Left: the best-matching H₂O template, scaled such that subtracting it would exactly cancel the signal from the planet at ﹩{V}_{\mathrm{sys}}=-33﹩ km s⁻¹ and ﹩{K}_{{\rm{P}}}=133﹩ km s⁻¹. The template is displayed as a flux ratio, where the planet model was divided by a blackbody spectrum with the same ﹩{T}_{\mathrm{eff}}﹩ as the host star and then had its baseline continuum subtracted and was convolved to the CRIRES resolution of R = 100,000. The deepest lines correspond to a relative contrast ratio between the star and planet of ﹩1.0\times {10}^{-3}﹩ for the unconvolved model, and reduced to ﹩0.9\times {10}^{-3}﹩ for the convolved model. Right: a simple schematic displaying the temperature–pressure profile of the best-matching template, whose properties are listed in the upper-right corner.