Imprint of spatial curvature on inflation power spectrum

Abstract

If the universe had a large curvature before inflation there is a deviation from the scale invariant perturbations of the inflaton at the beginning of inflation. This may have some effect on the CMB anisotropy at large angular scales. We calculate the density perturbations for both open and closed universe cases using the Bunch-Davies vacuum condition on the initial state. We use our power spectrum to calculate the temperature anisotropy spectrum and compare the results with the WMAP three year data. We find that our power spectrum gives a lower quadrupole anisotropy when $\Omega -1>0$, but matches the temperature anisotropy calculated from the standard Ratra-Peebles power spectrum at large $l$. The determination of spatial curvature from temperature anisotropy data is not much affected by the different power spectra which arise from the choice of different boundary conditions for the inflaton perturbation.

arXiv comment17 pages, 4 figures, revtex4; section on comparison with WMAP3 data added

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Cited by in corpus (14)

• Planck 2015 constraints on the non-flat $\Lambda$CDM inflation model
• Primordial backgrounds of relic gravitons
• Pixelated Dark Energy
• Inflation in a closed universe
• Inflation in the closed FLRW model and the CMB
• Current data are consistent with flat spatial hypersurfaces in the $\Lambda$CDM cosmological model but favor more lensing than the model predicts
• Lorentzian Vacuum Transitions: Open or Closed Universes?
• General theory of cosmological perturbations in open and closed universes from the Horndeski action
• Non-Gaussianity as a signature of thermal initial condition of inflation
• Large Scale Suppression of Scalar Power on a Spatial Condensation
• Role of spatial curvature in the primordial gravitational wave power spectrum
• Quantum initial conditions for curved inflating universes
• Slow-roll inflationary senario in the maximally extended background
• Tilted non-spatially-flat inflation