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Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo

Abbott, B. P. and Abbott, R. and Adhikari, R. X. and Anand, S. and Ananyeva, A. and Anderson, S. B. and Appert, S. and Arai, K. and Araya, M. C. and Barayoga, J. C. and Barish, B. C. and Billingsley, G. and Biscans, S and Blackburn, J. K. and Bork, R. and Brooks, A. F. and Brunett, S. and Cahillane, C. and Callister, T. A. and Coughlin, M. W. and Couvares, P. and Coyne, D. C. and Ehrens, P. and Eichholz, J. and Etzel, T. and Feicht, J. and Gossan, S. E. and Grassia, P. and Gustafson, E. K. and Heptonstall, A. W. and Hulko, M. and Isi, M. and Kamai, B. and Kanner, J. B. and Kasprzack, M. and Kondrashov, V. and Korth, W. Z. and Kozak, D. B. and Lazzarini, A. and Lo, R. K. L. and Maros, E. and Markowitz, A. and Massinger, T. J. and Matichard, F. and McIver, J. and Meshkov, S. and Pedraza, M. and Quintero, E. A. and Reitze, D. H. and Richardson, J. W. and Robertson, N. A. and Rollins, J. G. and Sanchez, E. J. and Sanchez, L. E. and Sun, L. and Taylor, R. and Torrie, C. I. and Trudeau, R. and Vajente, G. and Vass, S. and Venugopalan, G. and Wade, A. R. and Wallace, L. and Weinstein, A. J. and Willis, J. L. and Wipf, C. C. and Xiao, S. and Yamamoto, H. and Zhang, L. and Zucker, M. E. and Zweizig, J. and Barkett, K. and Chen, Y. and Li, X. and Ma, Y. and Pang, B. and Scheel, M. and Tso, R. and Varma, V. (2019) Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo. Astrophysical Journal Letters, 882 (2). Art. No. L24. ISSN 2041-8213. https://resolver.caltech.edu/CaltechAUTHORS:20190910-090330995

