Dynamical dark energy in models with an evolution close to <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mi mathvariant="normal">Λ</mml:mi> <mml:mi>CDM</mml:mi> </mml:math>

In this communication, we address whether or not there is an equivalence between the kinematical and dynamical descriptions of the spatially flat $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ model. We address this by investigating whether an almost $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ expansion history [$j(z)\ensuremath{\approx}1$] corresponds to an almost $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ model [${w}_{\mathrm{DE}}(z)\ensuremath{\approx}\ensuremath{-}1$] by considering two particular explicit examples. At least for the cases considered, this turns out not to be the case. Instead, what we find is that an almost $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ cosmic evolution rather corresponds to an almost unified dark-fluid model. Considering that one never gets the exact condition $j(z)=1$ from any cosmographic datasets, this raises further questions on whether the $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ model is the best candidate for the standard model of the evolution of the Universe.