  In this study, we have explored a scalar field cosmological model in the
axially symmetric Bianchi type-I universe. In this study, our aim is to
constrain the scalar field dark energy model in an anisotropic background. For
this purpose, the explicit solution of the developed field equations for the
model is determined and analysed. Constraints on the cosmological model
parameters are established utilizing Markov Chain Monte Carlo (MCMC) analysis
and using the latest observational data sets of OHD, BAO, and Pantheon. For the
combined dataset (OHD, BAO, and Pantheon), the best-fit values of Hubble and
density parameters are estimated as $ H_{0} = 71.54\pm 0.28$,
$\Omega_{m0}=0.2622\pm0.0021$ $\Omega_{\phi0} = 0.7331\pm0.0046$, and
$\Omega_{\sigma 0} = 0.000162\pm0.000063$. The model shows a flipping nature
and redshift transition occurs at $z_{t} = 0.6964^{+0.0136}_{-0.0006}$, and the
present value of decelerated parameter is computed to be $q_{0} =
-0.6964\pm0.028$ for the combined dataset. We have explored characteristics
like the universe's age, particle horizon, deceleration parameter, and jerk
parameter. The dynamical properties such as energy density $\rho_{\phi}$,
scalar field pressure $p_{\phi}$, and equation of state parameter
$\omega_{\phi}$ are analyzed and presented. We have also described the behavior
of the scalar potential $V(\phi)$ and scalar fields. Furthermore, the authors
also described the behavior of energy conditions in scalar-tensor cosmology.
The scenario of the present accelerated expansion of the universe is described
by the contribution of the scalar field.