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Abstract

We present results on the mass, spin, and redshift distributions of the ten binary black hole mergers detected in the first and second observing runs completed by Advanced LIGO and Advanced Virgo. We constrain properties of the binary black hole (BBH) mass spectrum using models with a range of parameterizations of the BBH mass and spin distributions. We find that the mass distribution of the more massive black hole in such binaries is well approximated by models with no more than 1% of black holes more massive than 45M⊙, and a power law index of α=1.6^(+1.5)_(−1.7) (90% credibility). We also show that BBHs are unlikely to be composed of black holes with large spins aligned to the orbital angular momentum. Modelling the evolution of the BBH merger rate with redshift, we show that it is flat or increasing with redshift with 88% probability. Marginalizing over uncertainties in the BBH population, we find robust estimates of the BBH merger rate density of R=53.2^(+58.5)_(−28.8) Gpc^(-3) yr^(-1) (90% credibility). As the BBH catalog grows in future observing runs, we expect that uncertainties in the population model parameters will shrink, potentially providing insights into the formation of black holes via supernovae, binary interactions of massive stars, stellar cluster dynamics, and the formation history of black holes across cosmic time.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/2041-8213/ab3800DOIArticle
https://arxiv.org/abs/1811.12940arXivDiscussion Paper
ORCID:
AuthorORCID
Adhikari, R. X.0000-0002-5731-5076
Arai, K.0000-0001-8916-8915
Billingsley, G.0000-0002-4141-2744
Callister, T. A.0000-0001-9892-177X
Coughlin, M. W.0000-0002-8262-2924
Isi, M.0000-0001-8830-8672
Kamai, B.0000-0001-6521-9351
Kanner, J. B.0000-0001-8115-0577
Korth, W. Z.0000-0003-3527-1348
Kozak, D. B.0000-0003-3118-8950
Massinger, T. J.0000-0002-3429-5025
Sun, L.0000-0001-7959-892X
Weinstein, A. J.0000-0002-0928-6784
Zucker, M. E.0000-0002-2544-1596
Zweizig, J.0000-0002-1521-3397
Ma, Y.0000-0001-7192-4874
Pang, B.0000-0002-5697-2162
Additional Information:© 2019 The American Astronomical Society. Received 2018 December 15; revised 2019 July 11; accepted 2019 July 21; published 2019 September 9. The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as 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 Foundation for Fundamental Research on Matter supported by the Netherlands Organisation 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 Turisme and the Conselleria d'Educació i Universitat del Govern de les Illes Balears, the Conselleria d'Educació Investigació Cultura i Esport de la Generalitat Valenciana, the National Science Centre of Poland, 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 Lyon Institute of Origins (LIO), the Paris Île-de-France Region, the National Research, Development and Innovation Office Hungary (NKFIH), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the Natural Science and Engineering Research Council Canada, the Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, Innovations, and Communications, 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, and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS, and the State of Niedersachsen/Germany for provision of computational resources.
Group:LIGO
Funders:
Funding AgencyGrant Number
NSFUNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
Max-Planck-SocietyUNSPECIFIED
State of Niedersachsen/GermanyUNSPECIFIED
Australian Research CouncilUNSPECIFIED
Istituto Nazionale di Fisica Nucleare (INFN)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Stichting voor Fundamenteel Onderzoek der Materie (FOM)UNSPECIFIED
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)UNSPECIFIED
Council of Scientific and Industrial Research (India)UNSPECIFIED
Department of Science and Technology (India)UNSPECIFIED
Science and Engineering Research Board (SERB)UNSPECIFIED
Ministry of Human Resource Development (India)UNSPECIFIED
Agencia Estatal de InvestigaciónUNSPECIFIED
Vicepresidència i Conselleria d'Innovació, Recerca i TurismeUNSPECIFIED
Conselleria d'Educació i Universitat del Govern de les Illes BalearsUNSPECIFIED
Conselleria d'Educació, Investigació, Cultura i Esport de la Generalitat ValencianaUNSPECIFIED
National Science Centre (Poland)UNSPECIFIED
Swiss National Science Foundation (SNSF)UNSPECIFIED
Russian Foundation for Basic ResearchUNSPECIFIED
Russian Science FoundationUNSPECIFIED
European CommissionUNSPECIFIED
European Regional Development Funds (ERDF)UNSPECIFIED
Royal SocietyUNSPECIFIED
Scottish Funding CouncilUNSPECIFIED
Scottish Universities Physics AllianceUNSPECIFIED
Hungarian Scientific Research Fund (OTKA)UNSPECIFIED
Lyon Institute of Origins (LIO)UNSPECIFIED
Paris Île-de-France RegionUNSPECIFIED
National Research, Development and Innovation Office (Hungary)UNSPECIFIED
National Research Foundation of KoreaUNSPECIFIED
Industry CanadaUNSPECIFIED
Ontario Ministry of Economic Development and InnovationUNSPECIFIED
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Canadian Institute for Advanced Research (CIFAR)UNSPECIFIED
Ministério da Ciência, Tecnologia, Inovações e Comunicações (MCTIC)UNSPECIFIED
International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR)UNSPECIFIED
Research Grants Council of Hong KongUNSPECIFIED
National Natural Science Foundation of ChinaUNSPECIFIED
Leverhulme TrustUNSPECIFIED
Research CorporationUNSPECIFIED
Ministry of Science and Technology (Taipei)UNSPECIFIED
Kavli FoundationUNSPECIFIED
Subject Keywords:black holes – gravitational waves – statistical
Issue or Number:2
Record Number:CaltechAUTHORS:20190910-090330995
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190910-090330995
Official Citation:B. P. Abbott et al 2019 ApJL 882 L24
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:98537
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:10 Sep 2019 16:34
Last Modified:03 Oct 2019 21:42

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