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In the quest to understand high-mass star formation, it is necessary tounderstand that from which the high-mass stars will form -- the dense moleculargas clouds and clumps. The Herschel infrared GALactic plane survey (Hi-GAL) isa comprehensive survey of thermal dust emission that can be used tocharacterize the properties and Galactic distribution of molecular gas. We haveanalyzed the survey maps within the Galactic longitude range $10^\circ < \ell <56^\circ$ and have transformed these 2D maps into a 3D dense gas map of theGalactic plane using distance probability density functions. This rangecorresponds to the extent of the Galactic Ring Survey (GRS), which provided themajority of our line-of-sight velocities, and thus kinematic distances. In thissection of Hi-GAL, we identify 19,886 clumps, out of which 10,124 have, atminimum, a kinematic distance, and 5,405 have their distances well constrainedthrough Bayesian techniques. Of those with well-constrained distances, clumpmasses tend to decrease with Galactocentric radius, whereas clump radii areindependent of Galactocentric radius.

Northern Galactic Molecular Cloud Clumps in Hi-GAL: Dense Gas Map and Environmental Trends