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Omega Centauri ($\omega$ Cen) is the most massive globular cluster of theMilky Way and has been the focus of many studies that reveal the complexity ofits stellar populations and kinematics. However, most previous studies haveused photometric and spectroscopic datasets with limited spatial or magnitudecoverage, while we aim to investigate it having full spatial coverage out toits half-light radius and stars ranging from the main sequence to the tip ofthe red giant branch. This is the first paper in a new survey of $\omega$ Centhat combines uniform imaging and spectroscopic data out to its half-lightradius to study its stellar populations, kinematics, and formation history. Inthis paper, we present an unprecedented MUSE spectroscopic dataset combining 87new MUSE pointings with previous observations collected from guaranteed timeobservations. We extract spectra of more than 300,000 stars reaching more thantwo magnitudes below the main sequence turn-off. We use these spectra to derivemetallicity and line-of-sight velocity measurements and determine robustuncertainties on these quantities using repeat measurements. Applying qualitycuts we achieve signal-to-noise ratios of 16.47/73.51 and mean metallicityerrors of 0.174/0.031 dex for the main sequence stars (18 mag $\rm <mag_{F625W}<$22 mag) and red giant branch stars (16 mag $<\rm mag_{F625W}<$10mag), respectively. We correct the metallicities for atomic diffusion andidentify foreground stars. This massive spectroscopic dataset will enablefuture studies that will transform our understanding of $\omega$ Cen, allowingus to investigate the stellar populations, ages, and kinematics in greatdetail.

oMEGACat I: MUSE spectroscopy of 300,000 stars within the half-light radius of $\omega$ Centauri