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Warm Little Inflaton Becomes Cold Dark Matter

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Warm Little Inflaton Becomes Cold Dark Matter PHYSICAL REVIEW LETTERS 122, 161301 (2019) Warm Little Inflaton Becomes Cold Dark Matter † João G. Rosa* and Luís B. Ventura Departamento de Física da Universidade de Aveiro and CIDMA, Campus de Santiago, 3810-183 Aveiro, Portugal (Received 22 November 2018; published 24 April 2019) 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 and particle content 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 postinflationary epochs. The latter behaves as dark radiation during nucleosynthesis, leading to a non-negligible contribution to the effective number of relativistic degrees of freedom, and becomes the dominant cold dark matter component in the Universe shortly before matter-radiation equality for inflaton masses in the 10−4–10−1 eV range. Cold dark matter isocurvature perturbations, anticorrelated with the main adiabatic component, provide a smoking gun for this scenario that can be tested in the near future. DOI: 10.1103/PhysRevLett.122.161301 Inflation [1] has inevitably become a part of the modern can smoothly take over as the dominant component at the cosmological paradigm. Observations are consistent with end of inflation, with no need for a reheating period its predictions of a flat universe with a nearly scale- [11,12]. Since dissipation induces small thermal fluctua- invariant, Gaussian, and adiabatic spectrum of primordial tions of the inflaton field about the background value ϕ, the density perturbations [2]. However, the exact nature of the primordial spectrum of curvature perturbations can differ inflaton field and its scalar potential remain open questions significantly in the cold and warm inflation scenarios that may hopefully be addressed with future measurements [13–20], the latter, e.g., predicting a suppression of the of B modes in the cosmic microwave background (CMB) tensor-to-scalar ratio in chaotic models [11,13,19]. Warm polarization, as well as possibly non-Gaussian features and inflation thus provides a unique observational window into isocurvature perturbations. inflationary particle physics. The present ambiguity is no less apparent when one Warm inflation models were, however, hindered by regards two consistent, yet distinct, descriptions of this several technical difficulties [21,22]. Interactions between 2 2 2 period of accelerated expansion: cold and warm inflation the inflaton and other fields, e.g., g ϕ χ or gϕψψ¯ , typically [3,4]. The former is described by the overdamped motion of give the latter a large mass. On the one hand, to keep the one (or more) field(s), coupled solely with gravity, whose fields light, and also avoid the associated large thermal nearly flat potential dominates the energy content of the corrections to the inflaton potential, one must consider small Universe, acting as an effective cosmological constant for a coupling constants that make dissipative effects too feeble to finite period. Inflaton quantum fluctuations then act as sustain a radiation bath for ∼50–60 e folds of inflation. On seeds for structure formation and CMB anisotropies. the other hand, heavy fields acting as mediators between the If, however, interactions between the inflaton, ϕ, and inflaton and the light degrees of freedom in the radiation bath other fields are non-negligible during inflation, dissipative can yield sufficiently strong dissipative effects [23–26],but effects transfer the inflaton’s energy into light degrees of at the expense of considering a large number of such freedom (DOF), sustaining a subdominant radiation bath mediators that may only be present in certain string con- that significantly changes the dynamics of inflation [5].In structions [27] or extradimensional models [28]. particular, the additional dissipation makes the inflaton These shortcomings were recently overcome in the warm field roll more slowly than in the cold case [6]. When little inflaton (WLI) scenario, which provides the only dissipation becomes sufficiently strong, the radiation bath consistent model of warm inflation with only two light fields coupled to the inflaton [29]. In this Letter, we show, for the first time, that the underlying symmetries and particle content of this model necessarily lead to a stable Published by the American Physical Society under the terms of inflaton remnant that survives until the present day, the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to naturally accounting for the cold dark matter component the author(s) and the published article’s title, journal citation, in our Universe. In this sense, warm inflation implies and DOI. Funded by SCOAP3. inflaton–dark matter unification. 