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Temperature inversion layers are predicted to be present in ultra-hot giantplanet atmospheres. Although such inversion layers have recently been observedin several ultra-hot Jupiters, the chemical species responsible for creatingthe inversion remain unidentified. Here, we present observations of the thermalemission spectrum of an ultra-hot Jupiter, WASP-189b, at high spectralresolution using the HARPS-N spectrograph. Using the cross-correlationtechnique, we detect a strong Fe I signal. The detected Fe I spectral lines arefound in emission, which is direct evidence of a temperature inversion in theplanetary atmosphere. We further performed a retrieval on the observed spectrumusing a forward model with an MCMC approach. When assuming a solar metallicity,the best-fit result returns a temperature of $4320_{-100}^{+120}$ K at the topof the inversion, which is significantly hotter than the planetary equilibriumtemperature (2641 K). The temperature at the bottom of the inversion isdetermined as $2200_{-800}^{+1000}$ K. Such a strong temperature inversion isprobably created by the absorption of atomic species like Fe I.

A temperature inversion with atomic iron in the ultra-hot dayside atmosphere of WASP-189b