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@ARTICLE{Melville:192487,
      author       = {Melville, Scott and Lerner, Rose},
      title        = {{Q}uantifying the `naturalness' of the curvaton model},
      journal      = {Journal of cosmology and astroparticle physics},
      volume       = {2014},
      number       = {07},
      issn         = {1475-7516},
      address      = {London},
      publisher    = {IOP},
      reportid     = {PUBDB-2014-04084, DESY-14-015. arXiv:1402.3176},
      pages        = {026},
      year         = {2014},
      note         = {(c) IOP Publishing Ltd and Sissa Medialab srl},
      abstract     = {We investigate the probability of obtaining an observable
                      curvature perturbation, using as an example the minimal
                      curvaton-higgs (MCH) model. We determine ``probably
                      observable'' and ``probably excluded'' regions of parameter
                      space assuming generic initial conditions and applying a
                      stochastic approach for the curvaton's evolution during
                      inflation. Inflation is assumed to last longer than the
                      N(obs) simeq 55 observable e-folds, and the total number of
                      e-folds of inflation determines the particular ranges of
                      parameters that are probable. For the MCH model, these
                      ``probably observable'' regions always lie within the range
                      8 × 10(4) GeV ≤ m(σ) ≤ 2 × 10(7) GeV, where m(σ)
                      is the curvaton mass, and the Hubble scale at horizon exit
                      is chosen as H(*) = 10(10) GeV. Because the ``probably
                      observable'' region depends on the total duration of
                      inflation, information on parameters in the Lagrangian from
                      particle physics and from precision CMB observations can
                      therefore provide information about the total duration of
                      inflation, not just the last N(obs) e-folds. This method
                      could also be applied to any model that contains additional
                      scalar fields to determine the probability that these scalar
                      fields contribute to the curvature perturbation.},
      keywords     = {curvature: perturbation (INSPIRE) / field theory: scalar
                      (INSPIRE) / curvaton: mass (INSPIRE) / inflation (INSPIRE) /
                      cosmic background radiation (INSPIRE) / boundary condition
                      (INSPIRE) / stochastic (INSPIRE) / horizon (INSPIRE)},
      cin          = {T},
      ddc          = {530},
      cid          = {I:(DE-H253)T-20120731},
      pnm          = {514 - Theoretical Particle Physics (POF2-514)},
      pid          = {G:(DE-HGF)POF2-514},
      experiment   = {EXP:(DE-MLZ)NOSPEC-20140101},
      typ          = {PUB:(DE-HGF)16},
      UT           = {WOS:000339802700027},
      eprint       = {1402.3176},
      howpublished = {arXiv:1402.3176},
      archivePrefix = {arXiv},
      SLACcitation = {$\%\%CITATION$ = $arXiv:1402.3176;\%\%$},
      doi          = {10.1088/1475-7516/2014/07/026},
      url          = {https://bib-pubdb1.desy.de/record/192487},
}