A model for halo formation with axion mixed dark matter

By D. Marsh, J. Silk. 2013

184 citations recorded by the source corpus.

There are several issues to do with dwarf galaxy predictions in the standard CDM cosmology that have suscitated much recent debate about the possible modication of the nature of dark matter as providing a solution. We explore a novel solution involving ultra-light axions that can potentially resolve the missing satellites problem, the cusp-core problem, and the ‘too big to fail’ problem. We discuss approximations to non-linear structure formation in dark matter models containing a component of ultra-light axions across four orders of magnitude in mass, 10 24 eV . ma . 10 20 eV, a range too heavy to be well constrained by linear cosmological probes such as the CMB and matter power spectrum, and too light/non-interacting for other astrophysical or terrestrial axion searches. We nd that an axion of mass ma 10 21 eV contributing approximately 85% of the total dark matter can introduce a signicant kpc

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/09985be16bdc76c565500ac8f587df3f62fb5042

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Citations in the corpus

CONTRASTING GALAXY FORMATION FROM QUANTUM WAVE DARK MATTER, ψDM, WITH ΛCDM, USING PLANCK AND HUBBLE DATA (2015, background): “…(e.g., Mielke & Pérez 2009; Woo & Chiueh 2009; Chavanis 2011; Suárez & Matos 2011; Robles & Matos 2012; Bray & Goetz 2014; Lora & Magaña 2014; Marsh & Silk 2014; Rindler-Daller & Shapiro 2014; Suárez et al. 2014; Bozek et al. 2015; Guzmán & Lora-Clavijo 2015; Harko & Lobo 2015; Madarassy &…”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, methodology): “[838] showed that in this regard it may out-perform WDM and avoid the so-called “Catch 22” of WDM whereby one cannot form dwarf galaxies and simultaneously give large core radii to their density profiles.”
Constraining the mass of light bosonic dark matter using SDSS Lyman-α forest (2017, methodology): “Viel et al. (2013a); Baur et al. (2016)) to the FDM scenario, by using the correspondance between ma and mX which matches the cutoff position kc in the linear matter power spectrum (Marsh & Silk 2014).”
CMB-S4 Science Case, Reference Design, and Project Plan (2019, background): “Realizing this sensitivity will require better modeling of the non-linear clustering of axions [315], building upon and applying the results of previous work [316, 317, 318, 319, 320, 321, 322, 323, 324, 325, 326, 327, 328, 329, 330, 331, 332].”
Ultralight scalars as cosmological dark matter (2016, methodology): “We close by discussing WDM constraints from Lyman-α forest data on large scales and low redshifts (k ∼ 0.06– 1.6 Mpc−1, z ∼ 2.2–4.4), for instance Seljak et al. [185], and more recently, Baur et al. [186]—the latter gave a 2σ lower limit of mWDM > 4.1 keV.”