  We have used data from the Outer Galaxy High-Resolution Survey (OGHReS) to
refine the velocities, distances, and physical properties of a large sample of
3584 clumps detected in far infrared/submillimetre emission in the HiGAL survey
located in the $\ell = 250^\circ-280^\circ$ region of the Galactic plane. Using
$^{12}$CO and $^{13}$CO spectra, we have determined reliable velocities to 3412
clumps (95% of the sample). In comparison to the velocities from the HiGAL
catalogue, we find good agreement for 80% of the sample (within 5 km/s). Using
the higher resolution and sensitivity of OGHReS has allowed us to correct the
velocity for 632 clumps and provide velocities for 687 clumps for which no
velocity had been previously allocated. The velocities are used with a rotation
curve to refine the distances to the clumps and to calculate the clumps'
properties using a distance-dependent gas-to-dust ratio. We have determined
reliable physical parameters for 3200 outer Galaxy dense clumps (~90% of the
HiGAL sources in the region). We find a trend of decreasing luminosity-to-mass
ratio with increasing Galactocentric distance, suggesting the star formation
efficiency is lower in the outer Galaxy or that it is resulting in more lower
mass stars than in the inner Galaxy. We also find a similar surface density for
protostellar clumps located in the inner and outer Galaxy, revealing that the
surface density requirements for star formation are the same across the
Galactic disc.
