Integral field unit data

Figure: A schematic view of the way in which the IFU reformats a two dimensional field of view into a staggered column of slices, which is then used as the input to the UIST long-slit spectrometer (four of the eighteen slices are not usable due to misalignment during manufacture of the slicing mirrors).

The UIST integral field unit slices a rectangular region of the sky into strips and rearranges them in order to use them as the input to the UIST long slit spectrometer, as shown in Figure . Note that the slice images on the array are not in the same order as the slices on the sky. The offsets from one slice to another in the dispersion direction lead to an apparent offset in wavelength from one spectrum to another. These data reduction recipes are designed to transform this raw output into a datacube with (x, y, $\lambda$) axes, which will be divided by a standard-star spectrum and flux calibrated if appropriate.