Determine the CNM–UNM transition temperature in the LMC
Determine the temperature boundary between the cold neutral medium and thermally unstable neutral medium in the Large Magellanic Cloud, accounting for its lower metallicity and stronger ultraviolet radiation field.
References
However, this criterion may not be directly applicable to the LMC. As shown in Figure~\ref{fig:cdf_comp}, the spin temperatures in the LMC are systematically lower than those in the Milky Way, suggesting that the boundary between CNM and UNM may also shift to lower temperatures in a lower metallicity and higher UV radiation environment. Quantifying this shift is challenging. In our sample, we identify 34 components with $T_s > 100$ K, including 4 with $T_s \sim 200$ K and 2 with $T_s \sim 600$ K. While the classification of components with moderate temperatures ($T_s \sim 100$â200 K) remains uncertain, the two components with $T_s \sim 600$ K are well above any plausible CNMâUNM boundary and can be robustly identified as UNM.