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We have used the ratio of column densities (CDR) derived independently fromthe 850-$\mu$m continuum JCMT Plane Survey (JPS) and the $^{13}$CO/C$^{18}$O$(J=3-2)$ Heterodyne Inner Milky Way Plane Survey (CHIMPS) to produce maps ofthe dense-gas mass fraction (DGMF) in two slices of the Galactic Plane centredat $\ell$=30$^{\circ}$ and $\ell$=40$^{\circ}$. The observed DGMF is a metricfor the instantaneous clump-formation efficiency (CFE) in the molecular gas. Wesplit the two fields into velocity components corresponding to the spiral armsthat cross them, and a two-dimensional power-spectrum analysis of the spiralarm DGMF maps reveals a break in slope at the approximate size scale ofmolecular clouds. We interpret this as the characteristic scale of theamplitude of variations in the CFE and a constraint on the dominant mechanismregulating the CFE and, hence, the star-formation efficiency in CO-tracedclouds.

Characteristic scale of star formation. I. Clump formation efficiency on local scales