  We present observations of the Vela X region at 31 GHz using the Cosmic
Background Imager (CBI). We find a strong compact radio source (5.9'x4.1',
FWHM) about the Vela pulsar, which we associate with the Vela pulsar wind
nebula (PWN) recently discovered at lower radio-frequencies. The CBI's 4'
resolution for a 45' field of view allows the PWN to be studied in the
large-scale context of Vela X. Filamentary structure in Vela X, which stands
out in lower frequency maps, is very low-level at 31 GHz. By combining the 10
CBI channels, which cover 26-36 GHz, and 8.4 GHz archive data, we study the
spectral energy distribution (SED) of the PWN and the brightest filaments. Our
results show that the spectral index alpha (F_{nu} propto nu^alpha) of the PWN
is flat, or even marginally positive, with a value of
alpha_{8.4}^{31}=0.10+-0.06, while the Vela X filamentary structure has a
negative spectral index of alpha_{8.4}^{31}=-0.28+-0.09. The SED inhomogeneity
observed in Vela X suggests different excitation processes between the PWN and
the filaments. We investigate whether the PWN's flat spectrum is a consequence
of variability or truly reflects the SED of the object. The peak of the PWN at
31 GHz is 80''+-20'' south-west of the peak at 8.4 GHz. This shift is confirmed
by comparing the 31 GHz CBI image with higher resolution 5 GHz Australia
Telescope Compact Array observations, and is likely to be due to SED variations
within the PWN. We also investigate the nature of the Vela X filamentary
structure.

Astrophysics