Abstract
| Original language | English |
|---|---|
| Article number | 042001 |
| Journal | Physical Review D |
| Volume | 110 |
| Issue number | 4 |
| DOIs | |
| Publication status | Published - 15 Aug 2024 |
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In: Physical Review D, Vol. 110, No. 4, 042001, 15.08.2024.
Research output: Contribution to journal › Article › Academic › peer-review
TY - JOUR
T1 - Ultralight vector dark matter search using data from the KAGRA O3GK run
AU - Abac, A. G.
AU - Andric, T.
AU - Buonanno, A.
AU - Dax, M.
AU - Dhani, A.
AU - Dietrich, T.
AU - Estellés, H.
AU - Gair, J. R.
AU - Gamboa, A.
AU - Green, S. R.
AU - Gupte, N.
AU - Haberland, M.
AU - Maggio, E.
AU - Mehta, A. K.
AU - Ossokine, S.
AU - Pfeiffer, H. P.
AU - Pompili, L.
AU - Prudenzi, L.
AU - Ramos-Buades, A.
AU - Sänger, E. M.
AU - Varma, V.
AU - Wildberger, J. B.
AU - Abbott, R.
AU - Adhikari, R. X.
AU - Anand, S.
AU - Ananyeva, A.
AU - Anderson, S. B.
AU - Anderson, W. G.
AU - Appert, S.
AU - Arai, K.
AU - Araya, M. C.
AU - Bai, Y.
AU - Barayoga, J. C.
AU - Barish, B. C.
AU - Beroiz, M.
AU - Bhatt, R.
AU - Billingsley, G.
AU - Blackburn, J. K.
AU - Brooks, A. F.
AU - Brunett, S.
AU - Chatziioannou, K.
AU - Clark, J. A.
AU - Couvares, P.
AU - Coyne, D. C.
AU - Cullen, T. J.
AU - Davis, D.
AU - Drori, Y.
AU - Edo, T. B.
AU - Etzel, T.
AU - Feicht, J.
AU - LIGO Scientific, Virgo, and KAGRA Collaborations
AU - de Vries, Jacco
AU - Amato, Alex
AU - Danilishin, Stefan
AU - Diksha, Diksha
AU - Guo, Yuefan
AU - Hennig, Jan-Simon
AU - Hennig, Margot
AU - Hild, Stefan
AU - Iandolo, Guido Alex
AU - Koekoek, Gideon
AU - Kranzhoff, Luise
AU - Massaro, Luca
AU - Singha, Ayatri
AU - Spagnuolo, Viola
AU - Steinlechner, Jessica
AU - Steinlechner, Sebastian
AU - Utina, Andrei
AU - van den Brand, Johannes
AU - van Ranst, Zeb
AU - Vardaro, Marco
AU - Wöhler, Janis
N1 - Funding Information: This material is based upon work supported by NSF\u2019s LIGO Laboratory which is a major facility fully funded by the National Science Foundation. The authors also gratefully acknowledge the support of the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO 600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Netherlands Organization for Scientific Research (NWO), for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigaci\u00F3n (AEI), the Spanish Ministerio de Ciencia e Innovaci\u00F3n and Ministerio de Universidades, the Conselleria de Fons Europeus, Universitat i Cultura and the Direcci\u00F3 General de Pol\u00EDtica Universitaria i Recerca del Govern de les Illes Balears, the Conselleria d\u2019Innovaci\u00F3, Universitats, Ci\u00E8ncia i Societat Digital de la Generalitat Valenciana and the CERCA Programme Generalitat de Catalunya, Spain, the National Science Centre of Poland and the European Union\u2014European Regional Development Fund; Foundation for Polish Science (FNP), the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Social Funds (ESF), the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the French Lyon Institute of Origins (LIO), the Belgian Fonds de la Recherche Scientifique (FRS-FNRS), Actions de Recherche Concert\u00E9es (ARC) and Fonds Wetenschappelijk Onderzoek\u2014Vlaanderen (FWO), Belgium, the Paris \u00CEle-de-France Region, the National Research, Development and Innovation Office Hungary (NKFIH), the National Research Foundation of Korea, the Natural Science and Engineering Research Council Canada, Canadian Foundation for Innovation (CFI), the Brazilian Ministry of Science, Technology, and Innovations, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the National Science and Technology Council (NSTC), Taiwan, the United States Department of Energy, and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, INFN and CNRS for provision of computational resources. This work was supported by MEXT, JSPS Leading-edge Research Infrastructure Program, JSPS Grant-in-Aid for Specially Promoted Research 26000005, JSPS Grant-inAid for Scientific Research on Innovative Areas 2905: JP17H06358, JP17H06361 and JP17H06364, JSPS Core-to-Core Program A. Advanced Research Networks, JSPS Grant in-Aid for Scientific Research (S) 17H06133 and 20H05639, JSPS Grant-in-Aid for Transformative Research Areas (A) 20A203: JP20H05854, the joint research program of the Institute for Cosmic Ray Research, University of Tokyo, National Research Foundation (NRF), Computing Infrastructure Project of Global Science experimental Data hub Center (GSDC) at KISTI, Korea Astronomy and Space Science Institute (KASI), and Ministry of Science and ICT (MSIT) in Korea, Academia Sinica (AS), AS Grid Center (ASGC) and the National Science and Technology Council (NSTC) in Taiwan under grants including the Rising Star Program and Science Vanguard Research Program, Advanced Technology Center (ATC) of NAOJ, and Mechanical Engineering Center of KEK. Additional acknowledgements for support of individual authors may be found in the following document [45]. We request that citations to this article use \u201CA. G. Abac et al. (LIGO-Virgo-KAGRA Collaboration), \u2026\u201D or similar phrasing, depending on journal convention. Funding Information: This material is based upon work supported by NSF\u2019s LIGO Laboratory which is a major facility fully funded by the National Science Foundation. The authors also gratefully acknowledge the support of the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO 