  The shape of the spectral energy distribution of active galaxies in the
EUV--soft X-ray band (13.6 eV to 1 keV) is uncertain because obscuration by
dust and gas can hamper our view of the continuum. To investigate the shape of
the spectral energy distribution in this energy band, we have generated a set
of photoionization models which reproduce the small dispersion found in
correlations between high-ionization mid-infrared emission lines in a sample of
hard X-ray selected AGN. Our calculations show that a broken power-law
continuum model is sufficient to reproduce the [Ne V]14.32 mm/[NeIII], [Ne
V]24.32mm/[O IV]25.89mm and [O IV] 25.89mm/[Ne III] ratios, and does not
require the addition of a "big bump" EUV model component. We constrain the
EUV--soft X-ray slope, alpha_i, to be between 1.5 -- 2.0 and derive a best fit
of alpha_i ~ 1.9 for Seyfert 1 galaxies, consistent with previous studies of
intermediate redshift quasars. If we assume a blue bump model, most sources in
our sample have derived temperatures between T_{BB}=10^{5.18} K to 10^{5.7} K,
suggesting that the peak of this component spans a large range of energies
extending from ~ lambda 600A to lambda 1900A. In this case, the best fitting
peak energy that matches the mid-infrared line ratios of Seyfert 1 galaxies
occurs between ~ lambda 700--1000A. Despite the fact that our results do not
rule out the presence of an EUV bump, we conclude that our power-law model
produces enough photons with energies > 4 Ry to generate the observed amount of
mid-infrared emission in our sample of BAT AGN.
