  The atmospheric abundances of elements provide essential insights into the
formation and evolution history of stars. The visible wavelength window has
been used almost exclusively in the past to determine the abundances of
chemical elements in B-type stars.
  However, some elements do not have useful spectral lines in the visible. A
high resolution spectrum of $\iota$~Herculis is available from 999 to
1400\,\AA.\ In this project, we investigate the abundance determination in the
UV. We identify the elements whose abundances can be tested, and search for
elements whose abundances can be determined in the UV to add to those in the
current literature. We also investigate the completeness of the VALD line list
in this region, and the adequacy of LTE modeling in the UV for this star. We
have used the LTE spectrum synthesis code {\sc zeeman} to model the UV spectrum
of $\iota$~Herculis for elements with 5 $\le$ Z $\le$ 80. Abundances or upper
limits are derived for 24 elements.
  We find that most of our results are in reasonable agreement with previous
results. We estimate a value or an upper limit for the abundance of nine
elements in this star that were not detected in the visible.
  LTE UV spectral synthesis is found to be a useful tool for abundance
determination, even though limitations such as incomplete and uncertain atomic
data, uncertain continuum normalization and scattered light, and severe
blending can introduce difficulties. The high abundance of two heavy elements
may be a sign of radiative levitation.
