  Aims. We aim to investigate and characterise the photoionised X-ray emission
line regions within NGC 7469. Methods. We apply the photoionisation model,
PION, within the spectral fitting code SPEX to analyse the 640 ks RGS spectrum
of NGC 7469 gathered during an XMM-Newton observing campaign in 2015. Results.
We find the emission line region in NGC 7469 to be multiphased, consisting of
two narrow components with ionisation parameters of $\log \xi = 0.4$ and 1.6. A
third, broad emission component, with a broadening velocity of $v_b \sim 1400$
km s\textsuperscript{-1} and an outflow velocity of $v_{out} \sim -4500$ km
s\textsuperscript{-1}, is required to fit the residuals in the O VII triplet,
at around 22 \AA. Assuming a volume filling factor of 0.1, the lower distance
limits of the narrow emission line region components are estimated for the
first time at 2.6 and 2.5 pc from the central black hole, whereas the broad
component has an estimated lower bound distance between 0.004 to 0.03 pc,
depending on the assumed plasma parameters. The collisionally ionised plasma
from the star burst region in NGC 7469 has a plasma temperature of 0.32 keV and
outflow velocity of $-280$ km s\textsuperscript{-1}, consistent with previous
results in this campaign. In addition, we model the photoionised plasma of the
warm absorber (WA) in NGC 7469, and find that it consists of three photoionised
phases, with different values of $\xi$, $N_H$ and $v_{out}$. The upper bound
distances of these WA components are 1.9, 0.3 and 0.6 pc, respectively,
consistent with archival results. Conclusions. The environment of NGC 7469 is a
complex mix of plasma winds absorbing and emitting X-rays. We find the picture
painted by our results can be attributed to line emitting plasma located at
distances ranging from near the black hole to the torus and beyond the ionised
outflows.
