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tokens: GR 290 in the remainder of this paper. The standard deviations are of similar value to our estimated measurement uncertainty of ±30 km s −1 . Since we do not detect variability in our two spectra that is larger than the uncertainty discussed above, we combined the July and August spectra, shifted the average by +179 km s −1 , and remeasured the lines. We list in Table 3 the RV of the emission in Col. 7, the equivalent width in Col. 8, the RV of the absorption component in the case of P Cyg profiles in Col. 9, and the intersection of the P Cyg absorption with the continuum level in Col. 10. The measurements for P Cyg profiles were performed with two-Gaussian fits 6 . We note that the contribution of nebular emission affects the FWHM. For example, in the case of H α , we measure FWHM = 6.6 Å if the line is fit with a single Gaussian while FWHM = 10.2 Å if the line is treated as a blend of a broad stellar line and a narrow superposed nebular emission. Despite this large difference in FWHM, the RV in both cases is nearly the same. The average V edge = −400 ± 144 km s −1 is similar to the value of v ∞ listed in Polcaro et al. (2016) for recent spectra. However, the He I lines have V edge ≃ 620 km s −1 , implying wind speeds that are faster than ever before observed. The Balmer-H lines also show the signs of a relatively fast outflow, as can be seen from the growing asymmetry in the blue wing of the higher excitation lines of this series. This is illustrated in Fig. 4 where H α and H β were scaled in intensity so as to align the red wings with that of H γ . The other lines plotted are H ∊ and H I 3835 Å. This asymmetry results from the same process that leads to P Cyg absorptions in He I but because of the large optical depth of the H-lines a fully developed absorption component is not visible. Fig. 4. Line profiles of the Balmer-H sequence plotted on a velocity scale corrected for the adopted −179 km s −1 systemic velocity. The lines of H α and H β are scaled by factors of 0.17 and 0.48, respectively, so as to align the red wings with that of H γ . The continuous lines show H γ , H ∊ , and H I 3835 Å. The progressive red-shift at shorter wavelengths appears to be a consequence of the increasing strength of the blue-shifted absorption which, in the helium lines, takes on the form of P Cyg absorption. This effect is explained by the fact that the optical depth of the wind is highest for H α and H β and decreases for lines that have smaller transition probabilities. 3.2. Stellar wind models We used the CMFGEN atmospheric modelling code ( Hillier Miller 1998 ) in order to estimate the current stellar parameters of GR 290. This code solves the radiative transfer equation for objects with spherically symmetric extended outflows using either the Sobolev approximation or the full comoving-frame solution of the radiative transfer equation. CMFGEN incorporates line blanketing, the effect of Auger ionization and clumping, which is parametrized by the volume