& B15455 & & &\
\
[09$^{\rm h}$11$^{\rm m}$33$\stackrel{\rm s}{.}$72]{} & [$-$64$^{\circ}$56249]{} & W6022 & & & B11345& & &\
[09$^{\rm h}$11$^{\rm m}$36$\stackrel{\rm s}{.}$59]{} & [$-$64$^{\circ}$58010]{} & W6849 & & & B23335& & &\
[09$^{\rm h}$11$^{\rm m}$37$\stackrel{\rm s}{.}$53]{} & [$-$64$^{\circ}$53311]{} & W7084 & & & B26161 & & &\
[09$^{\rm h}$11$^{\rm m}$42$\stackrel{\rm s}{.}$47]{} & [$-$64$^{\circ}$56571]{} & W8750 & & & B25082& & &\
[09$^{\rm h}$11$^{\rm m}$36$\stackrel{\rm s}{.}$34]{} & [$-$64$^{\circ}$54077]{} & W9855 & & & B24578 & & &\
[09$^{\rm h}$11$^{\rm m}$45$\stackrel{\rm s}{.}$79]{} & [$-$64$^{\circ}$56271]{} & W9863 & & & B16326& & &\

UIT observations
----------------

We would like to compare the results of our ground-based spectroscopy with the positions of our target stars in the UV colour-magnitude diagram. Unfortunately, we cannot use the UV colour-magnitude diagram of Brown et al. ([@brsw01]) because all of their stars lie within 35 of the cluster center and are thus too crowded for ground-based spectroscopy. As an alternative, we have derived new 1520 Å photometry of stars in the outer region of NGC 2808 using archival UIT images. The UIT photometry of NGC 2808 has not been previously published, although optical spectroscopy of three UV-bright stars on the image was presented by Moehler et 