Dark matter from an ultra-light pseudo-Goldsone-boson

By Luca Amendola, R. Barbieri. 2005

169 citations recorded by the source corpus.

Abstract Dark matter (DM) and dark energy (DE) can be both described in terms of ultra-light pseudo-Goldstone-bosons (PGB) with masses m DM ≳ 10 −23 eV and m DE ≲ 10 −33 eV respectively. Following Barbieri et al., we entertain the possibility that a PGB exists with mass m I intermediate between these two limits, giving a partial contribution to DM. We evaluate the related effects on the power spectrum of the matter density perturbations and on the cosmic microwave background and we derive the bounds on the density fraction, f I , of this intermediate field from current data, with room for a better sensitivity on f I in the near future. We also give a simple and unified analytic description of the free streaming effects both for an ultra-light scalar and for a massive neutrino.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/1cf9f699952205e884aca294566be7a79f2f8623

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Citations in the corpus

Using the Full Power of the Cosmic Microwave Background to Probe Axion Dark Matter (2017, methodology): “In the intervening nine orders of magnitude in axion mass, the CMB provides stringent constraints on the axion energy density, leading to a “U-shaped” posterior distribution in the (ma,Ωah2) plane (H15, Amendola & Barbieri 2006).”
Axion dark matter, solitons and the cusp–core problem (2015, result): “This HUDF bound is, however, still rather conservative compared to other constraints to ULAs using non-linear scales (e.g. Lyman α forest; Amendola & Barbieri 2006).”
Constraining the mass of light bosonic dark matter using SDSS Lyman-α forest (2017, unknown): “In fact, Amendola & Barbieri (2006) disfavors pure FDM models with ma 10−22 eV, by making use essentially of highresolution Lyman-α forest spectra.”
Pulsar timing signal from ultralight scalar dark matter (2013, background): “We would also like to note, that an even lighter scalar field would behave as hot dark matter and would fail to form observed structures, unless it constitutes a subdominant fraction of all dark matter [7].”
CONTRASTING GALAXY FORMATION FROM QUANTUM WAVE DARK MATTER, ψDM, WITH ΛCDM, USING PLANCK AND HUBBLE DATA (2015, background): “Various observable properties of this model have been proposed (Amendola & Barbieri 2006; Arvanitaki & Dubovsky 2011; Schive et al. 2014a, 2014b; Khmelnitsky & Rubakov 2014; Hlozek et al. 2015; Van Tilburg et al. 2015; Stadnik & Flambaum 2015).”
Galaxy UV-luminosity function and reionization constraints on axion dark matter (2014, methodology): “Amendola & Barbieri (2006) used older Lyman-α data to constrain ULAs, placing the bound ma > 5×10−23 eV if the ULA is to be all of the DM. Analyses of the Lyman-α forest involve considerable complexity related to the non-linear mapping of the optical depth and to the required calibration from…”
A model for halo formation with axion mixed dark matter (2013, methodology): “1 eV (Amendola & Barbieri 2006; Marsh et al. 2012).”
Gravitational probes of dark matter physics (2017, background): “(43) With mF in the range of 10 6 − 1011 GeV, the gravitino masses can range from ∼ 100 eV up to 100 TeV.”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, background): “10−29 eV are similar in many ways to massive neutrinos [49], the major difference being that their non-thermal production breaks the link between the scale of suppression, km, and the fraction of dark matter, fax, through the dependence of fax on the initial field value φi.”
The Simons Observatory: science goals and forecasts (2018, background): “…2010), however we consider here not the QCD axion with mass ∼ 10−7 eV but its much lighter cousin, the ULA, with masses between 10−33 < ma/eV < 10 −22 (Amendola and Barbieri 2006; Arvanitaki et al. 2010a; Hui et al. 2017) The light end of the mass range are axions that exhibit dark-energy-like…”