First results from the Super-Extended Very Small Array.

Anna Scaife

University of Cambridge

Standard Features:

• Negligible pointing error

• Negligible beam uncertainty

• Dedicated source subtractor

• Tracking elements allow fringe-rate filtering

COMPACT EXTENDED SUPER-EXTENDED

Dickinson et al. 2004

New Features:

• 60 cm parabolic mirrors

• Longer baselines

• Upgraded front-end amplifiers

• Broad-banded source subtraction

Source Subtraction:

1. NVSS and First Catalogues at 1.4GHz.

2. Ryle Observations at 15GHz.

3. VSA Source Subtractor at 33GHz.

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.

Excess emission seen by CBI at high multipoles.

Prediction of Super-Extended VSA performance for Deep Field

observing program.

Cluster Sample

Cluster RA(J2000) δ(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 7.9A2409 22 00 52.8 +20 58 15 0.1470 6.7 7.6

Abell 655

&

Abell 646

Model parameters obtained from X-ray fits

and lensing data are then used with the SZ

data to estimate H0 and fg.

Prediction of Super-Extended VSA performance using mosaic-ed fields to constrain 4th and 5th peaks.

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