  Wilhelm et al. have recently called attention to the unidentified broad
emission features near 117 nm in the solar spectrum. They discuss the observed
properties of these features in detail but do not identify the source of this
emission.
  We show that the broad autoionizing transitions of neutral sulfur are
responsible for these emission features. Autoionizing lines of \ion{S}{i} occur
throughout the spectrum between Lyman alpha and the Lyman limit. Sulfur is a
normal contributor to stellar spectra.
  We use non-LTE chromospheric model calculations with line data from the
Kurucz 2004 \ion{S}{i} line list to simulate the solar spectrum in the range
116 to 118 nm. We compare the results with SUMER disk-center observations from
Curdt et al. and limb observations from Wilhelm et al.
  Our calculations generally agree with the SUMER observations of the broad
autoionizing \ion{S}{i} emission features, the narrow \ion{S}{i} emission
lines, and the continuum in this wavelength region, and agree with basic
characteristics of the center-to-limb observations. In addition to modeling the
average spectrum, we show that a change of $\pm$ 200 K in the temperature
distribution causes the intensity to change by a factor of 4. This exceeds the
observed intensity variations 1) with time in quiet regions at these
wavelengths, and 2) with position from cell centers to bright network. These
results do not seem compatible with current dynamical models that have temporal
variations of 1000 K or more in the low chromosphere.
