Papers › KiDS+GAMA: Constraints on Horndeski gravity from combined large-scale structure probes
KiDS+GAMA: Constraints on Horndeski gravity from combined large-scale structure probes
Alessio Spurio Mancini, Fabian Köhlinger, Benjamin Joachimi, Valeria Pettorino, Björn Malte Schäfer, Robert Reischke, Edo van Uitert, Samuel Brieden, Maria Archidiacono, Julien Lesgourgues
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We present constraints on Horndeski gravity from a combined analysis of cosmic shear, galaxy-galaxy lensing and galaxy clustering from 450 deg² of the Kilo-Degree Survey (KiDS) and the Galaxy And Mass Assembly (GAMA) survey. The Horndeski class of dark energy/modified gravity models includes the majority of universally coupled extensions to ΛCDM with one scalar field in addition to the metric. We study the functions of time that fully describe the evolution of linear perturbations in Horndeski gravity. Our results are compatible throughout with a ΛCDM model. By imposing gravitational wave constraints, we fix the tensor speed excess to zero and consider a subset of models including e.g. quintessence and f(R) theories. Assuming proportionality of the Horndeski functions α_B and α_M (kinetic braiding and the Planck mass run rate, respectively) to the dark energy density fraction Ω_(DE)(a) = 1 - Ωₘ(a), we find for the proportionality coefficients α̂_B = 0.20_(-0.33)^(+0.20) and α̂_M = 0.25_(-0.29)^(+0.19). Our value of S₈ ≡σ₈ √(Ωₘ/0.3) is in better agreement with the Planck estimate when measured in the enlarged Horndeski parameter space than in a pure ΛCDM scenario. In our joint three-probe analysis we report a downward shift of the S₈ best fit value from the Planck measurement of ΔS₈ = 0.016_(-0.046)^(+0.048) in Horndeski gravity, compared to ΔS₈ = 0.059_(-0.039)^(+0.040) in ΛCDM. Our constraints are robust to the modelling uncertainty of the non-linear matter power spectrum in Horndeski gravity. Our likelihood code for multi-probe analysis in both ΛCDM and Horndeski gravity is publicly available at http://github.com/alessiospuriomancini/KiDSHorndeski .
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