2009ApJ...690..580W

With the goal of deriving the physical and chemical conditions of star-forming regions in the Large Magellanic Cloud (LMC), a spectral line survey of the prominent star-forming region N 113 is presented. The observations cover parts of the frequency range from 85 GHz to 357 GHz and include 63 molecular transitions from a total of 16 species, among them are the spectra of rare isotopologues. Maps of selected molecular lines as well as the 1.2 mm continuum distribution are also presented. Molecular abundances in the core of the complex are consistent with a photon-dominated region in a nitrogen deficient environment. While carbon monoxide (CO) shows optical depths of the order of τ ∼ 10, ¹³CO is optically thin. The most prominent lines of carbon monosulfide (CS), HCN, and HCO⁺show signs of weak saturation (τ ∼ 0.5). Densities range from 5x10³/cm3 for CO to almost 10⁶ for CS, HCN, and a few other species, indicating that only the densest regions provide sufficient shielding, even for some of the most common species. An ortho- to para-formaldehyde (H₂CO) ratio of ∼ 3 hints at H₂ CO formation in a warm (≳ 40 K) environment. Isotope ratios are ¹²C/¹³C ∼ 49±5, ¹⁶O/¹⁸O ∼2000±250, ¹⁸O/¹⁷O ∼ 1.7±0.2, and ³²S/³⁴S ∼ 15. Agreement with data from other star-forming clouds shows that the gas is well mixed in the LMC. The isotope ratios not only differ from those seen in the Galaxy, they also do not form a continuation of the trends observed with decreasing metallicity from the inner to the outer Galaxy. This implies that the outer Galaxy, even though showing an intermediate metallicity, is not providing a transition zone between the inner Galaxy and the metal-poor environment of the Magellanic Clouds. A part of this discrepancy is likely caused by differences in the age of the stellar populations in the outer Galaxy and the LMC. While, however, this scenario readily explains measured carbon and oxygen isotope ratios, nitrogen and sulfur still lack a self-consistent interpretation.