The TPOD has a typo: "ESO astronomers have a different viewpoint" should be "ESA astronomers have a different viewpoint" (ESO is the European Southern Observatory; ESA is the European Space Agency: "The Hubble Space Telescope is a joint ESA/NASA project ...").
The ESA PR that this TPOD references (dated to 2003) has a paragraph which reads:
The paper which this relies upon, where the team report their observational results (etc), seems to be "The high-velocity outflow in the proto-planetary nebula Hen 3-1475", by A. Riera, P. Garcia-Lario, A. Manchado, M. Bobrowsky, and R. Estalella (link is to arXiv preprint abstract); the abstract is:A group of international astronomers led by Angels Riera from Universitat Politecnica de Catalunya, Barcelona, Spain, have combined observations from Hubble's Wide Field and Planetary Camera 2, the Space Telescope Imaging Spectrograph and ground-based telescopes. Their work suggests that the nebula's S-shape and hypervelocity outflow is created by a central source that ejects streams of gas in opposite directions and precesses once every 1500 years. It is like an enormous, slowly rotating garden sprinkler.
This paper has already been cited by 18 others, among those are several reporting observations of Hen 3-1475 in other parts of the electromagnetic spectrum. With so much high quality, quantitative, observational data now available, anyone wanting to test EU theory-based quantitative models of this class of astronomical object should be off to a flying start.Riera et al. wrote:The proto-planetary nebula Hen 3-1475 shows a remarkable highly collimated optical jet with an S-shaped string of three pairs of knots and extremely high velocities. We present here a detailed analysis of the overall morphology, kinematic structure and the excitation conditions of these knots based on deep ground-based high dispersion spectroscopy complemented with high spatial resolution spectroscopy obtained with STIS onboard HST, and WFPC2 [N II] images. The spectra obtained show double-peaked, extremely wide emission line profiles, and a decrease of the radial velocities with distance to the source in a step-like fashion. We find that the emission line ratios observed in the intermediate knots are consistent with a spectrum arising from the recombination region of a shock wave with shock velocities ranging from 100 to 150 km/s. We propose that the ejection velocity is varying as a function of time with a quasi-periodic variability (with timescale of the order of 100 years) and the direction of ejection is also varying with a precession period of the order of 1500 years.