摘要：Context.The ambiguous origin of the [C II] 158μm line in the interstellar medium complicates its use for diagnostics concerning the star-formation rate and physical conditions in photodissociation regions.Aims.We investigate the origin of [C II] in order to measure the total molecular gas content, the fraction of CO-dark H2gas, and how these parameters are impacted by environmental effects such as stellar feedback.Methods.We observed the giant H IIregion N 11 in the Large Magellanic Cloud with SOFIA/GREAT. The [C II] line is resolved in velocity and compared to H Iand CO, using a Bayesian approach to decompose the line profiles. A simple model accounting for collisions in the neutral atomic and molecular gas was used in order to derive the H2column density traced by C+.Results.The profile of [C II] most closely resembles that of CO, but the integrated [C II] line width lies between that of CO and that of H I. Using various methods, we find that [C II] mostly originates from the neutral gas. We show that [C II] mostly traces the CO-dark H2gas but there is evidence of a weak contribution from neutral atomic gas preferentially in the faintest components (as opposed to components with low [C II]/CO or low CO column density). Most of the molecular gas is CO-dark. The CO-dark H2gas, whose density is typically a few 100s cm−3and thermal pressure in the range 103.5−5K cm−3, is not always in pressure equilibrium with the neutral atomic gas. The fraction of CO-dark H2gas decreases with increasing CO column density, with a slope that seems to depend on the impinging radiation field from nearby massive stars. Finally we extend previous measurements of the photoelectric-effect heating efficiency, which we find is constant across regions probed withHerschel, with [C II] and [O I] being the main coolants in faint and diffuse, and bright and compact regions, respectively, and with polycyclic aromatic hydrocarbon emission tracing the CO-dark H2gas heating where [C II] and [O I] emit.Conclusions.We present an innovative spectral decomposition method that allows statistical trends to be derived for the molecular gas content using CO, [C II], and H Iprofiles. Our study highlights the importance of velocity-resolved photodissociation region (PDR) diagnostics and higher spatial resolution for H Iobservations as future steps.
关键词：Key wordsenISM: generalphoton-dominated regionMagellanic Cloudssubmillimeter: ISMinfrared: ISMgalaxies: star formation
