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Atmospheric studies at high spectral resolution have shown the presence ofmolecules, neutral and ionised metals, and hydrogen in the transmissionspectrum of ultra-hot Jupiters, and have started to probe the dynamics of theiratmospheres. We analyse the transmission spectrum of MASCARA-1b, one of thedensest ultra-hot Jupiters orbiting a bright (V=8.3) star. We focus on the CaIIH&K, NaI, LiI, H$\alpha$, and KI D1 spectral lines and on the cross-correlatedFeI, FeII, CaI, YI, VI, VII, CaH, and TiO lines. For those species that are notpresent in the stellar spectrum, no detections are reported, but we measureupper limits with an excellent precision ($\sim10$ ppm for particular species).For those species that are present in the stellar spectrum and whoseplanet-occulted spectral lines induce spurious features in the planetarytransmission spectrum, an accurate modelling of the Rossiter-McLaughlin effect(RM) and centre-to-limb variations (CLV) is necessary to recover possibleatmospheric signals. In the case of MASCARA-1b, this is difficult due to theoverlap between the radial velocities of the stellar surface regions occultedby MASCARA-1b and the orbital track along which the planet atmospheric signalis expected to be found. To try to disentangle a possible planetary signal, wecompare our results with models of the RM and CLV effects, and estimate theuncertainties of our models depending on the different system parameters.Unfortunately, more precise measurements of the spin-orbit angle are necessaryto better constrain the planet-occulted track and correct for the transiteffects in the transmission spectrum with enough precision to be able to detector discard possible planetary absorptions. Finally, we discuss the possibilitythat non-detections are related to the low absorption expected for a highsurface gravity planet such as MASCARA-1b.

Transmission spectroscopy of MASCARA-1b with ESPRESSO: Challenges of overlapping orbital and Doppler tracks