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Aims: We survey the transmission spectrum of WASP-121 b for line-absorptionby metals and molecules at high spectral resolution, and elaborate on existinginterpretations of the optical transmission spectrum observed with HST/STIS andWFC3. Methods: We use the cross-correlation technique and direct differentialspectroscopy to search for sodium and other neutral and ionised atoms, TiO, VOand SH in high-resolution transit spectra obtained with the HARPS spectrograph.We inject models assuming chemical and hydrostatic equilibrium with varyingtemperature and composition to enable model comparison, and employ twobootstrap methods to test the robustness of our detections. Results: We detectneutral Mg, Na, Ca, Cr, Fe, Ni and V, which we predict exists in equilibriumwith a significant quantity of VO, supporting earlier observations by HST/WFC3.Non-detections of Ti and TiO support the hypothesis that Ti is depleted via acold-trap mechanism as has been proposed in the literature. Atomic line depthsare under-predicted by hydrostatic models by a factor of 1.5 to 8, confirmingrecent findings that the atmosphere is extended. We predict the existence ofsignificant concentrations of gas-phase TiO$_2$, VO$_2$ and TiS, which could beimportant absorbers at optical and NIR wavelengths in hot Jupiter atmospheres,but for which accurate line-list data is currently not available. We find noevidence for absorption by SH, and find that inflated atomic lines canplausibly explain the slope of the transmission spectrum observed in the NUVwith HST/STIS. The Na D lines are significantly broadened and show a differencein their respective depths of 15 scale heights, which is not expected fromisothermal hydrostatic theory.

astronomy and astrophysics

Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS)  IV. A spectral inventory of atoms and molecules in the high-resolution  transmission spectrum of WASP-121 b