AB And    The third component is clearly seen in the LITE but has not been
AB And    detected during the CFHT AO observations.
GZ And    A multiple (trapezoidal) system, with colors and magnitudes indicating
GZ And    that all visual components may be physically associated. It does not
GZ And    have a Hipparcos parallax.
V410 Aur  The visual component, identical to that of the spectroscopic
V410 Aur  detection, shows RV variability, indicating that it is possibly SB1.
44 Boo    The closest contact binary. The 206yr period of the visual orbit is
44 Boo    reflected in the LITE but cannot be determined solely from this
44 Boo    effect, so it is considered as not detected by the LITE.
CK Boo    The third component, detected independently by the LITE and CFHT AO
CK Boo    observations, is very probably the same body. Krzesinski et al.
CK Boo    (1991Ap&SS.184...37K) detected a small but definite ultraviolet
CK Boo    excess, so it is possible that the third component is a white dwarf.
AO Cam    A very preliminary LITE solution has been given by Qian et al.
AO Cam    (2005AJ....129.1686Q). Spectral signatures of a companion detected by
AO Cam    D'Angelo et al. (2006AJ....132..650D).
AH Cnc    A member of M67. A physical link within WDS 08517+1151 is uncertain.
VW Cep    The third component has been detected by several techniques.
VW Cep    The visual and LITE orbits still show an additional wobble.
EM Cep    A member of the open cluster NGC 7160. The projected separation of the
EM Cep    components ({rho}/{pi}) is almost 50,000AU, which is much larger than
EM Cep    for all remaining wide systems of this sample. Hence, it is not
EM Cep    considered as a genuine triple system.
EE Cet    While the southern component of WDS 02499+0856 is a contact binary,
EE Cet    unpublished DDO spectroscopic observations show that the northern
EE Cet    component is a double-lined (SB2) binary and hence that it is a
EE Cet    quadruple system.
BV Dra    and BW Dra. A well-known quadruple system composed of two contact
BV Dra    binaries. BW Dra shows additional astrometric complications.
V345 Gem  The contact binary is the fainter component of a visual double.
AK Her    The fainter visual component cannot be identified with the component
AK Her    indicated by the LITE, so the system is possibly a quadruple one.
SW Lac    Lines of the third component were detected spectrally by  Hendry &
SW Lac    Mochnacki (1998ApJ...504..978H); this is probably the same component
SW Lac    as seen in the CFHT AO data. The LITE indicates two companions, but
SW Lac    the visual companion does not seem to correspond to any of the
SW Lac    possible bodies suggested by the LITE solution.
XY Leo    A member of a quadruple system detected by Barden
XY Leo    (1987ApJ...317..333B). The companion binary is a BY Dra-type
XY Leo    binary system. The LITE orbit is exceptionally well defined.
AM Leo    A member of a relatively wide visual binary. A marginally acceptable
AM Leo    LITE solution for the contact binary was given by Qian et al.
AM Leo    (2005AJ....129.1686Q).
VW LMi    A quadruple system according to DDO spectral observations (to be
VW LMi    published). The companion binary has an orbital period of 7.93 days,
VW LMi    while both binaries appear to revolve about the common center of
VW LMi    gravity in 356 days.
V752 Mon  The contact binary is the fainter component of the visual double. The
V752 Mon  brighter primary is a rapidly rotating A-type star obliterating
V752 Mon  signatures of the contact pair in the spectra.
V502 Oph  Lines of a third component were detected by Hendry & Mochnacki
V502 Oph  (1998ApJ...504..978H).
V2388 Oph A visual binary with an orbital period of only 8.9yr.
BB Peg    D'Angelo et al. (2006AJ....132..650D) detected M dwarf signatures in
BB Peg    the spectrum. A LITE analysis indicates a compatible body with a
BB Peg    minimum mass of 0.18 M_{Sun}.
AW UMa    A proper-motion pair with BD +30 2164. The projected separation of the
AW UMa    components is d={rho}/{pi}=4400AU. The magnitudes and colors indicate
AW UMa    a physical link. The LITE and systemic velocities show additional
AW UMa    perturbations that may be related to another, closer companion.
TV UMi    A quadruple system according to the DDO spectral observations (to be
TV UMi    published). The second binary is a detached system with a highly
TV UMi    eccentric orbit and a period of a few weeks.
AG Vir    The faint companion has been detected in the DDO spectra
AG Vir    (to be published).
AH Vir    The visual companion cannot be identified with the component
AH Vir    indicated by the LITE.
HT Vir    The components of WDS 13461+0507 revolving in 274yr orbit are both
HT Vir    binaries. While component B is a contact binary, component A is a
HT Vir    single-lined binary (SB1) with P=32.45 days (Lu et al.
HT Vir    2001AJ....122..402L).