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We examine observational characteristics of multi-phase turbulent flows inthe diffuse interstellar medium (ISM) using a synthetic radiation field ofatomic and molecular lines. We consider the multi-phase ISM which is formed bythermal instability under the irradiation of UV photons with moderate visualextinction $A_V\sim 1$. Radiation field maps of C$^{+}$, C$^0$, and CO lineemissions were generated by calculating the non-local thermodynamic equilibrium(nonLTE) level populations from the results of high resolution hydrodynamicsimulations of diffuse ISM models. By analyzing synthetic radiation field ofcarbon lines of [\ion{C}{2}] 158 $\mu$m, [\ion{C}{1}] $^3P_2-^3P_1$ (809 GHz),$^3P_1-^3P_0$ (492 GHz), and CO rotational transitions, we found a high ratiobetween the lines of high- and low-excitation energies in the diffusemulti-phase interstellar medium. This shows that simultaneous observations ofthe lines of warm- and cold-gas tracers will be useful in examining the thermalstructure, and hence the origin of diffuse interstellar clouds.

Synthetic Observations of Carbon Lines of Turbulent Flows in the Diffuse Multiphase Interstellar Medium