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Single dish observations of AGB star L$_2$ Pup have revealed exceptionallylow mass loss rate and expansion velocity, challenging interpretations in termsof standard wind models. Recent VLT and ALMA observations have drawn a detailedpicture of the circumstellar envelope within $\sim$20 au from the centre of thestar: a nearly edge-on rotating disc of gas and dust, probably hosting aplanetary companion near the star. However, these observations provide nodirect information on the wind escaping the gravity of the star. The presentarticle uses ALMA observations of the $^{12,13}$CO(3-2), $^{29}$SiO(8-7),$^{12}$CO(2-1) and $^{28}$SiO(5-4) line emissions to shed new light on thisissue. It shows the apparent normality of L$_2$ Pup in terms of the formationof the nascent wind, with important line broadening within 4 au from the centreof the star, but no evidence for a wind flowing along the disc axis. At largerdistances, up to some 200 au from the centre of the star, the windmorpho-kinematics is dominated by a disc, or equatorial enhancement, expandingisotropically and radially with a velocity not exceeding some 5 km s$^{-1}$ ,inclined in the north-west/south-east direction with respect to the plane ofthe sky. In addition, outflows of lower density are observed on both sides ofthe disc, covering large solid angles about the disc axis, contributing abouthalf the flux of the disc. Such morphology is at strong variance with theexpectation of a pair of back-to-back outflows collimated by the centralgas-and-dust disc.

Morpho-kinematics of the wind of AGB star L$_2$ Pup