Evaluation of transit cosmological model in f(R,Tϕ) theory of gravity

In this paper, we have explored a transitioning cosmic model, depicting late-time accelerated expansion in the [Formula: see text] theory of gravity for an isotropic and homogeneous universe, where the trace of the energy–momentum tensor [Formula: see text] is the function of the self-interacting scalar field [Formula: see text]. We have proposed an explicit solution to the derived model by utilizing a scale factor of the hybrid form [Formula: see text], where [Formula: see text] and [Formula: see text] are constants. To estimate the best-fit values of model parameters, statistical analysis based on the Markov Chain Monte Carlo (MCMC) method has been employed on 57 [Formula: see text] points in the range [Formula: see text] and Pantheon Sample consisting of a total of 1048 SNe Ia in the range of [Formula: see text]. We have described the dynamical features of the model, like energy density, cosmic pressure, and the equation of state parameter, in the context of the scalar field [Formula: see text]. We have also described the potential and behavior of the scalar field for quintessence and phantom scenarios. For the joint dataset of OHD and Pantheon, the deceleration parameter depicts a transitioning universe with signature flipping at [Formula: see text] with the present value of the deceleration parameter [Formula: see text]. The violation of SEC for the derived model indicates cosmic expansion at a faster rate. We have used state-finders to diagnose the model. The findings for our theoretical model indicate that the derived model agrees with observed findings within a particular range of limitations.