  We study the kinematics of emission lines that arise from many physical
processes in NGC 6153 based upon deep, spatially-resolved, high resolution
spectra acquired with the UVES spectrograph at the ESO VLT. Our most basic
finding is that the plasma in NGC 6153 is complex, especially its temperature
structure. The kinematics of most emission lines defines a classic expansion
law, with the outer part expanding fastest (normal nebular plasma). However,
the permitted lines of \ion{O}{1}, \ion{C}{2}, \ion{N}{2}, \ion{O}{2}, and
\ion{Ne}{2} present a constant expansion velocity that defines a second
kinematic component (additional plasma component). The physical conditions
imply two plasma components, with the additional plasma component having lower
temperature and higher density. The [\ion{O}{2}] density and the [\ion{N}{2}]
temperature are anomalous, but may be understood considering the contribution
of recombination to these forbidden lines. The two plasma components have very
different temperatures. The normal nebular plasma appears to be have
temperature fluctuations in part of its volume (main shell), but only small
fluctuations elsewhere. The additional plasma component contains about half of
the mass of the N$^{2+}$ and O$^{2+}$ ions, but only $3-5$\% of the mass of
H$^+$ ions, so the two plasma components have very different chemical
abundances. We estimate abundances of $12+\log(\mathrm O^{2+}/\mathrm H^+)\sim
9.2$\,dex and $\mathrm{He}/\mathrm H\sim 0.13$. Although they are all
complications, multiple plasma components, temperature fluctuations, and the
contributions of multiple physical processes to a given emission line are all
part of the reality in NGC 6153, and should generally be taken into account.
