First results from the SuperExtended Very Small Array'

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First results from the Super-Extended Very Small
Array.

• Anna Scaife
• University of Cambridge

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• Standard Features
• Negligible pointing error
• Negligible beam uncertainty
• Dedicated source subtractor
• Tracking elements allow fringe-rate filtering

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COMPACT EXTENDED SUPER-EXTENDED
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Dickinson et al. 2004
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• New Features
• 60 cm parabolic mirrors
• Longer baselines
• Upgraded front-end amplifiers
• Broad-banded source subtraction

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• Source Subtraction
• NVSS and First Catalogues at 1.4GHz.
• Ryle Observations at 15GHz.
• VSA Source Subtractor at 33GHz.

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Science objectives of the Super-Extended
VSA 1. Investigate excess emission at high
multipoles 2. SZ observations of moderate
redshift clusters 3. Mosaic observations to
constrain 4th and 5th peaks.
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Excess emission seen by CBI at high multipoles.
Prediction of Super-Extended VSA performance for
Deep Field observing program.
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Cluster Sample

• Cluster RA(J2000) d(J2000) z nH
  (cm2) Te (keV)
• A646 08 22 09.7 47 06 00 0.1303 3.8
  5.3
• A655 08 25 30.3 47 07 48 0.1267 4.3
  7.1
• A795 09 24 05.7 14 10 06 0.1357 3.5
  6.6
• A990 10 23 41.3 49 07 58 0.1440 1.0
  6.4
• A1033 10 31 43.6 35 02 58 0.1259 1.9
  6.3
• A1068 10 40 43.9 39 56 53 0.1372 1.3
  3.8
• A1361 11 43 30.3 46 23 04 0.1167 2.2
  5.5
• A1413 11 55 18.5 23 24 27 0.1427 1.6
  6.6
• A2034 15 10 11.7 33 30 53 0.1130 1.5
  7.9
• A2409 22 00 52.8 20 58 15 0.1470 6.7
  7.6

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Abell 655 Abell 646
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Model parameters obtained from X-ray fits and
lensing data are then used with the SZ data to
estimate H0 and fg.
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Prediction of Super-Extended VSA performance
using mosaic-ed fields to constrain 4th and 5th
peaks.
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Conclusions The upgrade of the Very Small Array
to its Super-Extended configuration has been
completed. Initial cluster observations have
measured decrements towards clusters in the
selected sample. Deep field observations of
primary anisotropies have begun. 4th and 5th
peaks Mosaic-ed observation program