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The number of magnetic stars detected among massive stars is small;nevertheless, the role played by the magnetic field in stellar evolution cannotbe disregarded. Links between line profile variability, enhancements/depletionsof surface chemical abundances, and magnetic fields have been identified forlow-mass B-stars, but for the O-type domain this is almost unexplored. Based onFORS2 and HARPS spectropolarimetric data, we present the first detection of amagnetic field in HD54879, a single slowly rotating O9.7 V star. Using twoindependent and different techniques we obtained the firm detection of asurface average longitudinal magnetic field with a maximum amplitude of about600 G, in modulus. A quantitative spectroscopic analysis of the star with thestellar atmosphere code FASTWIND results in an effective temperature and asurface gravity of 33000$\pm1000$ K and 4.0$\pm0.1$ dex. The abundances ofcarbon, nitrogen, oxygen, silicon, and magnesium are found to be slightly lowerthan solar, but compatible within the errors. We investigate line-profilevariability in HD54879 by complementing our spectra with spectroscopic datafrom other recent OB-star surveys. The photospheric lines remain constant inshape between 2009 and 2014, although H$\alpha$ shows a variable emission. TheH$\alpha$ emission is too strong for a standard O9.7 V and is probably linkedto the magnetic field and the presence of circumstellar material. Its normalchemical composition and the absence of photospheric line profile variationsmake HD54879 the most strongly magnetic, non-variable single O-star detected todate.

B fields in OB stars (BOB): Detection of a strong magnetic field in the O9.7 V star HD54879