  We present quantitative studies of 8 late O and early B-type supergiants in
the Magellanic Clouds using far-ultraviolet FUSE, ultraviolet IUE/HST and
optical VLT-UVES spectroscopy. Temperatures, mass-loss rates and CNO abundances
are obtained using the non-LTE, spherical, line-blanketed model atmosphere code
of Hillier & Miller (1998). We support recent results for lower temperatures of
OB-type supergiants as a result of stellar winds and blanketing, which amounts
to ~2000 K at B0 Ia. In general, H$\alpha$ derived mass-loss rates are
consistent with UV and far-UV spectroscopy, although from consideration of the
SIV $\lambda\lambda$1063-1073 doublet, clumped winds are preferred over
homogenous models. AV 235 (B0 Iaw) is a notable exception, which has an
unusually strong H$\alpha$ profile that is inconsistent with the other Balmer
lines and UV wind diagnostics. We also derive CNO abundances for our sample,
revealing substantial nitrogen enrichment, with carbon and oxygen depletion.
Our results are supported by comparison with the Galactic supergiant HD 2905
(BC0.7 Ia) for which near-solar CNO abundances are obtained. This bolsters
previous suggestions that ``normal'' OB-type supergiants exhibit atmospheric
compositions indicative of partical CNO processing.
