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 f(R,T-phi) theory of gravity for an isotropic and homogeneous universe, where the trace of the energy-momentum tensor T-phi is the function of the self-interacting scalar field phi. We have proposed an explicit solution to the derived model by utilizing a scale factor of the hybrid form a(t)=t(alpha)e(beta t), where alpha and beta 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 H(z) points in the range 0.07 <= z <= 2.36 and Pantheon Sample consisting of a total of 1048 SNe Ia in the range of 0.01 z<2:3. 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. 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 zl-0:78with the present value of the deceleration parameter q(0)- -0:565. 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