Ultra Light Axionic Dark Matter: Galactic Halos and Implications for Observations with Pulsar Timing Arrays
dc.contributor.author | De Martino, Ivan | |
dc.contributor.author | Broadhurst, Thomas | |
dc.contributor.author | Tye, S. H. Henry | |
dc.contributor.author | Chiueh, Tzihong | |
dc.contributor.author | Schive, Hsi-Yu | |
dc.contributor.author | Lazcoz Sáez, Ruth | |
dc.date.accessioned | 2018-11-09T13:45:24Z | |
dc.date.available | 2018-11-09T13:45:24Z | |
dc.date.issued | 2018-01-16 | |
dc.identifier.citation | Galaxies 6 : (2018) // Article ID UNSP 10 | es_ES |
dc.identifier.issn | 2075-4434 | |
dc.identifier.uri | http://hdl.handle.net/10810/29593 | |
dc.description.abstract | The cold dark matter (CDM) paradigm successfully explains the cosmic structure over an enormous span of redshifts. However, it fails when probing the innermost regions of dark matter halos and the properties of the Milky Way’s dwarf galaxy satellites. Moreover, the lack of experimental detection of Weakly Interacting Massive Particle (WIMP) favors alternative candidates such as light axionic dark matter that naturally arise in string theory. Cosmological N-body simulations have shown that axionic dark matter forms a solitonic core of size of ≃150 pc in the innermost region of the galactic halos. The oscillating scalar field associated to the axionic dark matter halo produces an oscillating gravitational potential that induces a time dilation of the pulse arrival time of ≃400 ns/(m B /10 −22 eV) for pulsar within such a solitonic core. Over the whole galaxy, the averaged predicted signal may be detectable with current and forthcoming pulsar timing array telescopes. | es_ES |
dc.description.sponsorship | IDM acknowledges financial support from University of the Basque Country UPV/EHU under the program "Convocatoria de contratacion para la especializacion de personal investigador doctor en la UPV/EHU 2015", from the Spanish Ministerio de Economia y Competitividad through research project FIS2010-15492, and from the Basque Government through research project IT-956-16. RL is supported by the Spanish Ministry of Economy and Competitiveness through research projects FIS2010-15492 and Consolider EPI CSD2010-00064, and by the University of the Basque Country UPV/EHU under program UFI 11/55. IDM and RL also acknowledge support from the COST Action CA1511 Cosmology and Astrophysics Network for Theoretical Advances and Training Actions (CANTATA). TJB acknowledges generous hospitality from the Institute for Advanced Studies in Hong Kong and helpful conversations with Nick Kaiser and Kfir Blum. SHHT is supported by CRF Grant HKUST4/CRF/13G and GRF 16305414 issued by the Research Grants Council (RGC) of the Government of the Hong Kong SAR. Chipbond Technology Corporation is acknowledged for donating the GPU cluster with which this work was conducted. This work was supported in part by the National Science Council of Taiwan under grants NSC100-2112-M-002-018-MY3 and NSC99-2112-M-002-009-MY3 | es_ES |
dc.language.iso | eng | es_ES |
dc.publisher | MDPI | es_ES |
dc.relation | info:eu-repo/grantAgreement/MINECO/(FIS2010-15492)(EPI CSD2010-00064) | es_ES |
dc.rights | info:eu-repo/semantics/openAccess | es_ES |
dc.rights.uri | http://creativecommons.org/licenses/by/3.0/es/ | * |
dc.subject | dark matter | es_ES |
dc.subject | axions | es_ES |
dc.subject | particle physics | es_ES |
dc.subject | general relativity | es_ES |
dc.subject | pulsars | es_ES |
dc.subject | SKA | es_ES |
dc.subject | onstraining F(R) gravity | es_ES |
dc.subject | invisible axion | es_ES |
dc.subject | scale | es_ES |
dc.subject | field | es_ES |
dc.subject | wave | es_ES |
dc.subject | modulation | es_ES |
dc.subject | cosmology | es_ES |
dc.subject | CDM | es_ES |
dc.title | Ultra Light Axionic Dark Matter: Galactic Halos and Implications for Observations with Pulsar Timing Arrays | es_ES |
dc.type | info:eu-repo/semantics/article | es_ES |
dc.rights.holder | C 2017 by the authors. Licensee MDPI, Basel, Switzerland. This article is an open access article distributed under the terms and conditions of the Creative Commons Attribution (CC BY) license (http://creativecommons.org/licenses/by/4.0/). | es_ES |
dc.rights.holder | Atribución 3.0 España | * |
dc.relation.publisherversion | https://www.mdpi.com/2075-4434/6/1/10 | es_ES |
dc.identifier.doi | 10.3390/galaxies6010010 | |
dc.departamentoes | Física teórica e historia de la ciencia | es_ES |
dc.departamentoeu | Fisika teorikoa eta zientziaren historia | es_ES |
Files in this item
This item appears in the following Collection(s)
Except where otherwise noted, this item's license is described as C 2017 by the authors. Licensee MDPI, Basel, Switzerland. This article is an open access
article distributed under the terms and conditions of the Creative Commons Attribution
(CC BY) license (http://creativecommons.org/licenses/by/4.0/).