Imprint of spatial curvature on inflation power spectrum

Simple item page
dc.creatorMasso, Eduard
dc.creatorMohanty, Subhendra
dc.creatorNautiyal, Akhilesh
dc.creatorZsembinszki, Gabriel
dc.date2006-09-13
dc.date2007-09-26
dc.date.accessioned2026-07-07T11:57:26Z
dc.date.available2026-07-07T11:57:26Z
dc.descriptionIf 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 $Ω-1 >0$, 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.
dc.description17 pages, 4 figures, revtex4; section on comparison with WMAP3 data added
dc.identifierhttps://arxiv.org/abs/astro-ph/0609349
dc.identifierhttp://arxiv.org/abs/astro-ph/0609349
dc.identifierPhys.Rev.D78:043534,2008
dc.identifierdoi:10.1103/PhysRevD.78.043534
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/205884
dc.subjectAstrophysics
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectHigh Energy Physics - Phenomenology
dc.titleImprint of spatial curvature on inflation power spectrum
dc.typetext

Files

Collections

arXiv