Cosmological parameter estimation and the spectral index from inflation

Details Cosmological parameter estimation and the spectral index from inflation Cosmological parameter estimation and the spectral index from inflation

1997-12-02

arxiv.org/abs/astro-ph/9712028v2

Mon.Not.Roy.Astron.Soc.298:1233,1998

Astronomy and Astrophysics

Astrophysics

6 pages LaTeX file with one figure incorporated (uses mn.sty and epsf). Important modifications to results

Scientific paper

10.1046/j.1365-8711.1998.01727.x

Accurate estimation of cosmological parameters from microwave background anisotropies requires high-accuracy understanding of the cosmological model. Normally, a power-law spectrum of density perturbations is assumed, in which case the spectral index $n$ can be measured to around $\pm 0.004$ using microwave anisotropy satellites such as MAP and Planck. However, inflationary models generically predict that the spectral index $n$ of the density perturbation spectrum will be scale-dependent. We carry out a detailed investigation of the measurability of this scale dependence by Planck, including the influence of polarization on the parameter estimation. We also estimate the increase in the uncertainty in all other parameters if the scale dependence has to be included. This increase applies even if the scale dependence is too small to be measured unless it is assumed absent, but is shown to be a small effect. We study the implications for inflation models, beginning with a brief examination of the generic slow-roll inflation situation, and then move to a detailed examination of a recently-devised hybrid inflation model for which the scale dependence of $n$ may be observable.

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