  The properties of the neutron stars are calculated for the hadronic matter
within the density-dependent relativistic mean-field model (DD-RMF). The phase
transition to the quark matter is studied and the hybrid star matter properties
are systematically calculated using the Vector-Enhanced Bag model (vBag). The
maximum mass of neutron star with DD-LZ1 and DD-RMF parameter sets is found to
be around 2.55$M_{\odot}$ for pure hadronic phase and around 2$M_{\odot}$ for
hadron-quark mixed phase using both Gibbs and Maxwell construction. The tidal
deformability for the hybrid EoS at 1.4$M_{\odot}$, $\Lambda_{1.4}$, remains
unchanged from the pure hadronic EoS with Maxwell construction, but decreases
with the increasing neutron star mass for Gibbs construction. While the pure
hadron matter EoS satisfies the mass constraint from recently observed GW190814
data, implying a stiff neutron star EoS, the hadron-quark phase transition
satisfies the constraints from the recent observations GW170817. Therefore, we
cannot exclude the possibility of the secondary object in GW190814 as a neutron
star with a phase transition to the quark matter that satisfies the
2$M_{\odot}$ maximum mass limit.
