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Ultra-hot jupiters (UHJs) are giant planets on short orbital periods withhigh equilibrium temperature (T_eq) values. Their hot, extended atmospheres areperfect laboratories for transmission spectroscopy studies based onhigh-resolution spectrographs. In recent years, a variety of atoms andmolecules were found in their atmospheres, using different methods such ascross-correlation or transmission and emission spectroscopy. Here, we presentthe studies of six ultra-hot Jupiters: HAT-P-57b, KELT-7b, KELT-17b, KELT-21b,MASCARA-1b, and WASP-189b, based on high-resolution observations obtained withHARPS-N and HARPS spectrographs. By applying line and cross-correlationtransmission spectroscopy methods, we searched for the absorption features of abroad range of atomic and molecular species. We did not detect any absorptionfeatures in our sample of UHJs, with the exception of WASP-189b, for which wedetected FeI, FeII, and TiI using cross-correlation. The transmissionspectroscopy of single lines for WASP-189b revealed several absorption features(including Halpha, Hbeta and Ca H&K), but they remain tentative pending abetter modelling of the gravity darkening deformation of theRossiter-McLaughlin effect. The non-detections with regard to the rest of theplanets can be explained via a combination of stellar pulsations and theRossiter-McLaughlin effect, which mask possible planetary signals for most ofthe planets, and by the low signal-to-noise ratios (S/N) of the observationsfor KELT-21b. Here, we compare our results with the known population of planetsfor which atmospheric detections have been reported in the literature. We findthat the empirical frontier between hot and ultra-hot planets, based on thedetection of atomic and ionized species in their atmospheres, can beestablished as Teq = 2150 K.

High-resolution transmission spectroscopy study of ultra-hot Jupiters HAT-P-57b, KELT-17b, KELT-21b, KELT-7b, MASCARA-1b, and WASP-189b