[CII] gas in IC 342
M. R\"ollig, R. Simon, R. G\"usten, J. Stutzki, H. W., H\"ubers, P. Hartogh, K.Jacobs, X. Guan, F. Israel

TL;DR
This study uses SOFIA observations to analyze the [C II] 158 μm emission in IC 342's molecular clouds, revealing distinct physical conditions and excitation mechanisms within the clouds.
Contribution
It provides detailed decomposition of [C II] emission into different gas components and applies PDR modeling to derive physical parameters of the local medium.
Findings
GMC E has both a cool, low-density component and a highly excited starburst/PDR region.
GMC C exhibits high gas density and moderate FUV intensity, with a large gas mass.
High spectral resolution enables separation of different gas components within a single beam.
Abstract
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…
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