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Characterising the atmospheres of hot Jupiters is important in understandingthe formation and migration of these exotic planets. However, there are stillmany open questions about the chemical and physical properties of theseatmospheres. Here, we confirm the detection of water vapour in thermal emissionfrom the non-transiting hot Jupiter {\tau} Bootis Ab with the high resolutionNIR CARMENES spectrograph. Combining over 17 h of observations (560 spectra)and using a Bayesian cross-correlation to log-likelihood approach, we measure asystemic velocity of $V_{sys} = -11.51^{+0.59}_{-0.60}$ km/s and a radialvelocity semi-amplitude of $K_{P} = 106.21^{+1.76}_{-1.71}$ km/s for theplanet, which results in an absolute mass of $M_{P} = 6.24^{+0.17}_{-0.18}M_{J}$ and an orbital inclination of $41.6^{+1.0}_{-0.9}$ degrees. Ourretrieved $V_{sys}$ shows a significant shift (+5 km/s) from the literaturevalue, which could be caused by an inaccurate time of periastron. Within theexplored model grid, we measure a preference for solar water abundance (VMR =$10^{-3}$) and no evidence for additional minor species in the atmosphere.Given the extensive orbital coverage of the data, we searched for a phasedependency in the water signal but found no strong evidence of variation withorbital phase. This detection is at odds with recent observations fromSPIRou/CFHT and their tight upper limit on water abundance. We recommendfurther observations of the atmosphere {\tau} Bootis Ab to try and resolvethese discrepancies.

Water observed in the atmosphere of {\tau} Bootis Ab with CARMENES/CAHA