Velocity resolved [CII], [CI], and CO observations of the N159
  star-forming region in the Large Magellanic Cloud: a complex velocity
  structure and variation of the column densities
  The [CII]158um line is one of the dominant cooling lines in star-forming
active regions. The commonly assumed clumpy UV-penetrated cloud models predict
a [CII] line profile similar to that of CO. However, recent spectral-resolved
observations show that they are often very different, indicating a more complex
origin of the line emission including the dynamics of the source region. The
aim of our study is to investigate the physical properties of the star-forming
ISM in the Large Magellanic Cloud (LMC) by separating the origin of the
emission lines spatially and spectrally. In this paper, we focus on the
spectral characteristics and the origin of the emission lines, and the phases
of carbon-bearing species in the N159 star-forming region in the LMC. We mapped
a 4'x(3-4)' region in N159 in [CII]158um and [NII]205um with the GREAT on board
SOFIA, and in CO(3-2), (4-3), (6-5), 13CO(3-2), and [CI]3P1-3P0 and 3P2-3P1
with APEX. The emission of all transitions observed shows a large variation in
the line profiles across the map and between the different species. At most
positions the [CII] emission line profile is substantially wider than that of
CO and [CI]. We estimated the fraction of the [CII] integrated line emission
that cannot be fitted by the CO line profile to be 20%-50%. We derived the
relative contribution from C+, C, and CO to the column density in each velocity
bin. The contribution from C+ dominates the velocity range far from the
velocities traced by the dense molecular gas, and the region located between
the CO cores of N159 W and E. We estimate the contribution of the ionized gas
to the [CII] emission using the ratio to the [NII] emission to be < 19% to the
[CII] emission at its peak position, and <15% over the whole observed region.
Using the integrated line intensities, we present the spatial distribution of
I([CII])/I(FIR). (abridged for arXiv)
