The Square Kilometre Array (SKA)

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Deep spectroscopy of a young radio source at z = 0.521

Astronomische Nachrichten Wiley 327:2‐3 (2006) 171-174

Authors:

KJ Inskip, D Lee, G Cotter, ACS Readhead, TJ Pearson
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Very Small Array. Flux density at 33GHz (Cleary+, 2005)

VizieR Online Data Catalog 736 (2006) 340-340

Authors:

KA Cleary, AC Taylor, E Waldram, RA Battye, C Dickinson, RD Davies, RJ Davis, R Genova-Santos, K Grainge, ME Jones, R Kneissl, GG Pooley, R Rebolo, JA Rubino-Martin, RDE Saunders, PF Scott, A Slosar, D Titterington, RA Watson

Very Small Array. Flux density at 33GHz (Cleary+, 2005)

VizieR Online Data Catalog 736 (2006) 340-340

Authors:

KA Cleary, AC Taylor, E Waldram, RA Battye, C Dickinson, RD Davies, RJ Davis, R Genova-Santos, K Grainge, ME Jones, R Kneissl, GG Pooley, R Rebolo, JA Rubino-Martin, RDE Saunders, PF Scott, A Slosar, D Titterington, RA Watson

VizieR Online Data Catalog: Very Small Array. Flux density at 33GHz (Cleary+, 2005)

VizieR Online Data Catalog 736 (2006) 340-340

Authors:

KA Cleary, AC Taylor, E Waldram, RA Battye, C Dickinson, RD Davies, RJ Davis, R Genova-Santos, K Grainge, ME Jones, R Kneissl, GG Pooley, R Rebolo, JA Rubino-Martin, RDE Saunders, PF Scott, A Slosar, D Titterington, RA Watson

Adapting and expanding interferometric arrays

ArXiv astro-ph/0602578 (2006)

Authors:

A Karastergiou, R Neri, MA Gurwell

Abstract:

We outline here a simple yet efficient method for finding optimized configurations of the elements of radio-astronomical interferometers with fixed pad locations. The method can be successfully applied, as we demonstrate, to define new configurations when changes to the array take place. This may include the addition of new pads or new antennas, or the loss of pads or antennas. Our method is based on identifying which placement of elements provides the most appropriate uv plane sampling for astronomical imaging.
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