A Bayesian model selection analysis of WMAP3
| dc.creator | Parkinson, David | |
| dc.creator | Mukherjee, Pia | |
| dc.creator | Liddle, Andrew R | |
| dc.date | 2006-05-01 | |
| dc.date | 2006-06-19 | |
| dc.date.accessioned | 2026-07-07T11:42:31Z | |
| dc.date.available | 2026-07-07T11:42:31Z | |
| dc.description | We present a Bayesian model selection analysis of WMAP3 data using our code CosmoNest. We focus on the density perturbation spectral index $n_S$ and the tensor-to-scalar ratio $r$, which define the plane of slow-roll inflationary models. We find that while the Bayesian evidence supports the conclusion that $n_S \neq 1$, the data are not yet powerful enough to do so at a strong or decisive level. If tensors are assumed absent, the current odds are approximately 8 to 1 in favour of $n_S \neq 1$ under our assumptions, when WMAP3 data is used together with external data sets. WMAP3 data on its own is unable to distinguish between the two models. Further, inclusion of $r$ as a parameter weakens the conclusion against the Harrison-Zel'dovich case (n_S = 1, r=0), albeit in a prior-dependent way. In appendices we describe the CosmoNest code in detail, noting its ability to supply posterior samples as well as to accurately compute the Bayesian evidence. We make a first public release of CosmoNest, now available at http://www.cosmonest.org. | |
| dc.description | 7 pages RevTex with 4 figures included. Updated to match PRD accepted version. Main results unchanged. CosmoNest code now version 1.0 and includes calculation of the Information. Code available at http://www.cosmonest.org | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0605003 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0605003 | |
| dc.identifier | Phys.Rev.D73:123523,2006 | |
| dc.identifier | doi:10.1103/PhysRevD.73.123523 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/200912 | |
| dc.subject | Astrophysics | |
| dc.title | A Bayesian model selection analysis of WMAP3 | |
| dc.type | text |