  Using ALMA observations of $^{12}$CO(2-1), $^{28}$SiO(5-4) and
$^{32}$SO$_2$(16$_{6,10}$-17$_{5,13}$) emissions of the circumstellar envelope
of AGB star EP Aqr, we describe the morpho-kinematics governing the nascent
wind. Main results are: 1) Two narrow polar structures, referred to as jets,
launched from less than 25 au away from the star, build up between $\sim$ 20 au
and $\sim$ 100 au to a velocity of $\sim$ 20 \kms. They fade away at larger
distances and are barely visible in CO data. 2) SO$_2$, SiO and CO emissions
explore radial ranges reaching respectively $\sim$30 au, 250 au and 1000 au
from the star, preventing the jets to be detected in SO$_2$ data. 3) Close to
the star photosphere, rotation (undetected in SiO and CO data) and isotropic
radial expansion combine with probable turbulence to produce a broad SO$_2$
line profile ($\sim$ 7.5 \kms\ FWHM). 4) A same axis serves as axis of rotation
close to the star, as jet axis and as axi-symmetry axis at large distances. 5)
A radial wind builds up at distances up to $\sim$ 300 au from the star, with
larger velocity near polar than equatorial latitudes. 6) A sharp depletion of
SiO and CO emissions, starting near the star, rapidly broadens to cover the
whole blue-western quadrant, introducing important asymmetry in the CO and
particularly SiO observations. 7) The $^{12}$C/$^{13}$C abundance ratio is
measured as 9$\pm$2. 8) Plausible interpretations are discussed, in particular
assuming the presence of a companion.
