  We observed Hubble V, the brightest HII region complex in the dwarf irregular
galaxy NGC 6822, at near-infrared (1.8--2.4 um) wavelengths using the Cooled
Grating Spectrometer 4 (CGS4) at the United Kingdom Infra-Red Telescope
(UKIRT). The line emission maps of Hubble V show the typical structure of a
photo-dissociation region (PDR) where an ionized core, traced by compact He I
emission (2.0587 um) and Br_gamma emission (2.1661 um), is surrounded by an
outer layer traced by molecular hydrogen (H_2) emission. The measured line
ratios of H_2 2-1 S(1) (2.2477 um) / 1-0 S(1) (2.1218 um) from 0.2 to 0.6 and
the un-shifted and un-resolved line profiles suggest that the H_2 emission
originates purely from a PDR. By comparing the H_2 results with a PDR model, we
conclude that Hubble V includes dense (10^{4.5} cm^{-3}) and warm PDRs. In this
environment, most of the H_2 molecules are excited by far-UV photons (with a
field strength of 10^{2-4} times that of the average interstellar field),
although collisional processes de-excite H_2 and contribute significantly to
the excitation of the first vibrational level. We expect that Hubble V is in
the early stage of molecular cloud dissolution.
