Cosmological Density Perturbations From A Quantum Gravitational Model Of Inflation

Details Cosmological Density Perturbations From A Quantum Gravitational Model Of Inflation Cosmological Density Perturbations From A Quantum Gravitational Model Of Inflation

1998-03-16

arxiv.org/abs/astro-ph/9803172v1

Fortsch.Phys. 47 (1999) 389-400

Astronomy and Astrophysics

Astrophysics

18 pages, LaTeX 2 epsilon, 1 eps file, uses epsfig

Scientific paper

We derive the implications for anisotropies in the cosmic microwave background following from a model of inflation in which a bare cosmological constant is gradually screened by an infrared process in quantum gravity. The model predicts that the amplitude of scalar perturbations is $A_S = (2.0 \pm .2) \times 10^{-5}$, that the tensor-to-scalar ratio is $r \approx 1.7 \times 10^{-3}$, and that the scalar and tensor spectral indices are $n \approx .97$ and $n_T \approx -2.8 \times 10^{-4}$, respectively. By comparing the model's power spectrum with the COBE 4-year RMS quadrupole, the mass scale of inflation is determined to be $M = (.72 \pm .03) \times 10^{16}~{\rm GeV}$. At this scale the model produces about $10^8$ e-foldings of inflation, so another prediction is $\Omega = 1$.

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