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We study the morpho-kinematics of the circumbinary envelope of Mira Cetibetween $\sim$100 and $\sim$350 au from the stars using ALMA observations ofthe SiO ($\nu$=0, $J$=5-4) and CO ($\nu$=0, $J$=3-2) emissions with the aim ofpresenting an accurate and reliable picture of what cannot be ignored whenmodelling the dynamics at stake. A critical study of the uncertainties attachedto imaging is presented. The line emissions are shown to be composed of a fewseparated fragments. They are described in detail and plausible interpretationsof their genesis are discussed. Evidence for a focusing effect of the Mira Awind by Mira B over the past century is presented; it accounts for only a smallfraction of the overall observed emission but its accumulation over severalorbital periods may have produced an enhancement of CO emission in the orbitalplane of Mira B. We identify a South-western outflow and give arguments for theanti-correlation observed between CO and SiO emissions being the result of arecent mass ejection accompanied by a shock wave. We discuss the failure ofsimple scenarios that have been proposed earlier to explain some of theobserved features and comment on the apparent lack of continuity between thepresent observations and those obtained in the close environment of the stars.Evidence is obtained for the presence of large Doppler velocity components nearthe line of sight aiming to the star, possibly revealing the presence ofimportant turbulence at $\sim$5 to 10 au away from Mira A.

Revealing new features of the millimetre emission of the circumbinary envelope of Mira Ceti