Model-independent determination of the cosmic expansion rate. I. Application to type-Ia supernovae

Abstract

Aims: In view of the substantial uncertainties regarding the possible dynamics of the dark energy, we aim at constraining the expansion rate of the universe without reference to a specific Friedmann model and its parameters. Methods: We show that cosmological observables integrating over the cosmic expansion rate can be converted into a Volterra integral equation which is known to have a unique solution in terms of a Neumann series. Expanding observables such as the luminosity distances to type-Ia supernovae into a series of orthonormal functions, the integral equation can be solved and the cosmic expansion rate recovered within the limits allowed by the accuracy of the data. Results: We demonstrate the performance of the method applying it to synthetic data sets of increasing complexity, and to the first-year SNLS data. In particular, we show that the method is capable of reproducing a hypothetical expansion function containing a sudden transition.

9 pages, 8 figures; accepted by A&A; subsection 3.6 added, new references and minor changes

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• Constraints on dark energy from baryon acoustic peak and galaxy cluster gas mass measurements
• Reconstruction of cosmological matter perturbations in Modified Gravity
• On the sensitivity of weak gravitational lensing to the cosmic expansion function