz, as well as in key bands below 1 GHz, with continuum sensitivity and spectral survey speeds increased by factors of 100 or more in select cases. Science targets relevant to large surveys include galactic observations of diffuse gas and compact objects, local group and distant galaxies, high-redshift molecular lines, super-massive black holes throughout the Universe, and pulsars, supernovae, and other transient events. The EVLA becomes available to general users starting in March 2010, with a phased increase in offered capabilities over the next few years. In this presentation, I describe the salient features of the EVLA for survey work, and summarize the complementary nature of prospective radio survey and follow-up observations to those in other wavebands, such as those with ALMA and next generation optical, infrared, X-ray and Gamma-ray telescopes. Where possible, example data taken from EVLA commissioning tests is used to illustrate these features. I also describe possible future evolution of the EVLA as the nucleus of a "North America Array" (NAA), a realization of a high-frequency component of the Square Kilometer Array (SKA).

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