Details
| Original language | English |
|---|---|
| Article number | A84 |
| Journal | Astronomy and Astrophysics |
| Volume | 659 |
| Publication status | Published - 16 Mar 2022 |
Abstract
Keywords
- Black hole physics, Gravitational waves, Stars: black holes
ASJC Scopus subject areas
- Physics and Astronomy(all)
- Astronomy and Astrophysics
- Earth and Planetary Sciences(all)
- Space and Planetary Science
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In: Astronomy and Astrophysics, Vol. 659, A84, 16.03.2022.
Research output: Contribution to journal › Article › Research › peer review
}
TY - JOUR
T1 - Search for intermediate-mass black hole binaries in the third observing run of Advanced LIGO and Advanced Virgo
AU - The Virgo Collaboration
AU - The Virgo Collaboration
AU - Abbott, R.
AU - Abbott, T. D.
AU - Acernese, F.
AU - Ackley, K.
AU - Adams, C.
AU - Adhikari, N.
AU - Adhikari, R. X.
AU - Adya, V. B.
AU - Affeldt, C.
AU - Agarwal, D.
AU - Agathos, M.
AU - Agatsuma, K.
AU - Aggarwal, N.
AU - Aguiar, O. D.
AU - Aiello, L.
AU - Ain, A.
AU - Ajith, P.
AU - Akutsu, T.
AU - Albanesi, S.
AU - Allocca, A.
AU - Altin, P. A.
AU - Amato, A.
AU - Anand, C.
AU - Anand, S.
AU - Ananyeva, A.
AU - Anderson, S. B.
AU - Anderson, W. G.
AU - Ando, M.
AU - Andrade, T.
AU - Andres, N.
AU - Andrić, T.
AU - Angelova, S. V.
AU - Ansoldi, S.
AU - Antelis, J. M.
AU - Antier, S.
AU - Appert, S.
AU - Danilishin, S.
AU - Danzmann, K.
AU - Heurs, M.
AU - Hreibi, A.
AU - Isleif, K.
AU - Junker, J.
AU - Lück, H.
AU - Matiushechkina, M.
AU - Nery, M.
AU - Schulte, B. W.
AU - Vahlbruch, H.
AU - Wilken, D.
AU - Willke, B.
AU - Wu, D. S.
AU - Bergamin, Fabio
AU - Bisht, Aparna
AU - Bode, Nina
AU - Booker, Phillip
AU - Brinkmann, Marc
AU - Gohlke, N.
AU - Heidt, A.
AU - Heinze, J.
AU - Hochheim, S.
AU - Kastaun, Wolfgang
AU - Kirchhoff, R.
AU - Koch, Patrick
AU - Koper, N.
AU - Kringel, Volker
AU - Krishnendu, N. V.
AU - Kühn, Gerrit
AU - Leavey, S.
AU - Lehmann, J.
AU - Liu, J.
AU - Lough, James
AU - Mehmet, Moritz
AU - Meylahn, Fabian
AU - Mukund, Nikhil
AU - Nadji, S. L.
AU - Ohme, F.
AU - Schneewind, M.
AU - Schutz, B. F.
AU - Venneberg, J.
AU - von Wrangel, J.
AU - Weinert, Michael
AU - Wellmann, F.
AU - Weßels, Peter
AU - Winkler, W.
AU - Woehler, J.
