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We explore the development of structures in molecular gas in the Milky Way byapplying the analysis of the brightness distribution function (BDF) and thebrightness distribution index (BDI) in the archival data from the BostonUniversity-Five College Radio Astronomy Observatory 13CO J=1-0 Galactic RingSurvey. The BDI measures the fractional contribution of spatially confinedbright molecular emission over faint emission extended over large areas. Thisrelative quantity is largely independent of the amount of molecular gas and ofany conventional, pre-conceived structures, such as cores, clumps, or giantmolecular clouds. The structured molecular gas traced by higher BDI is locatedcontinuously along the spiral arms in the Milky Way in the longitude-velocitydiagram. This clearly indicates that molecular gas changes its structure as itflows through the spiral arms. Although the high-BDI gas generally coincideswith H II regions, there is also some high-BDI gas with no/little signature ofongoing star formation. These results support a possible evolutionary sequencein which unstructured, diffuse gas transforms itself into a structured state onencountering the spiral arms, followed by star formation and an eventual returnto the unstructured state after the spiral arm passage.

Structured Molecular Gas Reveals Galactic Spiral Arms