  Recent analysis of Gemini-North/NIFS H-band (1.45 - 1.8 $\mu$m) observations
of Uranus, recorded in 2010, with recently updated line data has revealed the
spectral signature of hydrogen sulphide (H$_2$S) in Uranus's atmosphere (Irwin
et al., 2018). Here, we extend this analysis to Gemini-North/NIFS observations
of Neptune recorded in 2009 and find a similar detection of H$_2$S spectral
absorption features in the 1.57 - 1.58 $\mu$m range, albeit slightly less
evident, and retrieve a mole fraction of $\sim1-3$ ppm at the cloud tops. We
find a much clearer detection (and much higher retrieved column abundance above
the clouds) at southern polar latitudes compared with equatorial latitudes,
which suggests a higher relative humidity of H$_2$S here. We find our retrieved
H$_2$S abundances are most consistent with atmospheric models that have reduced
methane abundance near Neptune's south pole, consistent with HST/STIS
determinations (Karkoschka and Tomasko, 2011). We also conducted a Principal
Component Analysis (PCA) of the Neptune and Uranus data and found that in the
1.57 - 1.60 $\mu$m range, some of the Empirical Orthogonal Functions (EOFs)
mapped closely to physically significant quantities, with one being strongly
correlated with the modelled H$_2$S signal and clearly mapping the spatial
dependence of its spectral detectability. Just as for Uranus, the detection of
H$_2$S at the cloud tops constrains the deep bulk sulphur/nitrogen abundance to
exceed unity (i.e. $ > 4.4 - 5.0$ times the solar value) in Neptune's bulk
atmosphere, provided that ammonia is not sequestered at great depths, and
places a lower limit on its mole fraction below the observed cloud of (0.4 -
1.3) $\times 10^{-5}$. The detection of gaseous H$_2$S at these pressure levels
adds to the weight of evidence that the principal constituent of the 2.5 -
3.5-bar cloud is likely to be H$_2$S ice.
