  We present a method to derive the relative pointing offsets for SPIRE
Fourier-Transform Spectrometer (FTS) solar system object (SSO) calibration
targets, which were observed regularly throughout the Herschel mission. We
construct ratios of the spectra for all observations of a given source with
respect to a reference. The reference observation is selected iteratively to be
the one with the highest observed continuum. Assuming that any pointing offset
leads to an overall shift of the continuum level, then these ratios represent
the relative flux loss due to mispointing. The mispointing effects are more
pronounced for a smaller beam, so we consider only the FTS short wavelength
array (SSW, 958-1546 GHz) to derive a pointing correction. We obtain the
relative pointing offset by comparing the ratio to a grid of expected losses
for a model source at different distances from the centre of the beam, under
the assumption that the SSW FTS beam can be well approximated by a Gaussian. In
order to avoid dependency on the point source flux conversion, which uses a
particular observation of Uranus, we use extended source flux calibrated
spectra to construct the ratios for the SSOs. In order to account for continuum
variability, due to the changing distance from the Herschel telescope, the SSO
ratios are normalised by the expected model ratios for the corresponding
observing epoch. We confirm the accuracy of the derived pointing offset by
comparing the results with a number of control observations, where the actual
pointing of Herschel is known with good precision. Using the method we derived
pointing offsets for repeated observations of Uranus (including observations
centred on off-axis detectors), Neptune, Ceres and NGC7027. The results are
used to validate and improve the point-source flux calibration of the FTS.
