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This overview paper presents ATOMIUM, a Large Programme in Cycle 6 with theAtacama Large Millimeter-submillimeter Array (ALMA). The goal of ATOMIUM is tounderstand the dynamics and the gas phase and dust formation chemistry in thewinds of evolved asymptotic giant branch (AGB) and red supergiant (RSG) stars.A more general aim is to identify chemical processes applicable to otherastrophysical environments. 17 oxygen-rich AGB and RSG stars spanning a rangein (circum)stellar parameters and evolutionary phases were observed in ahomogeneous observing strategy allowing for an unambiguous comparison. Datawere obtained between 213.83 and 269.71 GHz at high (0.025-0.050 arcsec),medium (0.13-0.24 arcsec), and low (about 1 arcsec) angular resolution. Thesensitivity per 1.3 km/s channel was 1.5-5 mJy/beam. 13 molecules weredesignated as primary molecules in the survey: CO, SiO, AlO, AlOH, TiO, TiO2,HCN, SO, SO2, SiS, CS, H2O, and NaCl. The scientific motivation, survey design,sample properties, data reduction, and an overview of the data products aredescribed; and we highlight one scientific result - the wind kinematics of theATOMIUM sources. The ATOMIUM sources often have a slow wind acceleration, and afraction of the gas reaches a velocity which can be up to a factor of two timeslarger than previously reported terminal velocities assuming isotropicexpansion, and the wind kinematic profiles establish that the radial velocitydescribed by the momentum equation for a spherical wind structure cannotcapture the complexity of the velocity field. In 15 sources, some moleculartransitions other than 12CO v=0 J=2-1 reach a higher outflow velocity, with aspatial emission zone that is often greater than 30 stellar radii, but muchless than the extent of CO. Binary interaction with a (sub)stellar companionmight (partly) explain the non-monotonic behaviour of the projected velocityfield.

ATOMIUM: ALMA tracing the origins of molecules in dust forming oxygen rich M-type stars: Motivation, sample, calibration, and initial results