Updated observational constraints on ϕCDM dynamical dark energy cosmological models

We present updated observational constraints on the spatially flat Formula: see textCDM cosmological model, in which dark energy is described by a minimally coupled scalar field Formula: see text with an inverse power-law potential energy density Formula: see text. Using a combination of Planck 2018 cosmic microwave background (CMB) temperature, polarization (P18), and lensing power spectra (lensing), along with a comprehensive compilation of non-CMB data including baryon acoustic oscillation, type Ia supernova, Hubble parameter and growth rate measurements, we analyze parameter constraints of the Formula: see textCDM and Formula: see textCDM+Formula: see text models where Formula: see text is the CMB lensing consistency parameter. We find that the scalar field parameter Formula: see text, which governs dark energy dynamics, is more tightly constrained by non-CMB data than by CMB data alone. From P18+lensing+non-CMB data, we obtain Formula: see text in the Formula: see textCDM model and Formula: see text in the Formula: see textCDM+Formula: see text model, mildly favoring evolving dark energy over a cosmological constant by Formula: see text and Formula: see text. The estimated Hubble constant is Formula: see text km sFormula: see text MpcFormula: see text for P18+lensing+non-CMB data in the Formula: see textCDM model, consistent with median statistics and some local determinations, but in tension with other local determinations. The constraints for matter density and clustering amplitude (Formula: see text, Formula: see text) of the flat Formula: see textCDM model statistically agree with Formula: see textCDM model values. Allowing the CMB lensing consistency parameter Formula: see text to vary reduces tensions between CMB and non-CMB data, although we find Formula: see text, Formula: see text higher than unity, consistent with the excess smoothing seen in Planck data. Model comparison using AIC and DIC shows that the Formula: see textCDM model provides a fit comparable to Formula: see textCDM, with the Formula: see textCDM+Formula: see text extension slightly preferred in some cases. Overall, our results indicate that while the Formula: see textCDM model remains an excellent fit, current data leave open the possibility of mildly evolving quintessence-like dynamical dark energy, without a phantom-divide crossing.