Model-independent determination of the cosmic expansion rate: I. application to type-Ia supernovae
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...
Guardado en:
| Autores principales: | , |
|---|---|
| Formato: | Article (Journal) Chapter/Article |
| Lenguaje: | inglés |
| Publicado: |
April 27, 2017
|
| In: |
Arxiv
|
| Acceso en línea: | Verlag, Volltext: http://arxiv.org/abs/0711.0370
|
| Notas de Autor: | Claudia Mignone, and Matthias Bartelmann |
| Sumario: | 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. |
|---|---|
| Notas: | Gesehen am 25.09.2017 |
| Descripción Física: | Online Resource |