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Project Organization
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(Scientific Advisory
Group for EVLA)
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USEFUL LINKS:
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The Expanded Very Large Array Project
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The Expanded Very Large Array Project:
A Radio Telescope to Resolve Cosmic Evolution
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| 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:
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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.
To learn more about the EVLA, including its two phases, click on EVLA Phase I or EVLA Phase II on the left panel.
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