  Aims. Various studies indicate that interacting binary stars of Algol type
evolve non-conservatively. However, direct detections of systemic mass loss in
Algols have been scarce so far. We study the systemic mass loss in Algols by
looking for the presence of infrared excesses originating from the thermal
emission of dust grains, which is linked to the presence of a stellar wind.
  Methods. In contrast to previous studies, we make use of the fact that
stellar and interstellar material is piled up at the edge of the astrosphere
where the stellar wind interacts with the interstellar medium. We analyse WISE
W3 $12\,\mu$m and WISE W4 $22\,\mu$m data of Algol-type binary Be and B[e]
stars and the properties of their bow shocks. From the stand-off distance of
the bow shock we are able to determine the mass-loss rate of the binary system.
  Results. Although the velocities of the stars with respect to the
interstellar medium are quite low, we find bow shocks present in two systems,
namely $\pi$ Aqr, and $\varphi$ Per; a third system, CX Dra, shows a more
irregular circumstellar environment morphology which might somehow be related
to systemic mass loss. The properties of the two bow shocks point to mass-loss
rates and wind velocities typical of single B stars, which do not support an
enhanced systemic mass loss.
