[CII] gas in IC 342
  Methods: We used the dual-band receiver GREAT on board the SOFIA airborne
telescope to perform observations of the [C II] 158 {\mu}m fine-structure line
at the postitions of two giant molecular clouds (GMC) in the center of IC 342
(GMCs C and E) and compared the spectra with corresponding ground-based data
for low- and mid-J CO and [C I]. We performed model calculations assuming a
clumpy photo-dissociation region (PDR) environment using the KOSMA-tau PDR
model code to derive physical parameters of the local medium.
  Results: The [C II] 158 {\mu}m emission resembles the spectral signature of
ground-based atomic and molecular lines, which indicates a common origin. The
emission from GMC E can be decomposed into a cool, molecular component with
weak far-ultraviolet (FUV) fields and low, mean densities of 103 cm^-3 and a
strongly excited starburst/PDR region with higher densities of 104 cm^-3 and
FUV intensities of 250-300 Draine fields. The emission from GMC C is consistent
with gas densities of 5000 cm^-3, FUV intensities of a few Draine fields and
total gas masses of 20\times10^6 M$_\odot$.
  Conclusions: The high spectral resolution of the GREAT receiver allowed us to
decompose the [C II] emission of the GMC E into a strongly excited gas
component resembling a PDR/starburst environment and a quieter, less excited
gas component and to analyze the different components within a single beam
individually.