600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Netherlands Organization for Scientific Research (NWO), for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigaci\u00F3n (AEI), the Spanish Ministerio de Ciencia e Innovaci\u00F3n and Ministerio de Universidades, the Conselleria de Fons Europeus, Universitat i Cultura and the Direcci\u00F3 General de Pol\u00EDtica Universitaria i Recerca del Govern de les Illes Balears, the Conselleria d\u2019Innovaci\u00F3, Universitats, Ci\u00E8ncia i Societat Digital de la Generalitat Valenciana and the CERCA Programme Generalitat de Catalunya, Spain, the National Science Centre of Poland and the European Union\u2014European Regional Development Fund; Foundation for Polish Science (FNP), the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Social Funds (ESF), the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the French Lyon Institute of Origins (LIO), the Belgian Fonds de la Recherche Scientifique (FRS-FNRS), Actions de Recherche Concert\u00E9es (ARC) and Fonds Wetenschappelijk Onderzoek\u2014Vlaanderen (FWO), Belgium, the Paris \u00CEle-de-France Region, the National Research, Development and Innovation Office Hungary (NKFIH), the National Research Foundation of Korea, the Natural Science and Engineering Research Council Canada, Canadian Foundation for Innovation (CFI), the Brazilian Ministry of Science, Technology, and Innovations, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the National Science and Technology Council (NSTC), Taiwan, the United States Department of Energy, and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, INFN and CNRS for provision of computational resources. This work was supported by MEXT, JSPS Leading-edge Research Infrastructure Program, JSPS Grant-in-Aid for Specially Promoted Research 26000005, JSPS Grant-inAid for Scientific Research on Innovative Areas 2905: JP17H06358, JP17H06361 and JP17H06364, JSPS Core-to-Core Program A. Advanced Research Networks, JSPS Grant in-Aid for Scientific Research (S) 17H06133 and 20H05639, JSPS Grant-in-Aid for Transformative Research Areas (A) 20A203: JP20H05854, the joint research program of the Institute for Cosmic Ray Research, University of Tokyo, National Research Foundation (NRF), Computing Infrastructure Project of Global Science experimental Data hub Center (GSDC) at KISTI, Korea Astronomy and Space Science Institute (KASI), and Ministry of Science and ICT (MSIT) in Korea, Academia Sinica (AS), AS Grid Center (ASGC) and the National Science and Technology Council (NSTC) in Taiwan under grants including the Rising Star Program and Science Vanguard Research Program, Advanced Technology Center (ATC) of NAOJ, and Mechanical Engineering Center of KEK. Additional acknowledgements for support of individual authors may be found in the following document . We request that citations to this article use \u201CA.\u2009G. Abac et al. (LIGO-Virgo-KAGRA Collaboration), \u2026\u201D or similar phrasing, depending on journal convention. Publisher Copyright: © 2024 American Physical Society.
PY - 2024/8/15
Y1 - 2024/8/15
N2 - Among the various candidates for dark matter (DM), ultralight vector DM can be probed by laser interferometric gravitational wave detectors through the measurement of oscillating length changes in the arm cavities. In this context, KAGRA has a unique feature due to differing compositions of its mirrors, enhancing the signal of vector DM in the length change in the auxiliary channels. Here we present the result of a search for Formula Presented gauge boson DM using the KAGRA data from auxiliary length channels during the first joint observation run together with GEO600. By applying our search pipeline, which takes into account the stochastic nature of ultralight DM, upper bounds on the coupling strength between the Formula Presented gauge boson and ordinary matter are obtained for a range of DM masses. While our constraints are less stringent than those derived from previous experiments, this study demonstrates the applicability of our method to the lower-mass vector DM search, which is made difficult in this measurement by the short observation time compared to the auto-correlation timescale of DM.
AB - Among the various candidates for dark matter (DM), ultralight vector DM can be probed by laser interferometric gravitational wave detectors through the measurement of oscillating length changes in the arm cavities. In this context, KAGRA has a unique feature due to differing compositions of its mirrors, enhancing the signal of vector DM in the length change in the auxiliary channels. Here we present the result of a search for Formula Presented gauge boson DM using the KAGRA data from auxiliary length channels during the first joint observation run together with GEO600. By applying our search pipeline, which takes into account the stochastic nature of ultralight DM, upper bounds on the coupling strength between the Formula Presented gauge boson and ordinary matter are obtained for a range of DM masses. While our constraints are less stringent than those derived from previous experiments, this study demonstrates the applicability of our method to the lower-mass vector DM search, which is made difficult in this measurement by the short observation time compared to the auto-correlation timescale of DM.
U2 - 10.1103/PhysRevD.110.042001
DO - 10.1103/PhysRevD.110.042001
M3 - Article
SN - 1550-7998
VL - 110
JO - Physical Review D
JF - Physical Review D
IS - 4
M1 - 042001
ER -