Published September 10, 2025 | Version Published
Journal Article Open

GW250114: Testing Hawking's Area Law and the Kerr Nature of Black Holes

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Abstract

The gravitational-wave signal GW250114 was observed by the two LIGO detectors with a network matched-filter signal-to-noise ratio of 80. The signal was emitted by the coalescence of two black holes with near-equal masses m= 33.6_(−0.8)^(+1.2)M⊙ and m= 32.2_(−1.3)^(+0.8)M⊙, and small spins χ1,2 ≤ 0.26 (90% credibility) and negligible eccentricity e ≤ 0.03. Postmerger data excluding the peak region are consistent with the dominant quadrupolar (ℓ = |m| = 2) mode of a Kerr black hole and its first overtone. We constrain the modes' frequencies to ±30% of the Kerr spectrum, providing a test of the remnant's Kerr nature. We also examine Hawking's area law, also known as the second law of black hole mechanics, which states that the total area of the black hole event horizons cannot decrease with time. A range of analyses that exclude up to five of the strongest merger cycles confirm that the remnant area is larger than the sum of the initial areas to high credibility.

Copyright and License

Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article’s title, journal citation, and DOI.

Acknowledgement

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 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 Investigación (AEI), the Spanish Ministerio de Ciencia, Innovación y Universidades, the European Union NextGenerationEU/PRTR (PRTR-C17.I1), the Italian Center for Super Computing–CentroNazionale di Ricerca in High Performance Computing, Big Data and Quantum Computing, funded by the European Union NextGenerationEU, the Comunitat Autonòma de les Illes Balears through the Conselleria d’Educació i Universitats, the Conselleria d’Innovació, Universitats, Ciència i Societat Digital de la Generalitat Valenciana and the CERCA Programme Generalitat de Catalunya, Spain, the Polish National Agency for Academic Exchange, the National Science Centre of Poland and the European Union–European Regional Development Fund; the Foundation for Polish Science (FNP), the Polish Ministry of Science and Higher Education, the Swiss National Science Foundation (SNSF), 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 Concertées (ARC) and Fonds Wetenschappelijk Onderzoek–Vlaanderen (FWO), Belgium, the Paris Île-de-France Region, the National Research, Development and Innovation Office of Hungary (NKFIH), the National Research Foundation of Korea, the Natural Sciences and Engineering Research Council of Canada (NSERC), the 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 Israel Science Foundation (ISF), the U.S.-Israel Binational Science Fund (BSF), 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, the 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 2402: 24103006, 24103005, and 2905: JP17H06358, JP17H06361, and JP17H06364, JSPS Core-to-Core Program A. Advanced Research Networks, JSPS Grants-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, the National Research Foundation (NRF), the Computing Infrastructure Project of the Global Science experimental Data hub Center (GSDC) at KISTI, the Korea Astronomy and Space Science Institute (KASI), the Ministry of Science and ICT (MSIT) in Korea, Academia Sinica (AS), the AS Grid Center (ASGC) and the National Science and Technology Council (NSTC) in Taiwan under grants including the Science Vanguard Research Program, the Advanced Technology Center (ATC) of NAOJ, and the Mechanical Engineering Center of KEK. Additional acknowledgements for support of individual authors may be found in [277].

Data Availability

The data that support the findings of this Letter are openly available [232], embargo periods may apply.

Supplemental Material

Additional technical details and plots

GW250114_supplement.pdf

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Additional details

Identifiers

Related works

Is new version of
Discussion Paper: arXiv:2509.08054 (arXiv)
Is supplemented by
Dataset: 10.5281/zenodo.16877102 (DOI)
Other: https://dcc.ligo.org/LIGO-M2300033/public (URL)

Funding

National Science Foundation
Science and Technology Facilities Council
Max Planck Society
Australian Research Council
Istituto Nazionale di Fisica Nucleare
Centre National de la Recherche Scientifique
Dutch Research Council
Council of Scientific and Industrial Research
Department of Science and Technology
Science and Engineering Research Board
Ministry of Human Resource Development
Agencia Estatal de Investigación
Ministerio de Ciencia, Innovación y Universidades
European Commission
PRTR-C17.I1
Conselleria de Innovación, Universidades, Ciencia y Sociedad Digital
CERCA Institution
Government of Catalonia
Narodowa Agencja Wymiany Akademickiej
National Science Center
European Commission
European Commission
Foundation for Polish Science
Ministry of Science and Higher Education
Swiss National Science Foundation
Russian Science Foundation
European Commission
Royal Society
Scottish Funding Council
Scottish Universities Physics Alliance
Institut des Origines de Lyon
Fund for Scientific Research
Research Foundation - Flanders
Conseil Régional d'Île-de-France
National Research, Development and Innovation Office
National Research Foundation of Korea
Natural Sciences and Engineering Research Council
Canada Foundation for Innovation
Ministry of Science, Technology and Innovation
ICTP South American Institute for Fundamental Research
University Grants Committee
National Natural Science Foundation of China
Israel Science Foundation
United States-Israel Binational Science Foundation
Leverhulme Trust
National Science and Technology Council
United States Department of Energy
The Kavli Foundation
Ministry of Education, Culture, Sports, Science and Technology
Japan Society for the Promotion of Science
2402: 24103006
Japan Society for the Promotion of Science
24103005
Japan Society for the Promotion of Science
2905: JP17H06358
Japan Society for the Promotion of Science
JP17H06361
Japan Society for the Promotion of Science
JP17H06364
Japan Society for the Promotion of Science
17H06133
Japan Society for the Promotion of Science
20H05639
Japan Society for the Promotion of Science
20A203: JP20H05854
Institute for Cosmic Ray Research
Korea Institute of Science & Technology Information
Korea Astronomy and Space Science Institute
Ministry of Science and ICT
Academia Sinica
National Astronomical Observatory of Japan
Vanguard International Semiconductor (Taiwan)
High Energy Accelerator Research Organization
Simons Foundation
State of Niedersachsen
Italian Center for Super Computing
Centro Nazionale di Ricerca in High Performance Computing, Big Data and Quantum Computing
Comunitat Autonòma de les Illes Balears
Conselleria d'Educació i Universitats
Hungarian Scientific Research Fund
Actions de Recherche Concertées
Research Corporation
Global Science experimental Data hub Center
AS Grid Center

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Astronomy Department, LIGO, TAPIR, Walter Burke Institute for Theoretical Physics, Division of Physics, Mathematics and Astronomy (PMA)
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