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Title: Dark matter chaotic inflation in light of BICEP2

Abstract

We propose an economical model in which a singlet {sub 2}-odd scalar field accounts for the primordial inflation and the present dark matter abundance simultaneously in the light of recent BICEP2 result. Interestingly, the reheating temperature and the thermal dark matter abundance are closely connected by the same interaction between the singlet scalar and the standard model Higgs. In addition, the reheating temperature turns out to be quite high, T{sub R} ∼> 10{sup 12} GeV, and hence the thermal leptogenesis is compatible with this model. Therefore, it can be one of the simplest cosmological scenarios.

Authors:
;  [1]
  1. Department of Physics, Faculty of Science, University of Tokyo, Bunkyo-ku, Tokyo 133-0033 (Japan)
Publication Date:
OSTI Identifier:
22373367
Resource Type:
Journal Article
Resource Relation:
Journal Name: Journal of Cosmology and Astroparticle Physics; Journal Volume: 2014; Journal Issue: 08; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ABUNDANCE; CHAOS THEORY; COSMOLOGICAL INFLATION; GEV RANGE; HIGGS BOSONS; HIGGS MODEL; NONLUMINOUS MATTER; PARTICLE PRODUCTION; SCALAR FIELDS; STANDARD MODEL

Citation Formats

Mukaida, Kyohei, and Nakayama, Kazunori, E-mail: mukaida@hep-th.phys.s.u-tokyo.ac.jp, E-mail: kazunori@hep-th.phys.s.u-tokyo.ac.jp. Dark matter chaotic inflation in light of BICEP2. United States: N. p., 2014. Web. doi:10.1088/1475-7516/2014/08/062.
Mukaida, Kyohei, & Nakayama, Kazunori, E-mail: mukaida@hep-th.phys.s.u-tokyo.ac.jp, E-mail: kazunori@hep-th.phys.s.u-tokyo.ac.jp. Dark matter chaotic inflation in light of BICEP2. United States. doi:10.1088/1475-7516/2014/08/062.
Mukaida, Kyohei, and Nakayama, Kazunori, E-mail: mukaida@hep-th.phys.s.u-tokyo.ac.jp, E-mail: kazunori@hep-th.phys.s.u-tokyo.ac.jp. Fri . "Dark matter chaotic inflation in light of BICEP2". United States. doi:10.1088/1475-7516/2014/08/062.
@article{osti_22373367,
title = {Dark matter chaotic inflation in light of BICEP2},
author = {Mukaida, Kyohei and Nakayama, Kazunori, E-mail: mukaida@hep-th.phys.s.u-tokyo.ac.jp, E-mail: kazunori@hep-th.phys.s.u-tokyo.ac.jp},
abstractNote = {We propose an economical model in which a singlet {sub 2}-odd scalar field accounts for the primordial inflation and the present dark matter abundance simultaneously in the light of recent BICEP2 result. Interestingly, the reheating temperature and the thermal dark matter abundance are closely connected by the same interaction between the singlet scalar and the standard model Higgs. In addition, the reheating temperature turns out to be quite high, T{sub R} ∼> 10{sup 12} GeV, and hence the thermal leptogenesis is compatible with this model. Therefore, it can be one of the simplest cosmological scenarios.},
doi = {10.1088/1475-7516/2014/08/062},
journal = {Journal of Cosmology and Astroparticle Physics},
number = 08,
volume = 2014,
place = {United States},
year = {Fri Aug 01 00:00:00 EDT 2014},
month = {Fri Aug 01 00:00:00 EDT 2014}
}
  • The announcement by BICEP2 of the detection of B-mode polarization consistent with primordial gravitational waves with a tensor-to-scalar ratio, r=0.2{sup +0.07}{sub −0.05}, challenged predictions from most inflationary models of a lower value for r. More recent results by Planck on polarized dust emission show that the observed tensor modes signal is compatible with pure foreground emission. A more significant constraint on r was then obtained by a joint analysis of Planck, BICEP2 and Keck Array data showing an upper limit to the tensor to scalar ratio r≤ 0.12, excluding the case 0r= with low statistical significance. Forthcoming measurements by BICEP3, themore » Keck Array, and other CMB polarization experiments, open the possibility for making the fundamental measurement of r. Here we discuss how r sets the scale for models where the dark matter is created at the inflationary epoch, the generically called super-heavy dark matter models. We also consider the constraints on such scenarios given by recent data from ultrahigh energy cosmic ray observatories which set the limit on super-heavy dark matter particles lifetime. We discuss how super-heavy dark matter can be discovered by a precise measurement of r combined with future observations of ultra high energy cosmic rays.« less
