  Outflows in active galaxies (AGNs) are common, although their launching
mechanism, location, and physical impact on the host galaxy remain
controversial. We conducted a multiwavelength six-month campaign to observe the
nearby Seyfert galaxy NGC 7469 with several observatories in order to better
understand and quantify the outflow in this AGN. We report on the
time-integrated line-resolved X-ray spectrum of NGC 7469 obtained with the
Reflection Grating Spectrometer (RGS) on board XMM-Newton. We use the RGS
spectrum to discern the many AGN outflow components. A global fit is applied to
obtain their physical parameters. We find that the AGN wind can be well
described by three narrow velocity components at -650, -950, and -2050 km/s.
The RGS clearly resolves the -20 50 km/s component in C5+ Ly$\alpha$, while the
-650 km/s and -950 km/s velocities are blended. Similar velocities are resolved
in the UV. The H-equivalent column densities of these components are,
respectively, NH = 7x10^20, 2.2x10^21, and 10^20 cm^-2, for a total of 3x10^21
cm^-2. The -650 km/s component shows a broad ionisation distribution. We
identify a photo-ionised emission component blue-shifted by -450 km/s which we
ascribe to the same outflow that produces the absorption lines. The elemental
abundance ratios of C, N, Ne, S, and Fe to O in the outflow tend to be between
1 - 2 times solar. Preliminary estimates of the absorber distance from the AGN
center suggest it is at least a few pc away from the center, but more advanced
methods need to be applied in order to obtain better constraints. The complex
X-ray spectrum of NGC 7469 demonstrates the richness of high energy phenomena
taking place in AGN cores. The subtle spectroscopic differences between the
various components require deep, high-resolution observations, such as the
present RGS spectrum, if one is to resolve them and perform quantitative plasma
diagnostics.
