  We present the analysis of archival XMM-Newton European Photon Imaging Camera
(EPIC) X-ray observations of the symbiotic star R Aquarii. We used the Extended
Source Analysis Software (ESAS) package to disclose diffuse soft X-ray emission
extending up to 2.2 arcmin ($\approx$0.27 pc) from this binary system. The
depth of these XMM-Newton EPIC observations reveal in unprecedented detail the
spatial distribution of this diffuse emission, with a bipolar morphology
spatially correlated with the optical nebula. The extended X-ray emission
shares the same dominant soft X-ray-emitting temperature as the clumps in the
jet-like feature resolved by Chandra in the vicinity of the binary system. The
harder component in the jet might suggest that the gas cools down, however, the
possible presence of non-thermal emission produced by the presence of a
magnetic field collimating the mass ejection can not be discarded. We propose
that the ongoing precessing jet creates bipolar cavities filled with
X-ray-emitting hot gas that feeds the more extended X-ray bubble as they get
disrupted. These EPIC observations demonstrate that the jet feedback mechanism
produced by an accreting disk around an evolved, low-mass star can blow hot
bubbles, similar to those produced by jets arising from the nuclei of active
galaxies.
