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tokens: survive and maintain high levels of molecular gas fraction. To support this explanation, there is a noticeable difference in the number of YSOs detected in the Southern Pillars (>800) and in the western region where the Northern Cloud is (∼100), suggesting a lower level of triggered star formation toward the direction of the denser gas (Smith et al. 2010b ). 4.1.3. 8 <italic>μ</italic>m Figure 10 shows a comparison between the radio continuum emission and the 8 μ m image from Spitzer. In general, we detect some anticorrelation between the two tracers, with the radio continuum emission filling the cavities observed in the 8 μ m map. A Spearman’s rank correlation between the two images gives a value of 0.42, which indicates a poor level of correlation. As 8 μ m traces the polycyclic aromatic hydrocarbon (PAH) emission, it will be bright on the surfaces of the clouds being radiated by the nearby massive stars. Now, with the radio continuum map in hand, we are able to witness the complex distribution of the different gas phases in Carina, which deviates strongly from the classical view of a spherical region expanding symmetrically into the surrounding ISM. Because of the exquisite detail of our radio continuum image, we can see that the hot gas can indeed permeate through the molecular cloud and shape the material into features such as pillars, small shells, and arc-like structures. Figure 10. Color-composite image of the CNC-Gum 31 complex. Green shows the Spitzer IRAC 8 μ m map, while red shows the ATCA continuum image. A clear spatial anticorrelation between the two tracers is observed, with the radio continuum emission filling the cavities observed in the 8 μ m map. The 8 μ m map traces the PAH emission, so it will be bright on the cloud’s surfaces. Orange arrows show the apparent direction of the hot gas traced by the radio continuum map as it permeates through the denser gas, illuminating the cloud surfaces as traced by PAH emission. As the ionization fronts advance through the cloud, they can penetrate deep toward low-density regions and ultimately escape. Figure 4 shows structures resembling “plumes” at the edges of the H ii region. These features are likely to be tracing hot gas that had eroded the material in the nebula, extending to outside the molecular cloud, and now diffusing with the global component of the hot gas in the Galactic plane at distances >100 pc. There is clear alignment between the morphology of the illuminated gas traced by PAH emission and the plume-shaped structures traced by the radio continuum map. The direction of the elongated structures identified in the northeast section of the 8 μ m map (such as pillars and walls) is roughly the same as the direction of the plumes detected in the radio continuum (Figure 4 ). This correlation is more evident toward the Southern Pillars region, where the radio continuum emission is distributed along the cavities between the pillars. 4.1.4. 70 <italic>μ</italic>m In Figure 11 we