  Employing the Korea-IBS-Daegu-SKKU (KIDS) density functional for the hadron
phase and the MIT bag model with vector (vBag) model for the quark phase, we
obtain hadron-quark phase transition in neutron stars considering Maxwell
construction. The structural properties of the resultant hybrid stars are
computed for three different values of bag constant ($B$) in the range
$B^{1/4}=$(145$-$160 MeV). We study the effects of symmetry energy ($J$) on the
hybrid star properties with the different KIDS model and found that $J$ has
important influence not only on the transition properties like the transition
mass, transition radius and jump in density due to phase transition, but also
on the stability of the hybrid stars. The vector repulsion of the quark phase
via the parameter $G_V$ has profound influence in obtaining reasonable hybrid
star configurations, consistent with the recent astrophysical constraints on
the structural properties of compact stars. Within the aforesaid range of $B$,
the value of $G_V$ is constrained to be 0.3 $\lesssim G_V \lesssim$ 0.4 in
order to obtain reasonable hybrid star configurations.
