Unifying inflation and dark matter with the Peccei-Quinn field: Observable axions and observable tensors

Fairbairn, Malcolm; Hogan, Robert; Marsh, David J. E.

doi:10.1103/physrevd.91.023509

Cited by 51 publications

(66 citation statements)

References 65 publications

(72 reference statements)

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“…Although we considered the case of Higgs boson as the inflaton, we can also regard the PQ scalar as the inflaton in a similar way, by introducing a non-minimal coupling as [11] …”

Section: Discussionmentioning

confidence: 99%

“…Otherwise, the PQ symmetry may be restored after inflation and isocurvature constraint disappears, but there arises a serious domain wall problem. Conditions (11), (15), (16) and (17) are satisfied for reasonable choice of parameters.…”

Section: Toy Model Analysismentioning

confidence: 93%

“…For example, the PQ scale during inflation may be much larger than that in the present vacuum. In this case, the isocurvature perturbation is suppressed by the ratio of the PQ scale at present and during inflation [8]: see also [9][10][11][12]. Another way is to make the axion heavy during inflation so that it does not obtain large scale quantum fluctuations due to the stronger QCD [12][13][14][15] or the explicit PQ breaking term [16,17].…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Higgs inflation and suppression of axion isocurvature perturbation

Nakayama

Takimoto

2015

Physics Letters B

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“…Although we considered the case of Higgs boson as the inflaton, we can also regard the PQ scalar as the inflaton in a similar way, by introducing a non-minimal coupling as [11] …”

Section: Discussionmentioning

confidence: 99%

Section: Toy Model Analysismentioning

confidence: 93%

Section: Introductionmentioning

confidence: 99%

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Higgs inflation and suppression of axion isocurvature perturbation

Nakayama

Takimoto

2015

Physics Letters B

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“…These conclusions can be avoided if some of our cosmological assumptions are relaxed. An example non-minimal inflation model producing r T > 10 −3 consistent with the broken PQ scenario and high f a , uses the radial PQ field, χ, as the inflaton, non-minimally coupled to gravity (similarly to Higgs inflation) [234]. Such a scenario can allow for simultaneous detection of DM axions by CASPEr [235] (see Section 9.5.2), and detection of r T by, e.g., spider [236].…”

Section: Isocurvature and Axions As A Probe Of Inflationmentioning

confidence: 99%

Axion cosmology

2016

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Axions comprise a broad class of particles that can play a major role in explaining the unknown aspects of cosmology. They are also well-motivated within high energy physics, appearing in theories related to CP -violation in the standard model, supersymmetric theories, and theories with extra-dimensions, including string theory, and so axion cosmology offers us a unique view onto these theories. I review the motivation and models for axions in particle physics and string theory. I then present a comprehensive and pedagogical view on the cosmology and astrophysics of axion-like particles, starting from inflation and progressing via BBN, the CMB, reionization and structure formation, up to the present-day Universe. Topics covered include: axion dark matter (DM); direct and indirect detection of axions, reviewing existing and future experiments; axions as dark radiation; axions and the cosmological constant problem; decays of heavy axions; axions and stellar astrophysics; black hole superradiance; axions and astrophysical magnetic fields; axion inflation, and axion DM as an indirect probe of inflation. A major focus is on the population of ultralight axions created via vacuum realignment, and its role as a DM candidate with distinctive phenomenology. Cosmological observations place robust constraints on the axion mass and relic density in this scenario, and I review where such constraints come from. I next cover aspects of galaxy formation with axion DM, and ways this can be used to further search for evidence of axions. An absolute lower bound on DM particle mass is established. It is ma > 10 −24 eV from linear observables, extending to ma 10 −22 eV from nonlinear observables, and has the potential to reach ma 10 −18 eV in the future. These bounds are weaker if the axion is not all of the DM, giving rise to limits on the relic density at low mass. This leads to the exciting possibility that the effects of axion DM on structure formation could one day be detected, and the axion mass and relic density measured from cosmological observables.

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“…of the QCD axion) or f a (e.g. [39,43,44,45,46,47]) can also modify the cosmological evolution of the axion.…”

Section: Comments On Axion-like Fieldsmentioning

confidence: 99%

Lyman- α constraints on ultralight scalar dark matter: Implications for the early and late universe

et al. 2017

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We investigate constraints on scalar dark matter (DM) by analyzing the Lyman-α forest, which probes structure formation at medium and small scales, and also by studying its cosmological consequences at high and low redshift. For scalar DM that constitutes more than 30% of the total DM density, we obtain a lower limit m 10 −21 eV for the mass of scalar DM. This implies an upper limit on the initial field displacement (or the decay constant for an axion-like field) of φ 10 16 GeV. We also derive limits on the energy scale of cosmic inflation and establish an upper bound on the tensor-to-scalar ratio of r < 10 −3 in the presence of scalar DM. Furthermore, we show that there is very little room for ultralight scalar DM to solve the "small-scale crisis" of cold DM without spoiling the Lyman-α forest results. The constraints presented in this paper can be used for testing generic theories that contain light scalar fields.

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Unifying inflation and dark matter with the Peccei-Quinn field: Observable axions and observable tensors

Cited by 51 publications

References 65 publications

Higgs inflation and suppression of axion isocurvature perturbation

Higgs inflation and suppression of axion isocurvature perturbation

Axion cosmology

Lyman- α constraints on ultralight scalar dark matter: Implications for the early and late universe

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