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Euclid: Constraints on f(R) cosmologies from the spectroscopic and photometric primary probes

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Jun 19, 2023
19 pages
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2022202320240215
Abstract: (arXiv)
Euclid\textit{Euclid} will provide a powerful compilation of data including spectroscopic redshifts, the angular clustering of galaxies, weak lensing cosmic shear, and the cross-correlation of these last two photometric observables. In this study we extend recently presented Euclid\textit{Euclid} forecasts into the Hu-Sawicki f(R)f(R) cosmological model, a popular extension of the Hilbert-Einstein action that introduces an universal modified gravity force in a scale-dependent way. Our aim is to estimate how well future Euclid\textit{Euclid} data will be able to constrain the extra parameter of the theory, fR0f_{R0}, for the range in which this parameter is still allowed by current observations. For the spectroscopic probe, we use a phenomenological approach for the scale dependence of the growth of perturbations in the terms related to baryon acoustic oscillations and redshift-space distortions. For the photometric observables, we use a fitting formula that captures the modifications in the non-linear matter power spectrum caused by the f(R)f(R) model. We show that, in an optimistic setting, and for a fiducial value of fR0=5×10−6f_{R0} = 5 \times 10^{-6}, Euclid\textit{Euclid} alone will be able to constrain the additional parameter log⁡fR0\log f_{R0} at the 3%3\% level, using spectroscopic galaxy clustering alone; at the 1.4%1.4\% level, using the combination of photometric probes on their own; and at the 1%1\% level, using the combination of spectroscopic and photometric observations. This last constraint corresponds to an error of the order of 6×10−76 \times 10^{-7} at the 1σ1\sigma level on the model parameter fR0=5×10−6f_{R0} = 5 \times 10^{-6}. We report also forecasted constraints for fR0=5×10−5f_{R0} = 5 \times 10^{-5} and fR0=5×10−7f_{R0} = 5 \times 10^{-7} and show that in the optimistic scenario, Euclid\textit{Euclid} will be able to distinguish these models from ΛCDM\Lambda\mathrm{CDM} at more than 3σ\sigma. (abridged)
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  • 10 Figures, 3 Tables, 1 Appendix