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R Aqr is a symbiotic binary system consisting of a Mira variable with apulsation period of 387 days and a hot companion which is presumably a whitedwarf with an accretion disk. This binary system is the source of a prominentbipolar gaseous outflow. We use high spatial resolution and sensitive imagesfrom the Hubble Space Telescope to identify and investigate the differentstructural components that form the complex morphology of the R Aqr jet .Methods. We present new high-resolution HST WFC3/UVIS narrow-band images of theR Aqr jet obtained in 2013/14 in the light of the [OIII] 5007, [OI] 6300, [NII]6583, and Ha emission lines. These images also allow us to produce detailedmaps of the jet flow in several line ratios such as [OIII]/[OI] and [NII]/[OI]which are sensitive to the outflow temperature and its hydrogen ionisationfraction. The new emission maps together with archival HST data are used toderive and analyse the proper motion of prominent emitting features which canbe traced over 20 years with the HST observations. The images reveal the finegas structure of the jet out to distances of a few ten arcseconds from thecentral region, as well as in the innermost region, within a few arcsecondsaround the stellar source. They reveal for the first time the straighthighly-collimated jet component which can be traced to up to 900 AU in the NEdirection. Images in [OIII], [OI], and [NII] clearly show a helical pattern inthe jet beams which may derive from the small-scale precession of the jet. Thehighly-collimated jet is accompanied by a wide opening angle outflow which isfilled by low excitation gas. The position angles of the jet structures as wellas their opening angles are calculated. Our measurements of the proper motionsof some prominent emission knots confirm the scenario of gas accelerationduring the propagation of the outflow.

The bipolar jet of the symbiotic star R Aquarii: A study of its morphology using the high-resolution HST WFC3/UVIS camera