Warm Little Inflaton becomes Cold Dark Matter. (arXiv:1811.05493v1 [hep-ph])
<a href="http://arxiv.org/find/hep-ph/1/au:+Rosa_J/0/1/0/all/0/1">Joao G. Rosa</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Ventura_L/0/1/0/all/0/1">Luis B. Ventura</a>
We present a model where the inflaton can naturally account for all the dark
matter in the Universe within the warm inflation paradigm. In particular, we
show that the symmetries of the Warm Little Inflaton scenario (i) avoid large
thermal and radiative corrections to the scalar potential, (ii) allow for
sufficiently strong dissipative effects to sustain a radiation bath during
inflation that becomes dominant at the end of the slow-roll regime, and (iii)
enable a stable inflaton remnant in the post-inflationary epochs. The latter
behaves as dark radiation until parametrically before matter-radiation
equality, leading to a non-negligible contribution to the effective number of
relativistic degrees of freedom during nucleosynthesis, becoming the dominant
cold dark matter component in the Universe for inflaton masses in the
$10^{-4}-10^{-1}$ eV range. Cold dark matter isocurvature perturbations,
anti-correlated with the main adiabatic component, provide a smoking gun for
this scenario that can be tested in the near future.
We present a model where the inflaton can naturally account for all the dark
matter in the Universe within the warm inflation paradigm. In particular, we
show that the symmetries of the Warm Little Inflaton scenario (i) avoid large
thermal and radiative corrections to the scalar potential, (ii) allow for
sufficiently strong dissipative effects to sustain a radiation bath during
inflation that becomes dominant at the end of the slow-roll regime, and (iii)
enable a stable inflaton remnant in the post-inflationary epochs. The latter
behaves as dark radiation until parametrically before matter-radiation
equality, leading to a non-negligible contribution to the effective number of
relativistic degrees of freedom during nucleosynthesis, becoming the dominant
cold dark matter component in the Universe for inflaton masses in the
$10^{-4}-10^{-1}$ eV range. Cold dark matter isocurvature perturbations,
anti-correlated with the main adiabatic component, provide a smoking gun for
this scenario that can be tested in the near future.
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