  We present a study of carbon in N159/N160, an HII region complex in the low
metallicity Large Magellanic Cloud. We have mapped this region, which comprises
four distinct molecular clouds spanning a wide range of star-formation
activity, in four transitions: 13CO (1-0) CO (2-1) and (4-3), and [CI] (1-0).
Combining these data with existing [CII] observations provides a complete
picture of the predominant forms of carbon in the gas phase of the ISM. The new
CO (2-1) data show that the complex is immersed in an envelope of extended, low
level emission, undetected by previous (1-0) mapping efforts. The CO
(2-1)/(1-0) ratio in this envelope is >~3, a value consistent with optically
thin CO emission. The envelope is also relatively bright in [CI] and [CII], and
calculations show that it is mostly photodissociated: it appears to be
translucent (Av<1). Neutral carbon emission in the complex unexpectedly peaks
at the quiescent southern cloud (N159S). In the northern portion of the map
(the N160 nebula), the HII regions prominent in [CII] correspond to holes in
the [CI] distribution. Overall we find that, while the [CII]/CO ratio is
enhanced with respect to similar complexes in the Milky Way, the [CI]/CO ratio
appears to be similar or reduced.
