We study the $(w_0,w_a)$ parametrization of the dark energy (DE) equation of state, with and without the effective field theory of dark energy (EFTofDE) framework to describe the DE perturbations, parametrized here by the braiding parameter ${\alpha }_B$ and the running of the Planck mass ${\alpha }_M$. We combine the effective field theory of large-scale structure full-shape analysis of the power spectrum and bispectrum of BOSS data with the tomographic angular power spectra $C_{\ell }^{gg}$, $C_{\ell }^{\kappa g}$, $C_{\ell }^{Tg}$, and $C_{\ell }^{T\kappa }$, where $g$, $\kappa$, and $T$ stand for the DESI luminous red galaxy map, Planck Public Release 4 (PR4) lensing map and Planck PR4 temperature map, respectively. To analyze these angular power spectra, we go beyond the Limber approximation, allowing us to include large-scale data in $C_{\ell }^{gg}$. The combination of all these probes with Planck PR4, Dark Energy Spectroscopic Instrument (DESI) second data release of baryon acoustic oscillation (BAO), and DES Year 5 improves the constraint on the two-dimensional posterior distribution of $\{w_0,w_a\}$ by $\sim 50\%$ and increases the preference for evolving dark energy over $\mathrm{\Lambda }$ from $3.8\sigma$ to $4.6\sigma$. When we remove BAO and supernovae data, we obtain a hint for evolving dark energy at $2.3\sigma$. Regarding the EFTofDE parameters, we improve the constraints on ${\alpha }_B$ and ${\alpha }_M$ by $\sim 40\%$ and 50%, respectively, finding results compatible with general relativity at $\sim 2\sigma$. We show that these constraints do not depend on the choice of the BAO and supernovae likelihoods.

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• Dark energy
• Large scale structure of the Universe