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We present a dynamical study of the eclipsing intermediate polar XY Ari basedon time-resolved near-infrared spectroscopy obtained with the EMIR spectrographon the 10.4-m Gran Telescopio Canarias. Using main sequence template spectrataken with the same instrument setup as the target spectra, we measure a radialvelocity amplitude of the late K-type donor star $K_2=256 \pm 2$ km s$^{-1}$.We also obtain the rotational broadening of its photospheric lines$v_\mathrm{rot} \sin i = 141 \pm 3$ km s$^{-1}$. From these and the eclipsegeometry, we derive a donor-to-white-dwarf mass ratio $q = M_2/M_1 = 0.62 \pm0.02$, an orbital inclination $i = 80.8^{\circ} \pm 0.5^{\circ}$ and dynamicalmasses $M_{1} = 1.21 \pm 0.04 \, \mathrm{M}_{\odot}$ and $M_2 = 0.75 \pm 0.04\, \mathrm{M}_{\odot}$ ($1 \sigma$). This result places the white dwarf in XYAri as one of the three most massive known in a cataclysmic variable.Comparison with white dwarf mass estimates from X-ray spectral studies couldindicate the necessity of an improvement of the X-ray models and/or analysistechniques, as a number of X-ray white dwarf masses are in disagreement withthe dynamical mass value.

Dynamical mass of the white dwarf in XY Ari: a test for intermediate polar X-ray spectral models