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Far-infrared Herschel/PACS images at 70 and 160 micron of a sample of 78Galactic evolved stars are used to study the (dust) emission structures,originating from stellar wind-ISM interaction. In addition, two-fluidhydrodynamical simulations of the coupled gas and dust in wind-ISM interactionsare used to compare with the observations.  Four distinct classes of wind-ISM interaction (i.e. "fermata", "eyes","irregular", and "rings") are identified and basic parameters affecting themorphology are discussed. We detect bow shocks for ~40% of the sample anddetached rings for ~20%. De-projected stand-off distances (R_0) -- defined asthe distance between the central star and the nearest point of the interactionregion -- of the detected bow shocks ("fermata" and "eyes") are derived fromthe PACS images and compared to previous results, model predictions and thesimulations. All observed bow shocks have stand-off distances smaller than 1pc. Observed and theoretical stand-off distances are used together toindependently derive the local ISM density.  Both theoretical (analytical) models and hydrodynamical simulations givestand-off distances for adopted stellar properties that are in good agreementwith the measured de-projected stand-off distance of wind-ISM bow shocks. Thepossible detection of a bow shock -- for the distance limited sample -- appearsto be governed by its physical size as set roughly by the stand-off distance.In particular the star's peculiar space velocity and the density of the ISMappear decisive in detecting emission from bow shocks or detached rings.Tentatively, the "eyes" class objects are associated to (visual) binaries,while the "rings" generally appear not to occur for M-type stars, only for C orS-type objects that have experienced a thermal pulse.

A far-infrared survey of bow shocks and detached shells around AGB stars and red supergiants