  We present submillimeter observations of the Local Group, metal-poor,
irregular dwarf galaxy IC 10, directly relevant to the interaction between
interstellar medium and star formation activity in primeval galaxies. Using the
JCMT, we have observed the fine structure neutral carbon transition at 492 GHz
and the rotational J=3-2 transition of 12CO and 13CO in the most massive giant
molecular cloud complex in this galaxy, IC10-SE. We find that, although the
I([CII])/I(CO) ratio for this object is a factor of 4 larger than the typical
Milky Way value, its [C~I] to CO intensity ratio is I([CI])/I(CO)~18 is similar
(only about 50% larger) to that of the Milky Way. Modelling of the [CII]/CO and
[CI]/CO intensity ratios with metallicity indicates that, if C+ and C are
chiefly produced by UV photodissociation, both ratios should increase sharply
with decreasing metallicity (and consequently diminished UV shielding; Bolatto,
Jackson, and Ingalls 1999). These data then suggest a different origin for an
important fraction of C in these clouds, unrelated to photodissociation. We
have also mapped the 850 um continuum in this region using SCUBA. Employing
these data in conjunction with KAO and IRAM measurements we find an extremely
low emissivity exponent, b~0.5. We conclude that this low exponent is most
likely due to the destruction of small dust grains, brought about by the
increased penetration of UV radiation in the low metallicity ISM. If a low b in
the submillimeter is a general property of metal-poor systems then the
interpretation of millimeter and submillimeter surveys of high-z galaxies
should be revised.
