Robust constraints on dark energy and gravity from galaxy clustering data

Abstract

Galaxy clustering data provide a powerful probe of dark energy. We examine how the constraints on the scaled expansion history of the universe, x_h(z)=H(z)s (with s denoting the sound horizon at the drag epoch), and the scaled angular diameter distance, x_d(z)=D_A(z)/s, depend on the methods used to analyze the galaxy clustering data. We find that using the observed galaxy power spectrum, P_g^{obs}(k), x_h(z) and x_d(z) are measured more accurately and are significantly less correlated with each other, compared to using only the information from the baryon acoustic oscillations (BAO) in P_g^{obs}(k). Using the {x_h(z), x_d(z)} from P_g^{obs}(k) gives a DETF dark energy FoM approximately a factor of two larger than using the {x_h(z), x_d(z)} from BAO only; this provides a robust conservative method to go beyond BAO only in extracting dark energy information from galaxy clustering data. We find that a Stage IV galaxy redshift survey, with 0.7<z<2 over 15,000 (deg)^2, can measure {x_h(z), x_d(z), f_g(z)G(z)\tilde{P}_0^{1/2}/s^4} with high precision (where f_g(z) and G(z) are the linear growth rate and factor of large scale structure respectively, and \tilde{P}_0 is the dimensionless normalization of P_g^{obs}(k)), when redshift-space distortion information is included. The measurement of f_g(z)G(z)\tilde{P}_0^{1/2}/s^4 provides a powerful test of gravity, and significantly boosts the dark energy FoM when general relativity is assumed.

8 pages, 3 figures. Version with minor revisions, accepted for publication in MNRAS

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