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Ultra-hot Jupiters are perfect targets for transmission spectroscopy.However, their atmospheres feature strong spatial variations in temperature,chemistry, dynamics, cloud coverage, and scale height. This makes transitobservations at high spectral resolution challenging to interpret. In thiswork, we model the cross-correlation signal of five chemical species (Fe, CO,H$_\text{2}$O, OH, and TiO) on WASP-76b, a benchmark ultra-hot Jupiter. Wecompute phase-dependent high-resolution transmission spectra of 3D SPARC/MITgcmmodels. The spectra are obtained with gCMCRT, a 3D Monte-Carloradiative-transfer code. We find that, on top of atmospheric dynamics, thephase-dependent Doppler shift of the absorption lines in the planetary restframe is shaped by the combined effect of planetary rotation and the unique 3Dspatial distribution of chemical species. For species probing the dayside(e.g., refractories or molecules like CO and OH), the two effects act intandem, leading to increasing blueshifts with orbital phase. For species thatare depleted on the dayside (e.g., H$_\text{2}$O and TiO), the two effects actin an opposite manner, and could lead to increasing redshifts during thetransit. This behaviour yields species-dependent offsets from a planet'sexpected $K_\text{p}$ value that can be much larger than planetary wind speeds.The offsets are usually negative for refractory species. We provide ananalytical formula to estimate the size of a planet's $K_\text{p}$ offsets,which can serve as a prior for atmospheric retrievals. We conclude thatobserving the phase-resolved absorption signal of multiple species is key toconstraining the 3D thermochemical structure and dynamics of ultra-hotJupiters.

Modelling the effect of 3D temperature and chemistry on the  cross-correlation signal of transiting ultra-hot Jupiters: A study of 5  chemical species on WASP-76b