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VLA Expansion Project

The Expanded Very Large Array Project:
A Radio Telescope to Resolve Cosmic Evolution


The EVLA Project will provide a radio telescope of unprecedented sensitivity, resolution, and imaging capability by modernizing and extending the existing Very Large Array. When completed, the EVLA will provide the following capabilities:

  • Sensitivity: Continuum sensitivity improvement over the VLA by factors of 5 to 20, to give point-source sensitivity better than 1 microJy between 2 and 40 GHz.
  • Frequency Accessibility: Operation at any frequency between 1.0 and 50 GHz, with up to 8 GHz bandwidth per polarization.
  • Spectral Capability: Full polarization (8 GHz bandwidth per polarization), with a minimum of 16,384 channels, frequency resolution to 1 Hz, and 128 independently tunable sub-bands.
  • Resolution: Angular resolution up to 200 / (frequency in GHz) milliarcseconds with tens of Kelvin brightness temperature sensitivity at full resolution.
  • Low-Brightness Capability: Fast, high fidelity imaging of extended low-brightness emission with tens of arcseond resolution and microKelvin brightness sensitivity.
  • Imaging Capability: Spatial dynamic range greater than 106, frequency dynamic range greater than 105, image field of view greater than 109 with full spatial frequency samplng.
  • Operations: Dynamic scheduling, based on weather, array configuration, and science requirements. "Default" images automatically produced, with all data products archived.

  • An aerial view of the Very Large Array located on the Plains of San Agustin, New Mexico

    Last modified by Gene Cole
    on: 03 June 2009
    Thursday, 26-Feb-2009 17:52:06 MST