  Herschel/SPIRE Fourier transform spectrometer (FTS) observations contain
emission from both the Herschel Telescope and the SPIRE Instrument itself, both
of which are typically orders of magnitude greater than the emission from the
astronomical source, and must be removed in order to recover the source
spectrum. The effects of the Herschel Telescope and the SPIRE Instrument are
removed during data reduction using relative spectral response calibration
curves and emission models. We present the evolution of the methods used to
derive the relative spectral response calibration curves for the SPIRE FTS. The
relationship between the calibration curves and the ultimate sensitivity of
calibrated SPIRE FTS data is discussed and the results from the derivation
methods are compared. These comparisons show that the latest derivation methods
result in calibration curves that impart a factor of between 2 and 100 less
noise to the overall error budget, which results in calibrated spectra for
individual observations whose noise is reduced by a factor of 2-3, with a gain
in the overall spectral sensitivity of 23% and 21% for the two detector bands,
respectively.
