  We report the first detection of [CI] (3P1-3P0) emission at 609 um in a
region of the Small Magellanic Cloud (N27). Environments poor in heavy elements
and dust such as the SMC are thought to be dominated by photodissociation
regions. This is the lowest metallicity source where submillimeter neutral
carbon emission has been detected. Studying the [CI]/CO intensity ratio in
several sources spanning more than an order of magnitude in metallicity, Z, we
find that the [CI]/CO ratio increases for decreasing Z. The existence of such a
trend points to a photodissociation origin for most of neutral carbon in
molecular clouds, in agreement with standard PDR models. We also report ISO FIR
spectroscopic observations of N27, and use them to derive its physical
properties. Comparison between the density and radiation field revealed by FIR
diagnostics (n~300-1000 cm-3, Xuv~30-100 Xo) and those derived from millimeter
and submillimeter data (n~10^5 cm-3, Xuv<30 Xo) suggests that the FIR lines
originate in more diffuse gas, and are perhaps dominated by the interclump
medium. Regardless of the cause, analysis of the FIR and mm-submm data produces
a discrepancy of two orders of magnitude for the density of this source.
