The extended molecular envelope of the asymptotic giant branch star
  $\pi^{1}$ Gruis as seen by ALMA II. The spiral-outflow observed at
  high-angular resolution
  The AGB star $\pi^{1}$ Gruis has a known companion (at a separation of ~400
AU) which cannot explain the strong deviations from the spherical symmetry of
the CSE. Recently, hydrodynamic simulations of mass transfer in closer binary
systems have successfully reproduced the spiral-shaped CSEs found around a
handful of sources. There is growing evidence for an even closer, undetected
companion complicating the case of $\pi^{1}$ Gruis further. The improved
spatial resolution allows for the investigation of the complex circumstellar
morphology and the search for imprints on the CSE of the third component. We
have observed the 12CO J=3-2 line emission from $\pi^{1}$ Gruis using both the
compact and extended array of Atacama Large Millimeter/submillimeter Array
(ALMA). The interferometric data has furthermore been combined with data from
the ALMA total power (TP) array. The imaged brightness distribution has been
used to constrain a non-local, non-LTE 3D radiative transfer model of the CSE.
The high-angular resolution ALMA data have revealed the first example of a
source on the AGB where both a faster bipolar outflow and a spiral pattern
along the orbital plane can be seen in the gas envelope. The spiral can be
traced in the low- to intermediate velocity, from 13 to 25 km s$^{-1}$,
equatorial torus. The largest spiral-arm separation is $\approx$5".5 and
consistent with a companion with an orbital period of $\approx$330 yrs and a
separation of less than 70 AU. The kinematics of the bipolar outflow is
consistent with it being created during a mass-loss eruption where the
mass-loss rate from the system increased by at least a factor of 5 during 10-15
yrs. The spiral pattern is the result of an undetected companion. The bipolar
outflow is the result of a rather recent mass-loss eruption event.