  • Following the ground-breaking measurement of the tensor-to-scalar ratio r=0.20{sup +0.07}{sub -0.05} by the BICEP2 collaboration, we perform a statistical analysis of a model that combines Radiative Inflation with Dark Energy (RIDE) based on the M{sup 2}|Φ|{sup 2}ln(|Φ|{sup 2}/Λ{sup 2}) potential and compare its predictions to those based on the traditional chaotic inflation M{sup 2}|Φ|{sup 2} potential. We find a best-fit value in the RIDE model of r=0.18 as compared to r=0.17 in the chaotic model, with the spectral index being n{sub S}=0.96 in both models.
  • The magnitude of primordial tensor perturbations reported by the BICEP2 experiment is consistent with simple models of chaotic inflation driven by a single scalar field with a power-law potential ∝ φ{sup n} : n ≅ 2, in contrast to the WMAP and Planck results, which favored models resembling the Starobinsky R+R{sup 2} model if running of the scalar spectral index could be neglected. While models of inflation with a quadratic potential may be constructed in simple N = 1 supergravity, these constructions are more challenging in no-scale supergravity. We discuss here how quadratic inflation can be accommodated within supergravity, focusingmore » primarily on the no-scale case. We also argue that the quadratic inflaton may be identified with the supersymmetric partner of a singlet (right-handed) neutrino, whose subsequent decay could have generated the baryon asymmetry via leptogenesis.« less
  • The cosmic microwave background 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)/dlnk) on the degree of the potential (2n) 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 LSSmore » data narrows for growing n. New inflation yields 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) x 10-4<=dn(s)/dlnk<=-2 x 10-4. (The values of r, n(s), dn(s)/dlnk for arbitrary N(e) follow by a simple rescaling from the N(e)=50 values.) A reconstruction program is carried out suggesting quite generally that for n(s) consistent with the WMAP3 and LSS data and r<0.1 the symmetry breaking scale for new inflation is |phi0|~;;10MPl while the field scale at Hubble crossing is lbar phi(c) rbar~;;M(Pl). The family of chaotic models features 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)/dlnk with a narrow window in field amplitude around |phi(c)|~;;15M(Pl). We conclude that a measurement of r<0.16 (for N(e)=50) distinctly rules out a large class of chaotic scenarios and favors small field new inflationary models. As a general consequence, new inflation emerges more favored than chaotic inflation.« less
  • The cosmic microwave background 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{sub e}, where N{sub e}{approx}50 is the number of e-folds before the end of inflation. We study the dependence of the observables (n{sub s}, r and dn{sub s}/dlnk) on the degree of the potential (2n) 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 withmore » the WMAP3 and LSS data narrows for growing n. New inflation yields a good fit to the r and n{sub 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{sub e}=50). All members of the new inflation family predict a small but negative running -4(n+1)x10{sup -4}{<=}dn{sub s}/dlnk{<=}-2x10{sup -4}. (The values of r, n{sub s}, dn{sub s}/dlnk for arbitrary N{sub e} follow by a simple rescaling from the N{sub e}=50 values.) A reconstruction program is carried out suggesting quite generally that for n{sub s} consistent with the WMAP3 and LSS data and r<0.1 the symmetry breaking scale for new inflation is vertical bar {phi}{sub 0} vertical bar {approx}10M{sub Pl} while the field scale at Hubble crossing is vertical bar {phi}{sub c} vertical bar {approx}M{sub Pl}. The family of chaotic models features r{>=}0.16 (for N{sub e}=50) and only a restricted subset of chaotic models are consistent with the combined WMAP3 bounds on r, n{sub s}, dn{sub s}/dlnk with a narrow window in field amplitude around vertical bar {phi}{sub c} vertical bar {approx}15M{sub Pl}. We conclude that a measurement of r<0.16 (for N{sub e}=50) distinctly rules out a large class of chaotic scenarios and favors small field new inflationary models. As a general consequence, new inflation emerges more favored than chaotic inflation.« less