  I point to an interesting similarity in the morphology and some
non-dimensional quantities between pairs of X-ray-deficient bubbles in clusters
of galaxies and pairs of optical-deficient bubbles in planetary nebulae (PNs).
This similarity leads me to postulate a similar formation mechanism. This
postulate is used to strengthen models for PN shaping by jets (or collimated
fast winds: CFW). The presence of dense material in the equatorial plane
observed in the two classes of bubbles constrains the jets and CFW activity in
PNs to occur while the AGB star still blows its dense wind, or very shortly
after. I argue that only a stellar companion can account for such jets and CFW.
