The symbiotic star R Aqr is part of a small sample of binary AGB stars observed with the Atacama Large Millimeter/submillimeter Array ( ALMA ) .
The sample stars are : R Aqr , Mira , W Aql , and \pi ^ { 1 } Gru .
The sample covers a range in binary separation and wind properties , where R Aqr is the source with the smallest separation .
The R Aqr binary pair consists of an M-type AGB star and a white dwarf at a separation of 45 mas , equivalent to about 10 AU at 218 pc .
The aim of the ALMA study is to investigate the dependence of the wind shaping on the binary separation and to provide constraints for hydrodynamical binary interaction models .
R Aqr is particularly interesting as the source with the smallest separation and a complex circumstellar environment that is strongly affected by the interaction between the two stars and by the high-energy radiation resulting from this interaction and from the hot white dwarf companion .

The CO ( J = 3 \rightarrow 2 ) line emission has been observed with ALMA at \sim 0.5″spatial resolution .
The CO envelope around the binary pair is marginally resolved , showing what appears to be a rather complex distribution .
The outer radius of the CO emitting region is estimated from the data and found to be about a factor of 10 larger than previously thought .
This implies an average mass-loss rate during the past \sim 100 yr of \dot { M } \approx 2 \times 10 ^ { -7 } M _ { \odot } yr ^ { -1 } , a factor of 45 less than previous estimates .
The channel maps are presented and the molecular gas distribution is discussed and set into the context of what was previously known about the system from multiwavelength observations .
Additional molecular line emission detected within the bandwidth covered by the ALMA observations is also presented .

Because of the limited extent of the emission , firm conclusions about the dynamical evolution of the system will have to wait for higher spatial resolution observations .
However , the data presented here support the assumption that the mass-loss rate from the Mira star strongly varies and is focused on the orbital plane .