Optical studies of the galactic plane are hindered by the absorption by material in the disk of the Galaxy. The infrared window offers a much clearer view of the structure of the Milky Way and WFCAM will allow us to study individual objects and the Galaxy itself with unprecedented precision. This survey will map a large fraction of the galactic plane and will form the basis of a complete survey of the Galaxy. The 5 sigma magnitude limits of this survey are J=20.0, H=19.1, K=19.0 over a total area of ~1800 sq. degs. Additional more specialised observations of 300 sq. degs in star-formation regions with a narrow band H2 filter are also proposed.