New Inflation vs. Chaotic Inflation, Higher Degree Potentials and the Reconstruction Program in light of WMAP3

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dc.creatorBoyanovsky, D.
dc.creatorde Vega, H. J.
dc.creatorHo, C. M.
dc.creatorSanchez, N. G.
dc.date2007-02-23
dc.date2007-06-18
dc.date.accessioned2026-07-07T11:00:55Z
dc.date.available2026-07-07T11:00:55Z
dc.descriptionThe CMB power spectra are studied for different families of single field new and chaotic inflation models in the effective field theory approach to inflation. We implement a systematic expansion in 1/N_e where N_e ~ 50 is the number of e-folds before the end of inflation. We study the dependence of the observables (n_s, r and dn_s/d\ln k) on the degree of the potential (2 n) and confront them to the WMAP3 and large scale structure data: this shows in general that fourth degree potentials (n=2) provide the best fit to the data; the window of consistency with the WMAP3 and LSS data narrows for growing n. New inflation models yield a good fit to the r and n_s data in a wide range of field and parameter space. Small field inflation yields r<0.16 while large field inflation yields r>0.16 (for N_e=50). All members of the new inflation family predict a small but negative running -4(n+1)10^{-4}< dn_s/d\ln k <-2 10^{-4}. A reconstruction program is carried out suggesting quite generallythat for n_s consistent with the WMAP3 and LSS data and r<0.1 the symmetry breaking scale for new inflation is |ϕ_0| ~ 10 M_{Pl} while the field scale at Hubble crossing is |ϕ_{50}| ~ M_{Pl}.The family of chaotic models feature r>0.16 (for N_e=50) and only a restricted subset of chaotic models are consistent with the combined WMAP3 bounds on r, n_s,dn_s/d\ln k with a narrow window in field amplitude around |ϕ_{50}| ~ 15 M_{Pl}.A measurement of r<0.16 (for N_e =50) will distinctly rule out a large class of chaotic scenarios and will favor new inflationary models. As a general consequence, new inflation emerges more favoured than chaotic inflation.
dc.description19 pages, 18 figures. Minor additions. Matches version published in Phys. Rev. D
dc.identifierhttps://arxiv.org/abs/astro-ph/0702627
dc.identifierhttp://arxiv.org/abs/astro-ph/0702627
dc.identifierPhys.Rev.D75:123504,2007
dc.identifierdoi:10.1103/PhysRevD.75.123504
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/187807
dc.subjectAstrophysics
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectHigh Energy Physics - Phenomenology
dc.subjectHigh Energy Physics - Theory
dc.titleNew Inflation vs. Chaotic Inflation, Higher Degree Potentials and the Reconstruction Program in light of WMAP3
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