be compared to the +264.6km/s [@Smith71], $+262\pm16$km/s [@Danziger76], and +259km/s [@Feast64] for N127, a nearby HII region.

Since most of the H$\alpha$ emission arises in the recombination zone of the cloud shocks, we can estimate a lower limit for the cloud shock velocities, $v_s$, from the most extreme differences in the measured radial velocity of the cloud from the mean Heliocentric radial velocity of the photoionised halo of N132D. These are +173km/s for cloud P04, and -143km/s for cloud P19. Thus we have $v_s \gtrsim 160$km/s, in good agreement with the estimate based on the FWHM of the H$\alpha$ line profiles.

Measuring Emission Line Fluxes
------------------------------

For each extracted spectrum, the spectra were first reduced to rest wavelength based on their measured radial velocities listed in Table \[table1\], and then emission-line fluxes [ in units of erg/cm$^2$/s]{}, their uncertainties, the emission line FWHMs [ (in Å)]{} and the continuum levels were measured using the interactive routines in [Graf]{} [^4]and in [Lines]{} [^5]. The measured line fluxes [ relative to H$\beta$]{} and their uncertainties [ along with the absolute H$\beta$ fluxes in units of erg/cm$^2$/s]{}, are given for each of the clouds in Tables \[tableA1\] – \[tableA4\] in the Appendix.

Emission 