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Theoretical studies predict the presence of thermal inversions in theatmosphere of highly irradiated gas giant planets. Recent observations haveidentified these inversion layers. However, the role of different chemicalspecies in their formation remains unclear. We search for the signature of thethermal inversion agents TiO and Fe in the dayside emission spectrum of theultra-hot Jupiter WASP-33b. The spectra were obtained with CARMENES andHARPS-N, covering different wavelength ranges. Telluric and stellar absorptionlines were removed with SYSREM. We cross-correlated the residual spectra withmodel spectra to retrieve the signals from the planetary atmosphere. We findevidence for TiO at a significance of 4.9$\mathrm{\sigma}$ with CARMENES. Thestrength of the TiO signal drops close to the secondary eclipse. No TiO signalis found with HARPS-N. An injection-recovery test suggests that the TiO signalis below the detection level at the wavelengths covered by HARPS-N. Theemission signature of Fe is detected with both instruments at significancelevels of 5.7$\mathrm{\sigma}$ and 4.5$\mathrm{\sigma}$, respectively. Bycombining all observations, we obtain a significance level of7.3$\mathrm{\sigma}$ for Fe. We find the TiO signal at $K_\mathrm{p}$ =$248.0_{-2.5}^{+2.0}$ km s$^{-1}$, which is in disagreement with the Fedetection at $K_\mathrm{p}$ = $225.0_{-3.5}^{+4.0}$ km s$^{-1}$. The$K_\mathrm{p}$ value for Fe is in agreement with prior investigations. Themodel spectra require different temperature profiles for TiO and Fe to matchthe observations. We observe a broader line profile for Fe than for TiO. Ourresults confirm the existence of a temperature inversion layer in the planetaryatmosphere. The observed $K_\mathrm{p}$ offset and different strengths ofbroadening in the line profiles suggest the existence of a TiO-depleted hotspot in the planetary atmosphere.

Detection of Fe and evidence for TiO in the dayside emission spectrum of WASP-33b