  Discovering wide companions of stellar systems allows us to constrain the
dynamical environment and age of the latter. We studied four probable wide
companions of four different stellar systems. The central stars are V4046 Sgr,
HIP 74865, HIP 65426, and HIP 73145, and their probable wide companions are
2MASS J18152222-3249329, 2MASS J15174874-3028484, 2MASS J13242119-5129503, and
2MASS J14571503-3543505 respectively. V4046 Sgr is a member of $\beta$-Pictoris
Moving Group while the rest of the stellar systems are acknowledged as members
of the Scorpius-Centaurus association. The selected stellar systems are
particularly interesting because all of them are already known to possess a
low-mass companion and/or a spatially resolved disk. Identifying wider
companions of these stars can improve their eligibility as benchmarks for
understanding the formation channels of various triple systems, and can help us
to determine the orbits of their possibly undiscovered inner, wider companions
in case of higher multiplicity. We find that 2MASS J15174874-3028484 (0.11
$M_{\odot}$, 7.4$\pm$0.5 Myr), an already recognized pre-main sequence (PMS)
member of Scorpius-Centaurus association, is a highly probable wide companion
of HIP 74865. 2MASS J13242119-5129503 (0.04 $M_{\odot}$, 16$\pm$2.2 Myr) is
ruled out as a plausible wide companion of HIP 65426, but confirmed to be a new
sub-stellar member of the Scorpius-Centaurus association. 2MASS
J14571503-3543505 (0.02 $M_{\odot}$, 17.75$\pm$4.15 Myr) is a probable
sub-stellar member of the same association, but we cannot confirm whether or
not it is gravitationally bound to HIP 73145. 2MASS J18152222-3249329 (0.3
$M_{\odot}$, older than 150 Myr) is determined to be a mildly active main
sequence (MS) star, much older than members of $\beta$-Pictoris Moving Group,
and unbound to V4046 Sgr despite their similar kinematic features.
