  We present spectral results from a multi-satellite, broad-band campaign on
the Narrow-line Seyfert 1 galaxy Ton S180 performed at the end of 1999. We
discuss the spectral-energy distribution of the source, combining simultaneous
Chandra, ASCA and EUVE data with contemporaneous FUSE, HST, and ground-based
optical and infra-red data. The resulting SED shows that most of the energy is
emitted in the 10 -- 100 eV regime, which must be dominated by the primary
energy source. No spectral turnover is evident in the UV regime. This, the
strong soft X-ray emission, and the overall shape of the SED indicate that
emission from the accretion disk peaks between 15 and 100 eV. High resolution
FUSE spectra showing UV absorption due to O VI and the lack of detectable X-ray
absorption in the Chandra spectrum demonstrate the presence of a low column
density of highly ionized gas along our line-of-sight. The highly-ionized state
of the circumnuclear gas is most likely linked to the high luminosity and steep
spectrum of the active nucleus. Given the strong ionizing flux in Ton S180, it
is possible that the clouds within a few tens of light days of the central
source are too highly ionized to produce much line emission. Thus the narrow
width of the emission lines in Ton S180 is due to the emission arising from
large radii.
