Quintessence phase of the late-time Universe in $f(Q,T)$ gravity

In this paper, we have studied the late-time accelerating expansion of the Universe using the matter-geometry coupled $f(Q,T)$ gravity model, where $Q$ is the non-metricity scalar and $T$ represents the trace of the energy-momentum tensor. We constrain the best-fit values of cosmological parameters ${\mathrm{\Omega }}_{m0},H_0,{\alpha }_{0}and{\beta }_0$ through the Monte Carlo Markov Chain (MCMC) simulation {using 31 Hubble parameter data points from cosmic chronometers (CC) and 26 data points from baryon acoustic oscillations (BAO), making a total of 57 datasets (labeled $\mathtt{\text{CC+BAO}}$), as well as SNIa distance moduli measurements from the Pantheon+ sample, which consists of 1701 light curves of 1550 distinct supernovae (labeled $\mathtt{\text{Pantheon}}\mathtt{\text{+SHOES}}$), and their combination (labeled $\mathtt{\text{CC+BAO+Pantheon}}\mathtt{\text{+SHOES)}}$}. {We compare our constrained Hubble constant $H_0$ value with different late-time and early-time cosmological measurements.} Deceleration {parameter} $q(z)$, effective equation of state parameters $w_{eff}(z)$, Hubble parameter $H(z)$, and distance modulus $\mu (z)$ are numerical results of dynamical quantities that show that the $f(Q,T)$ gravity model is compatible with a transition towards a quintessence-like phase in the late-time. In conformity with $\mathrm{\Lambda }$CDM, we moreover take into account the geometrical interpretations by considering the state-finder parameters $r-s$ and $r-q$, which are crucial parameters for additional analysis. Additionally, the statistical analysis has been carried out for further investigation.