  The White Dwarf Binary Pathways Survey aims at increasing the number of known
detached A, F, G and K main sequence stars in close orbits with white dwarf
companions (WD+AFGK binaries) to refine our understanding about compact binary
evolution and the nature of Supernova Ia progenitors. These close WD+AFGK
binary stars are expected to form through common envelope evolution, in which
tidal forces tend to circularize the orbit. However, some of the identified
WD+AFGK binary candidates show eccentric orbits, indicating that these systems
are either formed through a different mechanism or perhaps they are not close
WD+AFGK binaries. We observed one of these eccentric WD+AFGK binaries with
SPHERE and find that the system TYC 7218-934-1 is in fact a triple system where
the WD is a distant companion. The inner binary likely consists of the G-type
star plus an unseen low mass companion in an eccentric orbit. Based on this
finding, we estimate the fraction of triple systems that could contaminate the
WD+AFGK sample. We find that less than 15 per cent of our targets with orbital
periods shorter than 100 days might be hierarchical triples.
