String theory naturally leads to the expectation that dark energy is not stable, and may be evolving as captured by the Swampland de Sitter conjectures. Moreover, motivated by the distance conjecture, a unification of dark sector has been proposed, where the smallness of dark energy leads to one extra dimension of micron size with dark matter being the Kaluza-Klein graviton excitations in this extra dimension. We consider the natural possibility that the radius of the dark dimension varies as the energy decreases, leading to the variation of the dark matter mass. This correlates the variation of the dark energy with the variation of the dark matter mass as they depend on the variations of a scalar field $\varphi$ controlling the radius of the extra dimension. A simple realization of this idea for small range of $\varphi$ is adequately captured by choosing a potential which is locally of the form $V=V_0\exp (-c\varphi )$ and dark matter mass $m_{\mathrm{DM}}=m_0\exp (-c^{\prime }\varphi )$ as was proposed in [1]. We find excellent agreement with recent experimental data from DESI DR2 combined with SN measurements (from DES, Union3 or Pantheon+) and reproduces the same significance as Chevallier–Polarski–Linder parametrization with the added benefit of providing a natural explanation for the apparent phantom behavior ($w<-1$) reported by DESI and DES based on a physical model. DESI and SN datasets independently favor nonzero values of $c^{\prime }$ and $c$, respectively, both lying within the expected $\mathcal{O}(1)$ range suggested by the Swampland criteria. Moreover, our best fit value $c^{\prime }\simeq 0.05\pm 0.01$ is remarkably consistent with the experimental upper bound of $c^{\prime }\lesssim 0.2$ demanded by the lack of detection of fifth force in the dark sector.

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• Dark energy
• Dark matter
• Particle astrophysics