Structure formation and microlensing with axion miniclusters
| Autor: | Simon Rozier, David J. E. Marsh, Jérémie Quevillon, Malcolm Fairbairn |
|---|---|
| Přispěvatelé: | Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), École polytechnique (X), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Laboratoire de Physique Subatomique et de Cosmologie ( LPSC ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut polytechnique de Grenoble - Grenoble Institute of Technology ( Grenoble INP ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ), École polytechnique ( X ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) |
| Jazyk: | angličtina |
| Rok vydání: | 2018 |
| Předmět: |
Particle physics
axion: oscillation Structure formation Cosmology and Nongalactic Astrophysics (astro-ph.CO) perturbation [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] Dark matter FOS: Physical sciences dark matter: collapse Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics hierarchy dark matter: direct detection dark matter: production Gravitational microlensing 01 natural sciences symmetry breaking horizon galaxy: formation High Energy Physics - Phenomenology (hep-ph) dark matter: halo 0103 physical sciences Galaxy formation and evolution Symmetry breaking structure 010303 astronomy & astrophysics Axion Astrophysics::Galaxy Astrophysics Physics axion: dark matter 010308 nuclear & particles physics Horizon High Energy Physics::Phenomenology quantum chromodynamics: axion Astrophysics - Astrophysics of Galaxies 3. Good health Dark matter halo High Energy Physics - Phenomenology gravitation Astrophysics of Galaxies (astro-ph.GA) [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph] non-Gaussianity axion-like particles [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph] [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] Astrophysics - Cosmology and Nongalactic Astrophysics |
| Zdroj: | Physical Review D Physical Review D, American Physical Society, 2018, 97 (8), pp.083502. ⟨10.1103/PhysRevD.97.083502⟩ Phys.Rev.D Phys.Rev.D, 2018, 97 (8), pp.083502. ⟨10.1103/PhysRevD.97.083502⟩ Phys.Rev.D, 2018, 97 (8), pp.083502. 〈10.1103/PhysRevD.97.083502〉 |
| ISSN: | 1550-7998 1550-2368 0038-5506 2296-424X |
| DOI: | 10.1103/PhysRevD.97.083502⟩ |
| Popis: | If the symmetry breaking responsible for axion dark matter production occurs during the radiation-dominated epoch in the early Universe, then this produces large amplitude perturbations that collapse into dense objects known as axion miniclusters. The characteristic minicluster mass, $M_0$, is set by the mass inside the horizon when axion oscillations begin. For the QCD axion $M_0\sim 10^{-10}M_\odot$, however for an axion-like particle $M_0$ can approach $M_\odot$ or higher. Using the Press-Schechter formalism we compute the mass function of halos formed by hierarchical structure formation from these seeds. We compute the concentrations and collapse times of these halos and show that they can grow to be as massive as $10^6M_0$. Within the halos, miniclusters likely remain tightly bound, and we compute their gravitational microlensing signal taking the fraction of axion dark matter collapsed into miniclusters, $f_{\rm MC}$, as a free parameter. A large value of $f_{\rm MC}$ severely weakens constraints on axion scenarios from direct detection experiments. We take into account the non-Gaussian distribution of sizes of miniclusters and determine how this effects the number of microlensing events. We develop the tools to consider microlensing by an extended mass function of non-point-like objects, and use microlensing data to place the first observational constraints on $f_{\rm MC}$. This opens a new window for the potential discovery of the axion. Comment: 27 pages, 23 figures, follow up paper to 1701.04787. v2 matches published version. Appendix added on non-Gaussian effects, discussion extended |
| Databáze: | OpenAIRE |
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