We propose to use SWS and LWS to observe the IR continuum and fine
structure lines of trace elements in H II regions in the far outer
Galaxy (R = 14-28 kpc).  These data will permit abundance determinations
for the interstellar medium near and beyond the edge of the optical disk
of the Milky Way and will constrain models of star formation and
Galactic chemical evolution.  The H II regions we propose to study
include the one at the greatest known Galactocentric distance.  The H II
regions and their associated molecular clouds are well characterized:
all have been mapped in CO and either in the radio continuum or in the
H-alpha line.