Constraints on the Cosmic Expansion History from GWTC-3

The LIGO Scientific Collaboration; Virgo Collaboration; KAGRA Collaboration

doi:10.3847/1538-4357/ac74bb

Constraints on the Cosmic Expansion History from GWTC-3

The LIGO Scientific Collaboration
, Virgo Collaboration
, KAGRA Collaboration

California Institute of Technology
Tokyo Institute of Technology
University of Salerno
INFN Sezione di Napoli
Monash University
University of Wisconsin-Milwaukee
Louisiana State University
Australian National University
Max-Planck-Institut fuer Gravitationsphysik
Leibniz Universität Hannover
Inter-University Centre for Astronomy and Astrophysics India
University of Cambridge
Friedrich-Schiller University
University of Birmingham
Northwestern University
Instituto Nacional de Pesquisas Espaciais
Cardiff University
Istituto Nazionale di Fisica Nucleare, Sezione di Pisa
Tata Institute of Fundamental Research
National Astronomical Observatory
University of Turin
INFN Sezione di Torino
University of Glasgow
University of Naples Federico II
IGFL, Université de Lyon, Université Lyon 1
University of Tokyo
Research Center for the Early Universe
University of Barcelona
Université Savoie Mont Blanc
Pompeu Fabra University (UPF)
Gran Sasso Science Institute
University of Strathclyde
and Physics University of Udine
INFN Sezione di Trieste
Embry-Riddle Aeronautical University, Prescott
Université Côte d'Azur
University of Amsterdam
University of Athens
INFN Sezione di Perugia
University of Camerino
American University
California State University Fullerton
Astroparticule and Cosmol APC
Université Paris-Saclay
European Gravitational Observatory (EGO)
College of Computing
Chennai Mathematical Institute
Hirosaki University
Columbia University
University of Portsmouth
The Graduate University for Advanced Studies
University of Urbino Carlo Bo
Istituto Nazionale di Fisica Nucleare, Sezione di Firenze
LIGO Livingston
Sezione di Roma
University of Louvain
Science Park 105
King's College London
Korea Institute of Science and Technology Information
National Institute for Mathematical Sciences
Christopher Newport University
Universiteit Utrecht
University of Oregon
Syracuse University
University of Liège
University of Milano-Bicocca
INFN Sezione di Milano-Bicocca
INAF
LIGO Hanford
University of Salerno
Massachusetts Institute of Technology
Wigner Research Centre for Physics
University of Florida
Stanford University
University of Pisa
University of Perugia
University of Padova
INFN
Bard College
Montana State University
Institute for Plasma Research
Ghent University
Nicolaus Copernicus Astronomical Center of the Polish Academy of Sciences
University of Sannio at Benevento
The University of Adelaide
The University of Texas Rio Grande Valley
California State University-Los Angeles
University of São Paulo
Sezione di Genova
The University of Western Australia
RRCAT
Missouri University of Science and Technology
Vrije Universiteit Amsterdam
Moscow State University
Center for Theoretical Physics of the Polish Academy of Sciences
Università di Trento
Trento Institute for Fundamental Physics and Applications
University of the West of Scotland
Bar-Ilan University
University of Rome
Institut FOTON-UMR6082
Indian Institute of Technology Bombay
Laboratori Nazionali del Gran Sasso
Sorbonne Université
University of Warsaw
University of Maryland, College Park
Université de Toulouse
Villanova University
Universidade de Santiago de Compostela
Stony Brook University
Flatiron Institute
NASA Goddard Space Flight Center
University of Genoa
Beijing Normal University
University of Melbourne
Dipartimento di Scienze Biomediche
INFN Sezione di Catania
University of Rome “Tor Vergata”
INFN Roma Tor Vergata
University of Valencia
Universität Hamburg
Rochester Institute of Technology
National Tsing Hua University
The Chinese University of Hong Kong
Fukuoka University
Charles Sturt University, Wagga Wagga
Tamkang University
National Central University
Academia Sinica, Institute Of Physics
INAF Osservatorio Astronomico di Padova
Swinburne University of Technology
Université Libre de Bruxelles
Universitat de les Illes Balears
Texas Tech University
University of Minnesota Twin Cities
Pennsylvania State University
University of Rhode Island
Bellevue College
Scuola Normale Superiore di Pisa
Eötvös Loránd University
Maastricht University
The University of Sheffield
University of Parma
University of Utah
Carleton College, USA
University of Zurich
Perimeter Institute for Theoretical Physics
Université de Strasbourg
West Virginia University
University of Chicago
Montclair State University
Cooperative Institute for Research in the Atmosphere
Institute of Nuclear Research ATOMKI
The University of Texas at Austin
Università degli Studi della Basilicata
Universidade de Minho
Niigata University
Osaka City University
Xiao Hong Shan
University of Szeged
Cornell University
University of British Columbia
Osservatorio Astronomico di Capodimonte
University of Mississippi
University of Michigan, Ann Arbor
Texas A&M University
Ulsan National Institute of Science and Technology
Shanghai Astronomical Observatory Chinese Academy of Sciences
University of Toyama
University of California, Berkeley
Lancaster University
Nihon University
CCLRC Rutherford Appleton Laboratory
Chungnam National University
Aoyama Gakuin University
Tsinghua University
Aristotle University of Thessaloniki
Services and Estate Management
Vanderbilt University
University of Antwerp
University of Białystok
Ewha Womans University
National Astronomical Observatories-CAS
University of Chinese Academy of Sciences
University of Southampton
Chung-Ang University
University of Washington Bothell
Institute of Applied Physics of the Russian Academy of Sciences
Inje University
Myongji University
KEK (High Energy Accelerator Research Organization)
Institute of Mathematics of the Polish Academy of Sciences
National Centre for Nuclear Research
Instituto de Fisica Teorica
Nagoya University
Université de Montréal/Polytechnique
Université de Nice
Seoul National University
Sungkyunkwan University
Université Paris Est, ENPC LIGM, IMAGINE
University of Florence
National Cheng Kung University
Wuhan University
National Applied Research Laboratories
National Taiwan Normal University
NASA Marshall Space Flight Center
CNRS
Kenyon College
Tongji University
University of Trieste
Indian Institute of Technology Madras
Saha Institute of Nuclear Physics
ISAS/JAXA
Institut des Hautes Études Scientifiques
Ryukoku University
Indian Institute of Science Education and Research Kolkata
University of Notre Dame
Ev-K2-CNR Committee
Korea Astronomy and Space Science Institute
Hobart and William Smith Colleges
The Federal University of Rio Grande do Norte
Museo Storico della Fisica e Centro Studi e Ricerche Enrico Fermi
University Roma Tre
University of Arizona
Université de Nantes
University of California, Riverside
University of Washington
Indian Institute of Technology Gandhinagar
National Institute of Technology
Universidade de Aveiro
Marquette University
Toho University
Gunma University
Chapman University
High Energy Accelerator Research Organization (KEK)
Osaka Institute of Technology
Osservatorio Astrofisico Di Arcetri
Indian Institute of Technology Hyderabad
Indian Institute of Science Education and Research (IISER)
Istituto di Astrofisica e Planetologia Spaziali
Andrews University
Tokyo City University
Kyoto University
Yukawa Institute for Theoretical Physics
Van Swinderen Institute for Particle Physics and Gravity
Vrjie Universiteit Brussel
High Energy Accelerator Research Organization (KEK)
National Defense Academy of Japan
Nagaoka University of Technology
Tata Institute of Fundamental Research, Mumbai
Technical University of Eindhoven
Sejong University
Concordia University Wisconsin
National Yang Ming Chiao Tung University
Rikkyo University

