Quasilinear observables in dark energy cosmologies
What are the fundamental limitations of reconstructing the properties of dark energy, given cosmological observations in the quasilinear regime in a range of redshifts, to be as precise as required? The aim of this paper is to address this question by constructing model-independent observables, whil...
Saved in:
| Main Authors: | , , |
|---|---|
| Format: | Article (Journal) |
| Language: | English |
| Published: |
13 June 2017
|
| In: |
Physical review
Year: 2017, Volume: 95, Issue: 12, Pages: 123516 |
| ISSN: | 2470-0029 |
| DOI: | 10.1103/PhysRevD.95.123516 |
| Online Access: | Verlag, Volltext: http://dx.doi.org/10.1103/PhysRevD.95.123516 Verlag, Volltext: https://link.aps.org/doi/10.1103/PhysRevD.95.123516 
|
| Author Notes: | Cornelius Rampf, Eleonora Villa, and Luca Amendola |
| Summary: | What are the fundamental limitations of reconstructing the properties of dark energy, given cosmological observations in the quasilinear regime in a range of redshifts, to be as precise as required? The aim of this paper is to address this question by constructing model-independent observables, while completely ignoring practical problems of real-world observations. Non-Gaussianities already present in the initial conditions are not directly accessible from observations because of a perfect degeneracy with the non-Gaussianities arising from the (weakly) nonlinear matter evolution in generalized dark energy models. By imposing a specific set of evolution equations that should cover a range of dark energy cosmologies, we find, however, a constraint equation for the linear structure growth rate f1 expressed in terms of model-independent observables. Entire classes of dark energy models which do not satisfy this constraint equation could be ruled out, and for models satisfying it, we could reconstruct e.g. the nonlocal bias parameters b1 and b2. |
|---|---|
| Item Description: | Gesehen am 15.09.2017 |
| Physical Description: | Online Resource |
| ISSN: | 2470-0029 |
| DOI: | 10.1103/PhysRevD.95.123516 |