N1 - Funding Information: Acknowledgements. This material is based upon work supported by NSF’s 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 GEO600 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, 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 Investigación, the Vicepresidència i Conselleria d’Innovació, Recerca i Tur-isme and the Conselleria d’Educació i Universitat del Govern de les Illes Balears, the Conselleria d’Innovació, Universitats, Ciència i Societat Digital de la Gener-alitat Valenciana and the CERCA Programme Generalitat de Catalunya, Spain, the National Science Centre of Poland and the 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 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 Concertées (ARC) and Fonds Wetenschappelijk Onderzoek – Vlaan-deren (FWO), Belgium, the Paris Île-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 Ministry of Science and Technology (MOST), 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-in-Aid 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, the joint research program of the Institute for Cosmic Ray Research, University of Tokyo, National Research Foundation (NRF) and Computing Infrastructure Project of KISTI-GSDC in Korea, Academia Sinica (AS), AS Grid Center (ASGC) and the Ministry of Science and Technology (MoST) in Taiwan under grants including AS-CDA-105-M06, Advanced Technology Center (ATC) of NAOJ, and Mechanical Engineering Center of KEK. We would like to thank all of the essential workers who put their health at risk during the COVID-19 pandemic, without whom we would not have been able to complete this work.
PY - 2022/3/16
Y1 - 2022/3/16
N2 - Intermediate-mass black holes (IMBHs) span the approximate mass range 100-10(5)x2006;M-circle dot, between black holes (BHs) that formed by stellar collapse and the supermassive BHs at the centers of galaxies. Mergers of IMBH binaries are the most energetic gravitational-wave sources accessible by the terrestrial detector network. Searches of the first two observing runs of Advanced LIGO and Advanced Virgo did not yield any significant IMBH binary signals. In the third observing run (O3), the increased network sensitivity enabled the detection of GW190521, a signal consistent with a binary merger of mass similar to 150 x2006;M-circle dot providing direct evidence of IMBH formation. Here, we report on a dedicated search of O3 data for further IMBH binary mergers, combining both modeled (matched filter) and model-independent search methods. We find some marginal candidates, but none are sufficiently significant to indicate detection of further IMBH mergers. We quantify the sensitivity of the individual search methods and of the combined search using a suite of IMBH binary signals obtained via numerical relativity, including the effects of spins misaligned with the binary orbital axis, and present the resulting upper limits on astrophysical merger rates. Our most stringent limit is for equal mass and aligned spin BH binary of total mass 200 x2006;M-circle dot and effective aligned spin 0.8 at 0.056 Gpc(-3) yr(-1) (90, a factor of 3.5 more constraining than previous LIGO-Virgo limits. We also update the estimated rate of mergers similar to GW190521 to 0.08 Gpc(-3) yr(-1).
AB - Intermediate-mass black holes (IMBHs) span the approximate mass range 100-10(5)x2006;M-circle dot, between black holes (BHs) that formed by stellar collapse and the supermassive BHs at the centers of galaxies. Mergers of IMBH binaries are the most energetic gravitational-wave sources accessible by the terrestrial detector network. Searches of the first two observing runs of Advanced LIGO and Advanced Virgo did not yield any significant IMBH binary signals. In the third observing run (O3), the increased network sensitivity enabled the detection of GW190521, a signal consistent with a binary merger of mass similar to 150 x2006;M-circle dot providing direct evidence of IMBH formation. Here, we report on a dedicated search of O3 data for further IMBH binary mergers, combining both modeled (matched filter) and model-independent search methods. We find some marginal candidates, but none are sufficiently significant to indicate detection of further IMBH mergers. We quantify the sensitivity of the individual search methods and of the combined search using a suite of IMBH binary signals obtained via numerical relativity, including the effects of spins misaligned with the binary orbital axis, and present the resulting upper limits on astrophysical merger rates. Our most stringent limit is for equal mass and aligned spin BH binary of total mass 200 x2006;M-circle dot and effective aligned spin 0.8 at 0.056 Gpc(-3) yr(-1) (90, a factor of 3.5 more constraining than previous LIGO-Virgo limits. We also update the estimated rate of mergers similar to GW190521 to 0.08 Gpc(-3) yr(-1).
KW - Black hole physics
KW - Gravitational waves
KW - Stars: black holes
UR - http://www.scopus.com/inward/record.url?scp=85127131576&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202141452
DO - 10.1051/0004-6361/202141452
M3 - Article
VL - 659
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 0004-6361
M1 - A84
ER -