  New line lists are presented for the two most abundant water isotopologues;
H$_{2}$$^{16}$O and H$_{2}$$^{18}$O. The H$_{2}$$^{16}$O line list extends to
25710 cm$^{-1}$ with intensity stabilities provided via ratios of calculated
intensities obtained from two different semi-empirical potential energy
surfaces. The line list for H$_{2}$$^{18}$O extends to 20000 cm$^{-1}$. The
minimum intensity considered for all is $10^{-30}$ cm molecule$^{-1}$ at 296~K,
assuming 100\% abundance for each isotopologue. Fluctuation of calculated
intensities caused by changes in the underlying potential energy are found to
be significant, particularly for weak transitions. Direct comparisons are made
against eighteen different sources of line intensities, both experimental and
theoretical, many of which are used within the HITRAN2016 database. With some
exceptions, there is excellent agreement between our line lists and the
experimental intensities in HITRAN2016. In the infrared region, many
H$_{2}$$^{16}$O bands which exhibit intensity differences of 5-10\% between to
the most recent 'POKAZATEL' line list (Polyansky \textit{et al.}, [Mon. Not.
Roy. Astron. Soc. \textbf{480}, 2597 (2018)] and observation, are now generally
predicted to within 1\%. For H$_{2}$$^{18}$O, there are systematic differences
in the strongest intensities calculated in this work versus those obtained from
semi-empirical calculations. In the visible, computed cross sections show
smaller residuals between our work and both HITRAN2016 and HITEMP2010 than
POKAZATEL. While our line list accurately reproduces HITEMP2010 cross sections
in the observed region, residuals produced from this comparison do however
highlight the need to update line positions in the visible spectrum of
HITEMP2010. These line lists will be used to update many transition intensities
and line positions in the HITRAN2016 database.