0031-9007=19=122(16)=161301(6) 161301-1 Published by the American Physical Society PHYSICAL REVIEW LETTERS 122, 161301 (2019) This is hard to implement within the cold inflation a chiral rotation. Hence, the only effects of the inflaton paradigm because the inflaton must decay efficiently at field’s interactions with the fermions are related to its the end of inflation to ensure a successful “reheating” of the dynamical nature; i.e., they correspond to nonlocal con- Universe, but cannot do so completely to provide a tributions to the effective action, in particular dissipative sufficiently long-lived dark relic [30]. This can be achieved effects. by introducing additional symmetries or cosmological The interchange symmetry corresponds to a Z2 reflec- phase(s) which, however, do not affect the inflationary tion for the inflaton field, ϕ ↔ −ϕ, that protects it from dynamics and have, in general, no direct observational decaying into any other fields besides the fermions ψ 1;2.As imprint [31–38]. discussed below, a significant dissipation of the inflaton’s In this Letter, we propose a radically different unification energy implies gM ≲ T ≲ M, which is only satisfied during scenario, where the inflaton decays during, but not after, inflation, thus ensuring the stability of the inflaton in the inflation. We show that this is possible due to the very same postinflationary Universe. symmetries that protect the scalar potential against thermal The fermion fields may decay into light scalar and and quantum corrections, independently of its form, while fermion fields, σ and ψ σ, respectively, with appropriate allowing for sufficiently strong adiabatic dissipation effects U(1) charges, through Yukawa interactions: that become exponentially suppressed once the inflaton X exits the slow-roll regime and radiation smoothly takes −Lψσ ¼ −hσ ðψ¯ iLψ σR þ ψ¯ σLψ iRÞ: ð3Þ over. These symmetries then ensure that the inflaton i¼1;2 behaves as a stable cold relic while oscillating about the minimum of its potential at late times, regardless of the full The dissipation coefficient resulting from the inflaton- form of the scalar potential. fermion interactions can be computed using standard ϕ The WLI model includes two complex scalar fields, 1;2, thermal field theory tools in the adiabatic regime with equal charge q under a U(1) gauge symmetry that is [5,25,39], where the fermions are kept close to thermal spontaneously broken by their identical vacuum expect- pffiffiffi equilibrium through decays and inverse decays, Γψ ≳ H ≫ ation values, hϕ1i¼hϕ2i ≡ M= 2. This yields masses of jϕ_ =ϕj [40]. Its dominant contribution corresponds to on- order M for the radial scalar components and the U(1) shell fermion production [26], being given by: gauge field that then decouple from the dynamics for ≲ temperatures T M. The remaining physical light degree 2 Z 3 g d p Γψ of freedom is the relative phase between ϕ1 and ϕ2, which ϒ ¼ 4 ðω Þ½1 − ðω Þ ð Þ 3 2 nF p nF p ; 4 we identify as the inflaton field, ϕ: T ð2πÞ mψ pffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffi M iϕ=M M −iϕ=M ¼ 2 2 þ 2 2 8 ϕ1 ¼ pffiffiffi e ; ϕ2 ¼ pffiffiffi e : ð1Þ where mψ g M h T = is the thermally corrected 2 2 qffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffi 2 2 fermion mass, ωp ¼ jpj þ mψ , Γψ is the fermion decay ψ 1 ψ 2 The model also includes a pair of fermions, and , width (see Ref. [29]) and nF is the Fermi-Dirac distribution. whose left-handed (right-handed) components have U(1) The momentum integral can be computed analytically for charge q (0), and we impose an interchange symmetry mψ =T ≪ 1 and mψ =T ≫ 1, yielding: ϕ1 ↔ ϕ2, ψ 1 ↔ ψ 2, such that the allowed Yukawa inter- actions are given by: 2 2 2g h 1 mψ ϒ ≈ T − ln ;mψ =T ≪ 1; 1 1 ð2πÞ3 5 T pffiffiffi ¯ pffiffiffi ¯ rffiffiffirffiffiffiffiffiffiffi −Lϕψ ¼ gϕ1ψ 1Lψ 1R þ gϕ2ψ 2Lψ 2R þ H:c: 2 2 2 2 2g h π mψ ϒ ≈ −ðmψ =TÞ ≫ 1 ð Þ 3 T e ;mψ =T : 5 iγ5ϕ=M −iγ5ϕ=M ð2πÞ 2 ¼ gMψ¯ 1e ψ 1 þ gMψ¯ 2e ψ 2; ð2Þ T where we have also imposed the sequestering of the “1” and In the high temperature regime relevant during inflation, the “2” sectors, which may be achieved, e.g., by considering dissipation coefficient is proportional to the temperature as additional global symmetries for each sector or by physi- in the original WLI model, although the proportionality cally separating them along an extra compact dimension. constant is smaller in this case. Inflationary observables can This is in contrast with the original WLI proposal [29], thus be computed as in Refs. [29,41,42], to which we refer providing the additional appealing feature that the fermion the interested reader. After inflation, dissipative effects are masses, m1 ¼ m2 ¼ gM, and therefore the associated exponentially suppressed as the ψ 1;2 fermions become radiative and thermal corrections to the effective potential nonrelativistic, halting the energy transfer between the are independent of the inflaton field.
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