We propose to study far-infrared line and continuum emission from HII regions
with unusually narrow radio recombination lines.  Compared with most star
forming regions, these objects require both very low electron temperature
(T_e<~4600 K) and small nonthermal line broadening in the ionized gas. The low
temperatures could be the result of high abundances, low electron density,
and/or low effective stellar temperature. The origin of the lack of nonthermal
broadening is more speculative, but may be produced by low density and the
absence of density gradients and stellar winds. By probing both the ionized gas
and the adjacent photodissociated material, the proposed FIR line measurements
([SIII] (33 microns), [SIV] (10.5 microns), and [SiII] (35 microns))
together with measurements already obtained during calibration of the LWS
([OIII] (52 and 88 microns), [NIII] 57 microns), [OI] (63 and 146
microns), [NII] (122 microns), and [CII] (158 microns), and the 43-173
micron continuum) on the same objects will determine the physical conditions
which are responsible for the low temperature and the lack of nonthermal line
broadening.