Résultats de recherche: Contribution à un journal › Article › Revue par des pairs

Résumé

We use 47 gravitational wave sources from the Third LIGO-Virgo-Kamioka Gravitational Wave Detector Gravitational Wave Transient Catalog (GWTC-3) to estimate the Hubble parameter H(z), including its current value, the Hubble constant H0. Each gravitational wave (GW) signal provides the luminosity distance to the source, and we estimate the corresponding redshift using two methods: the redshifted masses and a galaxy catalog. Using the binary black hole (BBH) redshifted masses, we simultaneously infer the source mass distribution and H(z). The source mass distribution displays a peak around 34Me, followed by a drop-off. Assuming this mass scale does not evolve with the redshift results in a H(z) measurement, yielding H0 = 68+12-8 km s-1 Mpc-1 (68% credible interval) when combined with the H0 measurement from GW170817 and its electromagnetic counterpart. This represents an improvement of 17% with respect to the H0 estimate from GWTC-1. The second method associates each GW event with its probable host galaxy in the catalog GLADE+, statistically marginalizing over the redshifts of each event's potential hosts. Assuming a fixed BBH population, we estimate a value of H0 = 68+8-6 km s-1 Mpc-1 with the galaxy catalog method, an improvement of 42% with respect to our GWTC-1 result and 20% with respect to recent H0 studies using GWTC-2 events. However, we show that this result is strongly impacted by assumptions about the BBH source mass distribution; the only event which is not strongly impacted by such assumptions (and is thus informative about H0) is the well-localized event GW190814.

