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Consideration of both low- and high-resolution transmission spectroscopy iskey for obtaining a comprehensive picture of exoplanet atmospheres. In studiesof transmission spectra, the continuum information is well established withlow-resolution spectra, while the shapes of individual lines are bestconstrained with high-resolution observations. In this work, we aim to mergehigh- with low-resolution transmission spectroscopy. We present the analysis ofthree primary transits of WASP-69b in the VIS channel of the CARMENESinstrument and perform a combined low- and high-resolution analysis usingadditional data from HARPS-N, OSIRIS/GTC, and WFC3/HST already available in theliterature. During the first CARMENES observing night, we detected the planetNa D$_{2}$ and D$_{1}$ lines at $\sim 7\sigma$ and $\sim 3\sigma$ significancelevels, respectively. We measured a D$_{2}$/D$_{1}$ intensity ratio of2.5$\pm$0.7, which is in agreement with previous HARPS-N observations. Ourmodelling of WFC3 and OSIRIS data suggests strong Rayleigh scattering, solar tosuper-solar water abundance, and a highly muted Na feature in the atmosphere ofthis planet, in agreement with previous investigations of this target. We usethe continuum information retrieved from the low-resolution spectroscopy as aprior to break the degeneracy between the Na abundance, reference pressure, andthermosphere temperature for the high-resolution spectroscopic analysis. We fitthe Na D$_{1}$ and D$_{2}$ lines individually and find that the posteriordistributions of the model parameters agree with each other within 1$\sigma$.Our results suggest that local thermodynamic equilibrium processes can explainthe observed D$_{2}$/D$_{1}$ ratio because the presence of haze opacity mutesthe absorption features.

Probing the atmosphere of WASP-69 b with low- and high-resolution transmission spectroscopy