Theoretical uncertainties on non-linear scales are among the main obstacles to exploit the sensitivity of forthcoming galaxy and hydrogen surveys like Euclid or the Square Kilometre Array (SKA). Here, we devise a new method to model the theoretical error that goes beyond the usual cut-o ff on small scales. The advantage of this more efficient implementation of the non-linear uncertainties is tested through a Markov-Chain-Monte-Carlo (MCMC) forecast of the sensitivity of Euclid and SKA to the parameters of the standard Lambda CDM model, including massive neutrinos with total mass M-nu, and to 3 extended scenarios, including 1) additional relativistic degrees of freedom (Lambda CDM + M-nu + N-eff), 2) a deviation from the cosmological constant (Lambda CDM + M-nu + w(0)), and 3) a time-varying dark energy equation of state parameter (CDM + M-nu + (w(0);w(a))). We compare the sensitivity of 14 di ff erent combinations of cosmological probes and experimental con fi gurations. For Euclid combined with Planck, assuming a plain cosmological constant, our method gives robust predictions for a high sensitivity to the primordial spectral index ns (sigma(n(s)) = 0.00085), the Hubble constant H-0 (sigma(H-0) = 0.141 km/s/Mpc), the total neutrino mass M-nu(sigma(M-nu) = 0.020 eV). Assuming dynamical dark energy we get sigma(M-nu) = 0.030 eV for the mass and (sigma(w(0)); sigma(w(a))) = (0.0214; 0.071) for the equation of state parameters. The predicted sensitivity to M-nu is mostly stable against the extensions of the cosmological model considered here. Interestingly, a significant improvement of the constraints on the extended model parameters is also obtained when combining Euclid with a low redshift HI intensity mapping survey by SKA1, demonstrating the importance of the synergy of Euclid and SKA.

Cosmology in the era of Euclid and the Square Kilometre Array / T. Sprenger, M. Archidiacono, T. Brinckmann, S. Clesse, J. Lesgourgues. - In: JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS. - ISSN 1475-7516. - 2(2019 Feb 22). [10.1088/1475-7516/2019/02/047]

Cosmology in the era of Euclid and the Square Kilometre Array

M. Archidiacono
Secondo
;
2019

Abstract

Theoretical uncertainties on non-linear scales are among the main obstacles to exploit the sensitivity of forthcoming galaxy and hydrogen surveys like Euclid or the Square Kilometre Array (SKA). Here, we devise a new method to model the theoretical error that goes beyond the usual cut-o ff on small scales. The advantage of this more efficient implementation of the non-linear uncertainties is tested through a Markov-Chain-Monte-Carlo (MCMC) forecast of the sensitivity of Euclid and SKA to the parameters of the standard Lambda CDM model, including massive neutrinos with total mass M-nu, and to 3 extended scenarios, including 1) additional relativistic degrees of freedom (Lambda CDM + M-nu + N-eff), 2) a deviation from the cosmological constant (Lambda CDM + M-nu + w(0)), and 3) a time-varying dark energy equation of state parameter (CDM + M-nu + (w(0);w(a))). We compare the sensitivity of 14 di ff erent combinations of cosmological probes and experimental con fi gurations. For Euclid combined with Planck, assuming a plain cosmological constant, our method gives robust predictions for a high sensitivity to the primordial spectral index ns (sigma(n(s)) = 0.00085), the Hubble constant H-0 (sigma(H-0) = 0.141 km/s/Mpc), the total neutrino mass M-nu(sigma(M-nu) = 0.020 eV). Assuming dynamical dark energy we get sigma(M-nu) = 0.030 eV for the mass and (sigma(w(0)); sigma(w(a))) = (0.0214; 0.071) for the equation of state parameters. The predicted sensitivity to M-nu is mostly stable against the extensions of the cosmological model considered here. Interestingly, a significant improvement of the constraints on the extended model parameters is also obtained when combining Euclid with a low redshift HI intensity mapping survey by SKA1, demonstrating the importance of the synergy of Euclid and SKA.
cosmological parameters from LSS; neutrino masses from cosmology
Settore FIS/05 - Astronomia e Astrofisica
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/2434/704698
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