We find soft X-ray emission lines from the X-ray binary Swift J1858.6-0814 in data from XMM-Newton-RGS: N VII, O VII and O VIII, as well as notable residuals short of a detection at Ne IX and other higher ionisation transitions. These could be associated with the disc atmosphere, as in accretion disc corona sources, or with a wind, as has been detected in Swift J1858.6-0814 in emission lines at optical wavelengths. Indeed, the N VII line is redshifted, consistent with being the emitting component of a P-Cygni profile. We find that the emitting plasma has an ionisation parameter log (ξ) = 1.35 ± 0.2 and a density n > 1.5 × 1011 cm-3. From this, we infer that the emitting plasma must be within 1013 cm of the ionising source, ∼5 × 107rg for a 1.4M⊙ neutron star, and from the line width that it is at least 104rg away (2 × 109(M/1.4M⊙) cm). We compare this with known classes of emission line regions in other X-ray binaries and active galactic nuclei.