dc.contributor.author | Fujikura, Kohei | |
dc.contributor.author | Hertzberg, Mark P. | |
dc.contributor.author | Schiappacasse, Enrico D. | |
dc.contributor.author | Yamaguchi, Masahide | |
dc.date.accessioned | 2022-01-10T14:21:58Z | |
dc.date.available | 2022-01-10T14:21:58Z | |
dc.date.issued | 2021 | |
dc.identifier.citation | Fujikura, K., Hertzberg, M. P., Schiappacasse, E. D., & Yamaguchi, M. (2021). Microlensing constraints on axion stars including finite lens and source size effects. <i>Physical Review D</i>, <i>104</i>(12), Article 123012. <a href="https://doi.org/10.1103/PhysRevD.104.123012" target="_blank">https://doi.org/10.1103/PhysRevD.104.123012</a> | |
dc.identifier.other | CONVID_103777778 | |
dc.identifier.uri | https://jyx.jyu.fi/handle/123456789/79268 | |
dc.description.abstract | A fraction of light scalar dark matter, especially axions, may organize into Bose-Einstein condensates, gravitationally bound clumps, “boson stars”, and be present in large number in galactic halos today. We compute the expected number of gravitational microlensing events of clumps composed of the ordinary QCD axion and axionlike particles and derive microlensing constraints from the EROS-2 survey and the Subaru Hyper Suprime-Cam observation. We perform a detailed lensing calculation, including the finite lens and source size effects in our analysis. We constrain the axion mass in terms of the fraction of dark matter collapsed into clumps, the individual clump densities, and the axion self-coupling. We also consider and constrain clumps composed of a generic scalar dark matter candidate with repulsive self-interactions. Our analysis opens up a new window for the potential discovery of dark matter. | en |
dc.format.mimetype | application/pdf | |
dc.language.iso | eng | |
dc.publisher | American Physical Society (APS) | |
dc.relation.ispartofseries | Physical Review D | |
dc.rights | CC BY 4.0 | |
dc.title | Microlensing constraints on axion stars including finite lens and source size effects | |
dc.type | article | |
dc.identifier.urn | URN:NBN:fi:jyu-202201101046 | |
dc.contributor.laitos | Fysiikan laitos | fi |
dc.contributor.laitos | Department of Physics | en |
dc.type.uri | http://purl.org/eprint/type/JournalArticle | |
dc.type.coar | http://purl.org/coar/resource_type/c_2df8fbb1 | |
dc.description.reviewstatus | peerReviewed | |
dc.relation.issn | 2470-0010 | |
dc.relation.numberinseries | 12 | |
dc.relation.volume | 104 | |
dc.type.version | publishedVersion | |
dc.rights.copyright | © 2021 American Physical Society | |
dc.rights.accesslevel | openAccess | fi |
dc.relation.grantnumber | 318319 | |
dc.subject.yso | kosmologia | |
dc.subject.yso | pimeä aine | |
dc.format.content | fulltext | |
jyx.subject.uri | http://www.yso.fi/onto/yso/p7160 | |
jyx.subject.uri | http://www.yso.fi/onto/yso/p14101 | |
dc.rights.url | https://creativecommons.org/licenses/by/4.0/ | |
dc.relation.doi | 10.1103/PhysRevD.104.123012 | |
dc.relation.funder | Research Council of Finland | en |
dc.relation.funder | Suomen Akatemia | fi |
jyx.fundingprogram | Academy Project, AoF | en |
jyx.fundingprogram | Akatemiahanke, SA | fi |
jyx.fundinginformation | This work was supported by the Academy of Finland Grant No. 318319. K. F. is supported by JSPS Grant-in-Aid for Research Fellows Grant No. 20J12415. M. P. H. is supported in part by National Science Foundation Grant No. PHY-2013953. M. P. H. and M. Y. thank the JSPS invitation fellowship. M. Y. is supported in part by JSPS Grant-in-Aid for Scientific Research Grants No. JP18K18764, No. JP21H01080, and No. JP21H00069. | |
dc.type.okm | A1 | |