### Abstract

The cosmological principle, promoting the view that the Universe is homogeneous and isotropic, is embodied within the mathematical structure of the Robertson-Walker (RW) metric. The equations derived from an application of this metric to the Einstein Field Equations describe the expansion of the Universe in terms of comoving coordinates, from which physical distances may be derived using a time-dependent expansion factor. These coordinates, however, do not explicitly reveal the properties of the cosmic space-time manifested in Birkhoff's theorem and its corollary. In this paper, we compare two forms of the metric - written in (the traditional) comoving coordinates, and a set of observer-dependent coordinates - first for the well-known de Sitter universe containing only dark energy, and then for a newly derived form of the RW metric, for a universe with dark energy and matter. We show that Rindler's event horizon - evident in the comoving system - coincides with what one might call the 'curvature horizon' appearing in the observer-dependent frame. The advantage of this dual prescription of the cosmic space-time is that with the latest Wilkinson Microwave Anisotropy Probe results, we now have a much better determination of the Universe's mass-energy content, which permits us to calculate this curvature with unprecedented accuracy. We use it here to demonstrate that our observations have probed the limit beyond which the cosmic curvature prevents any signal from having ever reached us. In the case of de Sitter, where the mass-energy density is a constant, this limit is fixed for all time. For a universe with a changing density, this horizon expands until de Sitter is reached asymptotically, and then it too ceases to change.

Original language | English (US) |
---|---|

Pages (from-to) | 1917-1921 |

Number of pages | 5 |

Journal | Monthly Notices of the Royal Astronomical Society |

Volume | 382 |

Issue number | 4 |

DOIs | |

State | Published - Dec 2007 |

### Fingerprint

### Keywords

- Cosmic microwave background
- Cosmological parameters
- Cosmology: observations
- Cosmology: theory
- Distance scale

### ASJC Scopus subject areas

- Space and Planetary Science

### Cite this

*Monthly Notices of the Royal Astronomical Society*,

*382*(4), 1917-1921. https://doi.org/10.1111/j.1365-2966.2007.12499.x

**The cosmic horizon.** / Melia, Fulvio.

Research output: Contribution to journal › Article

*Monthly Notices of the Royal Astronomical Society*, vol. 382, no. 4, pp. 1917-1921. https://doi.org/10.1111/j.1365-2966.2007.12499.x

}

TY - JOUR

T1 - The cosmic horizon

AU - Melia, Fulvio

PY - 2007/12

Y1 - 2007/12

N2 - The cosmological principle, promoting the view that the Universe is homogeneous and isotropic, is embodied within the mathematical structure of the Robertson-Walker (RW) metric. The equations derived from an application of this metric to the Einstein Field Equations describe the expansion of the Universe in terms of comoving coordinates, from which physical distances may be derived using a time-dependent expansion factor. These coordinates, however, do not explicitly reveal the properties of the cosmic space-time manifested in Birkhoff's theorem and its corollary. In this paper, we compare two forms of the metric - written in (the traditional) comoving coordinates, and a set of observer-dependent coordinates - first for the well-known de Sitter universe containing only dark energy, and then for a newly derived form of the RW metric, for a universe with dark energy and matter. We show that Rindler's event horizon - evident in the comoving system - coincides with what one might call the 'curvature horizon' appearing in the observer-dependent frame. The advantage of this dual prescription of the cosmic space-time is that with the latest Wilkinson Microwave Anisotropy Probe results, we now have a much better determination of the Universe's mass-energy content, which permits us to calculate this curvature with unprecedented accuracy. We use it here to demonstrate that our observations have probed the limit beyond which the cosmic curvature prevents any signal from having ever reached us. In the case of de Sitter, where the mass-energy density is a constant, this limit is fixed for all time. For a universe with a changing density, this horizon expands until de Sitter is reached asymptotically, and then it too ceases to change.

AB - The cosmological principle, promoting the view that the Universe is homogeneous and isotropic, is embodied within the mathematical structure of the Robertson-Walker (RW) metric. The equations derived from an application of this metric to the Einstein Field Equations describe the expansion of the Universe in terms of comoving coordinates, from which physical distances may be derived using a time-dependent expansion factor. These coordinates, however, do not explicitly reveal the properties of the cosmic space-time manifested in Birkhoff's theorem and its corollary. In this paper, we compare two forms of the metric - written in (the traditional) comoving coordinates, and a set of observer-dependent coordinates - first for the well-known de Sitter universe containing only dark energy, and then for a newly derived form of the RW metric, for a universe with dark energy and matter. We show that Rindler's event horizon - evident in the comoving system - coincides with what one might call the 'curvature horizon' appearing in the observer-dependent frame. The advantage of this dual prescription of the cosmic space-time is that with the latest Wilkinson Microwave Anisotropy Probe results, we now have a much better determination of the Universe's mass-energy content, which permits us to calculate this curvature with unprecedented accuracy. We use it here to demonstrate that our observations have probed the limit beyond which the cosmic curvature prevents any signal from having ever reached us. In the case of de Sitter, where the mass-energy density is a constant, this limit is fixed for all time. For a universe with a changing density, this horizon expands until de Sitter is reached asymptotically, and then it too ceases to change.

KW - Cosmic microwave background

KW - Cosmological parameters

KW - Cosmology: observations

KW - Cosmology: theory

KW - Distance scale

UR - http://www.scopus.com/inward/record.url?scp=37249015469&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=37249015469&partnerID=8YFLogxK

U2 - 10.1111/j.1365-2966.2007.12499.x

DO - 10.1111/j.1365-2966.2007.12499.x

M3 - Article

AN - SCOPUS:37249015469

VL - 382

SP - 1917

EP - 1921

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 4

ER -