  It is unclear how very close binary stars form, given that during the
pre-main-sequence phase the component stars would have been inside each other.
One hypothesis is that they formed further apart, but were brought in closer
after formation by gravitational interaction with a third member of the system.
If so, all close binaries should be members of triple (or higher-order)
systems. As a test of this prediction, we present a search for the signature of
third components in archival spectra of close binaries. In our sample of 75
objects, 23 show evidence for the presence of a third component, down to a
detection limit of tertiary flux contributions of about 0.8% at 5200 \AA\
(considering only contact and semi-detached binaries, we find 20 out of 66). In
a homogeneous subset of 58 contact binaries, we are fairly confident that the
15 tertiaries we have detected are all tertiaries present with mass ratios
$0.28\lesssim M_3/M_{12}\lesssim0.75$ and implied outer periods
$P\lesssim10^6{\rm d}$. We find that if the frequency of tertiaries was the
same as that of binary companions to solar-type stars, we would have expected
to detect about 12 tertiaries. In contrast, if all contact binaries were in
triple systems, one would expect about 20. Thus, our results are not
conclusive, but sufficiently suggestive to warrant further studies.
