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High-resolution optical spectra of the high-mass X-ray binary <ASTROBJ>4U 1907+09</ASTROBJ> covering the wavelength range 4680-10 400 Å indicate that the X-ray pulsar's massive companion is an O8/O9 supergiant with a dense stellar wind. The interstellar atomic lines of Na I and K I of this strongly reddened source ({E}(B-V) = 3.45 mag) are used to set a lower limit to its distance: d ≈ 5 kpc, excluding the possibility that the massive companion is a Be star. We re-evaluate the system parameters; the new spectral classification of <ASTROBJ>4U 1907+09</ASTROBJ>'s O supergiant companion is discussed in the context of its similarity in X-ray and orbital properties to <ASTROBJ>Wray 15-977</ASTROBJ>/<ASTROBJ>GX 301-2</ASTROBJ>. The Halpha line shows variability similar to what is observed in other wind-fed systems. A remarkable feature is the strong He ii 4686 Å emission line, which possibly originates in the accretion flow towards the X-ray pulsar

VLT/UVES spectroscopy of the O supergiant companion to 4U 1907+09(7)