Interacting dark energy with CPL admits exact solutions via incomplete gamma functions; Q proportional to dark energy density modestly improves AIC fit but BIC prefers LambdaCDM, showing phantom-to-quintessence transition and possible future transient acceleration.
A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s −1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
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Cosmological evolution of interacting dark energy with a CPL equation of state
Interacting dark energy with CPL admits exact solutions via incomplete gamma functions; Q proportional to dark energy density modestly improves AIC fit but BIC prefers LambdaCDM, showing phantom-to-quintessence transition and possible future transient acceleration.