000125973 001__ 125973 000125973 005__ 20241125101137.0 000125973 0247_ $$2doi$$a10.1103/PhysRevD.107.083510 000125973 0248_ $$2sideral$$a133522 000125973 037__ $$aART-2023-133522 000125973 041__ $$aeng 000125973 100__ $$aEggemeier, B. 000125973 245__ $$aAxion minivoids and implications for direct detection 000125973 260__ $$c2023 000125973 5060_ $$aAccess copy available to the general public$$fUnrestricted 000125973 5203_ $$aIn the scenario in which QCD axion dark matter is produced after inflation, the Universe is populated by large inhomogeneities on very small scales. Eventually, these fluctuations will collapse gravitationally to form dense axion miniclusters that trap up to ∼75% of the dark matter within asteroid-mass clumps. Axion miniclusters are physically tiny however, so haloscope experiments searching for axions directly on Earth are much more likely to be probing “minivoids”—the space in between miniclusters. This scenario seems like it ought to spell doom for haloscopes, but while these minivoids might be underdense, they are not totally devoid of axions. Using Schrödinger-Poisson and N-body simulations to evolve from realistic initial field configurations, we quantify the extent to which the local ambient dark matter density is suppressed in the postinflationary scenario. We find that a typical experimental measurement will sample an axion density that is only around 10% of the expected galactic dark matter density. Our results are taken as conservative estimates and have implications for experimental campaigns lasting longer than a few years, as well as broadband haloscopes that have sensitivity to transient signatures. We show that for a Oð(year)-long integration times, the measured dark matter density should be expected to vary by 20%–30%. 000125973 536__ $$9info:eu-repo/grantAgreement/ES/AEI-FEDER/PGC2018-095328-B-I00$$9info:eu-repo/grantAgreement/ES/DGA/E12-7R$$9info:eu-repo/grantAgreement/EC/H2020/674896/EU/The Elusives Enterprise: Asymmetries of the Invisible Universe/ELUSIVES$$9This project has received funding from the European Union’s Horizon 2020 research and innovation program under grant agreement No H2020 674896-ELUSIVES 000125973 540__ $$9info:eu-repo/semantics/openAccess$$aby$$uhttp://creativecommons.org/licenses/by/3.0/es/ 000125973 590__ $$a4.6$$b2023 000125973 592__ $$a1.587$$b2023 000125973 591__ $$aPHYSICS, PARTICLES & FIELDS$$b7 / 31 = 0.226$$c2023$$dQ1$$eT1 000125973 593__ $$aPhysics and Astronomy (miscellaneous)$$c2023$$dQ1 000125973 591__ $$aASTRONOMY & ASTROPHYSICS$$b17 / 84 = 0.202$$c2023$$dQ1$$eT1 000125973 593__ $$aNuclear and High Energy Physics$$c2023$$dQ1 000125973 594__ $$a9.3$$b2023 000125973 655_4 $$ainfo:eu-repo/semantics/article$$vinfo:eu-repo/semantics/publishedVersion 000125973 700__ $$aO’Hare, C. A. J. 000125973 700__ $$aPierobon, G. 000125973 700__ $$0(orcid)0000-0002-1044-8197$$aRedondo, J.$$uUniversidad de Zaragoza 000125973 700__ $$aWong, Y. Y. Y. 000125973 7102_ $$12004$$2405$$aUniversidad de Zaragoza$$bDpto. Física Teórica$$cÁrea Física Teórica 000125973 773__ $$g107, 8 (2023), 083510 [18 pp.]$$pPhys. rev. D$$tPhysical Review D$$x2470-0010 000125973 8564_ $$s2376309$$uhttps://zaguan.unizar.es/record/125973/files/texto_completo.pdf$$yVersión publicada 000125973 8564_ $$s2850003$$uhttps://zaguan.unizar.es/record/125973/files/texto_completo.jpg?subformat=icon$$xicon$$yVersión publicada 000125973 909CO $$ooai:zaguan.unizar.es:125973$$particulos$$pdriver 000125973 951__ $$a2024-11-22-12:01:19 000125973 980__ $$aARTICLE