The paper Hewett et al. (2006, MNRAS, in press) is available here as a pdf file (416kb). The paper contains a large number of long tables. These tables, providing the filter transmission functions (if you wish to produce your own synthetic colours), and all the synthetic colours, are available in a tar file of ascii files (188kb). The abstract of the paper is provided below, followed by the main figures (following the numbering in the paper), to illustrate the contents.
Abstract: The UKIRT Infrared Deep Sky Survey is a set of five surveys of complementary combinations of area, depth, and Galactic latitude, which began in 2005 May. The surveys use the UKIRT Wide Field Camera (WFCAM), which has a solid angle of 0.21deg2. Here we introduce and characterise the ZYJHK photometric system of the camera, which covers the wavelength range 0.83-2.37µm. We synthesise response functions for the 5 passbands, and compute colours in the WFCAM, SDSS and 2MASS bands, for brown dwarfs, stars, galaxies and quasars of different types. We provide a recipe for others to compute colours from their own spectra. Calculations are presented in the Vega system, and the computed offsets to the AB system are provided, as well as colour equations between WFCAM filters and the SDSS and 2MASS passbands. We highlight the opportunities presented by the new Y filter at 0.97-1.07µm for surveys for hypothetical Y dwarfs (brown dwarfs cooler than T), and for quasars of very-high redshift, z>6.4.
Figure 1. Transmission curves, from above atmosphere to detector, for the WFCAM filter set. Three curves are shown for each band. The upper, thick, curve is for no atmospheric absorption. The middle, thick, curve is for the default atmospheric conditions (1.3 airmass, 1.0mm water), and the lower, thin, curve is for extreme atmospheric conditions (2.0 airmass, 5.0 mm water). These curves have been computed on the basis of measurement or modelling of the relevant wavelength-dependent quantities. An overall wavelength-independent normalisation has been applied to match the photon count rate measured for standard stars with the instrument. The calculation is preliminary and the wavelength-independent normalisation is subject to revision.