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We use the distance probability density function (DPDF) formalism ofEllsworth-Bowers et al. (2013, 2015) to derive physical properties for thecollection of 1,710 Bolocam Galactic Plane Survey (BGPS) version 2 sources withwell-constrained distance estimates. To account for Malmquist bias, we estimatethat the present sample of BGPS sources is 90% complete above 400 $M_\odot$ and50% complete above 70 $M_\odot$. The mass distributions for the entire sampleand astrophysically motivated subsets are generally fitted well by a lognormalfunction, with approximately power-law distributions at high mass. Power-lawbehavior emerges more clearly when the sample population is narrowed inheliocentric distance (power-law index $\alpha = 2.0\pm0.1$ for sources nearerthan 6.5 kpc and $\alpha = 1.9\pm0.1$ for objects between 2 kpc and 10 kpc).The high-mass power-law indices are generally $1.85 \leq \alpha \leq 2.05$ forvarious subsamples of sources, intermediate between that of giant molecularclouds and the stellar initial mass function. The fit to the entire sampleyields a high-mass power-law $\hat{\alpha} = 1.94_{-0.10}^{+0.34}$. Physicalproperties of BGPS sources are consistent with large molecular cloud clumps orsmall molecular clouds, but the fractal nature of the dense interstellar mediummakes difficult the mapping of observational categories to the dominantphysical processes driving the observed structure. The face-on map of theGalactic disk's mass surface density based on BGPS dense molecular cloudstructures reveals the high-mass star-forming regions W43, W49, and W51 asprominent mass concentrations in the first quadrant. Furthermore, we present a0.25-kpc resolution map of the dense gas mass fraction across the Galactic diskthat peaks around 5%.

The Bolocam Galactic Plane Survey. XIII. Physical Properties and Mass Functions of Dense Molecular Cloud Structures