Molecular gas in M83 consists of two log-normal density components, with the high-density component enhanced along spiral arms and more tightly linked to star formation than the low-density component.
On the Density Distribution in Star-forming Interstellar Clouds
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abstract
We use deep adaptive mesh refinement simulations of isothermal self-gravitating supersonic turbulence to study the imprints of gravity on the mass density distribution in molecular clouds. The simulations show that the density distribution in self-gravitating clouds develops an extended power-law tail at high densities on top of the usual lognormal. We associate the origin of the tail with self-similar collapse solutions and predict the power index values in the range from -7/4 to -3/2 that agree with both simulations and observations of star-forming molecular clouds.
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Observational study of G12.79+0.43 identifies YSOs and HII regions powered by B-type stars and associates the complex with the rim of a molecular superbubble of diameter ~50 pc and expansion age ~0.3 Myr without establishing causality.
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Sub-kpc scale gas density histograms of the nearby barred spiral galaxy M83: Multi-component molecular gas structure reflecting the galactic environment
Molecular gas in M83 consists of two log-normal density components, with the high-density component enhanced along spiral arms and more tightly linked to star formation than the low-density component.
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Star Formation at the Periphery of a Molecular Superbubble: The Case of G12.79+0.43
Observational study of G12.79+0.43 identifies YSOs and HII regions powered by B-type stars and associates the complex with the rim of a molecular superbubble of diameter ~50 pc and expansion age ~0.3 Myr without establishing causality.