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We present 12 new transit light curves and 16 new out-of-transit radialvelocity measurements for the XO-3 system. By modelling our newly collectedmeasurements together with archival photometric and Doppler velocimetric data,we confirmed the unusual configuration of the XO-3 system, which contains amassive planet ($M_P=11.92^{+0.59}_{-0.63} M_J$) on a relatively eccentric($e=0.2853^{+0.0027}_{-0.0026}$) and short-period ($3.19152 \pm 0.00145\,$day)orbit around a massive star ($M_*=1.219^{+0.090}_{-0.095} M_{\odot}$).Furthermore, we find no strong evidence for a temporal change of either $V\sini_{*}$ (and by extension, the stellar spin vector of XO-3), or the transitprofile (and thus orbital angular momentum vector of XO-3b). We conclude thatthe discrepancy in previous Rossiter-McLaughlin measurements ($70.0^{\circ} \pm15.0^{\circ}$ (Hebrard et al. 2008); $37.3^{\circ} \pm 3.7^{\circ}$ (Winn etal. 2009); $37.3^{\circ} \pm 3.0^{\circ}$ (Hirano et al. 2011)) may havestemmed from systematic noise sources.

Revisiting the Full Sets of Orbital Parameters for the XO-3 System: No evidence for Temporal Variation of the Spin-Orbit Angle