The Very Small Array ( VSA ) has been used to survey the \ell \sim 27 ^ { \circ } to \sim 46 ^ { \circ } , | { \it { b } } | < 4 ^ { \circ } region of the Galactic plane at a resolution of 13 arcmin .
This \ell -range covers a section through the Local , Sagittarius and the Cetus spiral arms .
The survey consists of 44 pointings of the VSA , each with a r.m.s .
sensitivity of \sim 90 mJy beam ^ { -1 } .
These data are combined in a mosaic to produce a map of the area .
The majority of the sources within the map are HII regions .

The main aim of the programme was to investigate the anomalous radio emission from the warm dust in individual HII regions of the survey .
This programme required making a spectrum extending from GHz frequencies to the FIR IRAS frequencies for each of 9 strong sources selected to lie in unconfused areas .
It was necessary to process each of the frequency maps with the same u , v coverage as was used for the VSA 33 GHz observations .
The additional radio data were at 1.4 , 2.7 , 4.85 , 8.35 , 10.55 , 14.35 and 94 GHz in addition to the 100 , 60 , 25 and 12 \mu m IRAS bands .
From each spectrum the free-free , thermal dust and anomalous dust emission were determined for each HII region .
The mean ratio of 33 GHz anomalous flux density to FIR 100 \mu m flux density for the 9 selected HII regions was \Delta S ( 33 ~ { } { GHz } ) / S ( 100 ~ { } \mu m ) = 1.10 \pm 0.21 \times 10 ^ { -4 } .
When combined with 6 HII regions previously observed with the VSA and the CBI , the anomalous emission from warm dust in HII regions is detected with a 33 GHz emissivity of 4.65 \pm 0.40 \mu K ( MJy/sr ) ^ { -1 } ( 11.5 \sigma ) .
This level of anomalous emission is 0.3 to 0.5 of that detected in cool dust clouds .

A radio spectrum of the HII region anomalous emission covering GHz frequencies is constructed .
It has the shape expected for spinning dust comprised of very small grains .
The anomalous radio emission in HII regions is on average 41 \pm 10 per cent of the radio continuum at 33 GHz .
Another result is that the excess ( i.e .
non-free-free ) emission from HII regions at 94 GHz correlates strongly with the 100 \mu m emission ; it is also inversely correlated with the dust temperature .
Both these latter results are as expected for very large grain dust emission .
The anomalous emission on the other hand is expected to originate in very small spinning grains and correlates more closely with the 25 \mu m emission .