  We present deep Ka-band ($\nu \approx 33$ GHz) observations of the CMB made
with the extended Very Small Array (VSA). This configuration produces a
naturally weighted synthesized FWHM beamwidth of $\sim 11$ arcmin which covers
an $\ell$-range of 300 to 1500. On these scales, foreground extragalactic
sources can be a major source of contamination to the CMB anisotropy. This
problem has been alleviated by identifying sources at 15 GHz with the Ryle
Telescope and then monitoring these sources at 33 GHz using a single baseline
interferometer co-located with the VSA. Sources with flux densities $\gtsim 20$
mJy at 33 GHz are subtracted from the data. In addition, we calculate a
statistical correction for the small residual contribution from weaker sources
that are below the detection limit of the survey.
  The CMB power spectrum corrected for Galactic foregrounds and extragalactic
point sources is presented. A total $\ell$-range of 150-1500 is achieved by
combining the complete extended array data with earlier VSA data in a compact
configuration. Our resolution of $\Delta \ell \approx 60$ allows the first 3
acoustic peaks to be clearly delineated. The is achieved by using mosaiced
observations in 7 regions covering a total area of 82 sq. degrees. There is
good agreement with WMAP data up to $\ell=700$ where WMAP data run out of
resolution. For higher $\ell$-values out to $\ell = 1500$, the agreement in
power spectrum amplitudes with other experiments is also very good despite
differences in frequency and observing technique.
