SuperCAM CO(3-2) APEX survey at 6 pc resolution in the Small Magellanic Clouds

Abstract

We present the CO(3-2) APEX survey at 6 pc resolution of the bar of the SMC. We aboard the CO analysis in the SMC-Bar comparing the CO(3-2) survey with that of the CO(2-1) of similar resolution. We study the CO(3-2)-to-CO(2-1) ratio (R32) that is very sensitive to the environment properties (e.g., star-forming regions). We analyzed the correlation of this ratio with observational quantities that trace the star formation as the local CO emission, the Spitzer color [70/160], and the total IR surface brightness measured from the Spitzer and Herschel bands. For the identification of the CO(3-2) clouds, we used the CPROPS algorithm, which allowed us to measure the physical properties of the clouds. We analyzed the scaling relationships of such physical properties. We obtained an R32 of 0.65 as a median value for the SMC, with a standard deviation of 0.3. We found that R32 varies from region to region, depending on the star formation activity. In regions dominated by HII and photo-dissociated regions (e.g., N22, N66), R32 tends to be higher than the median values. Meanwhile, lower values were found toward quiescent clouds. We also found that R32 correlates positively with the IR color [70/160] and the total IR surface brightness. This finding indicates that R32 increases with environmental properties like the dust temperature, the total gas density, and the radiation field. We have identified 225 molecular clouds with sizes R > 1.5 pc and signal-to-noise (S/N) ratio > 3 and only 17 well-resolved CO(3-2) clouds increasing the S/N ratio to > 5. These 17 clouds follow consistent scaling relationships to the inner Milky Way clouds but with some departure. The CO(3-2) tends to be less turbulent and less luminous than the inner Milky Way clouds of similar size. Finally, we estimated a median virial-based CO-to-H2 conversion factor of 12.6_{-7}^{+10} Msun/(K km s^{-1} pc^{2}) for the total sample.

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Cited by in corpus (1)

• ALMA 0.1 pc View of Molecular Clouds Associated with High-Mass Protostellar Systems in the Small Magellanic Cloud: Are Low-Metallicity Clouds Filamentary or Not?