langue originale	Anglais
Numéro d'article	76
journal	Astrophysical Journal
Volume	949
Numéro de publication	2
Les DOIs	https://doi.org/10.3847/1538-4357/ac74bb
état	Publié - 1 juin 2023
Modification externe	Oui

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10.3847/1538-4357/ac74bb

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@article{4bbb4f08b53049ad94bf16a2cca836f6,

title = "Constraints on the Cosmic Expansion History from GWTC-3",

abstract = "We use 47 gravitational wave sources from the Third LIGO-Virgo-Kamioka Gravitational Wave Detector Gravitational Wave Transient Catalog (GWTC-3) to estimate the Hubble parameter H(z), including its current value, the Hubble constant H0. Each gravitational wave (GW) signal provides the luminosity distance to the source, and we estimate the corresponding redshift using two methods: the redshifted masses and a galaxy catalog. Using the binary black hole (BBH) redshifted masses, we simultaneously infer the source mass distribution and H(z). The source mass distribution displays a peak around 34Me, followed by a drop-off. Assuming this mass scale does not evolve with the redshift results in a H(z) measurement, yielding H0 = 68+12-8 km s-1 Mpc-1 (68\% credible interval) when combined with the H0 measurement from GW170817 and its electromagnetic counterpart. This represents an improvement of 17\% with respect to the H0 estimate from GWTC-1. The second method associates each GW event with its probable host galaxy in the catalog GLADE+, statistically marginalizing over the redshifts of each event's potential hosts. Assuming a fixed BBH population, we estimate a value of H0 = 68+8-6 km s-1 Mpc-1 with the galaxy catalog method, an improvement of 42\% with respect to our GWTC-1 result and 20\% with respect to recent H0 studies using GWTC-2 events. However, we show that this result is strongly impacted by assumptions about the BBH source mass distribution; the only event which is not strongly impacted by such assumptions (and is thus informative about H0) is the well-localized event GW190814.",

keywords = "Gravitational wave astronomy, Gravitational wave sources, Gravitational waves",

author = "\{The LIGO Scientific Collaboration\} and \{Virgo Collaboration\} and \{KAGRA Collaboration\} and R. Abbott and H. Abe and F. Acernese and K. Ackley and N. Adhikari and Adhikari, \{R. X.\} and Adkins, \{V. K.\} and Adya, \{V. B.\} and C. Affeldt and D. Agarwal and M. Agathos and K. Agatsuma and N. Aggarwal and Aguiar, \{O. D.\} and L. Aiello and A. Ain and P. Ajith and T. Akutsu and S. Albanesi and Alfaidi, \{R. A.\} and A. Allocca and Altin, \{P. A.\} and A. Amato and C. Anand and S. Anand and A. Ananyeva and Anderson, \{S. B.\} and Anderson, \{W. G.\} and M. Ando and T. Andrade and N. Andres and M. Andres-Carcasona and T. Andric and Angelova, \{S. V.\} and S. Ansoldi and Antelis, \{J. M.\} and S. Antier and T. Apostolatos and Appavuravther, \{E. Z.\} and S. Appert and Apple, \{S. K.\} and K. Arai and A. Araya and Araya, \{M. C.\} and Areeda, \{J. S.\} and M. Arene and N. Aritomi and N. Arnaud and M. Arogeti and S. Chaty",

note = "Publisher Copyright: {\textcopyright} 2023. The Author(s).",

year = "2023",

month = jun,

day = "1",

doi = "10.3847/1538-4357/ac74bb",

language = "English",

volume = "949",

journal = "Astrophysical Journal",

issn = "0004-637X",

number = "2",

}

TY - JOUR

T1 - Constraints on the Cosmic Expansion History from GWTC-3

AU - The LIGO Scientific Collaboration

AU - Virgo Collaboration

AU - KAGRA Collaboration

AU - Abbott, R.

AU - Abe, H.

AU - Acernese, F.

AU - Ackley, K.

AU - Adhikari, N.

AU - Adhikari, R. X.

AU - Adkins, V. K.

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 - Alfaidi, R. A.

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 - Andres-Carcasona, M.

AU - Andric, T.

AU - Angelova, S. V.

AU - Ansoldi, S.

AU - Antelis, J. M.

AU - Antier, S.

AU - Apostolatos, T.

AU - Appavuravther, E. Z.

AU - Appert, S.

AU - Apple, S. K.

AU - Arai, K.

AU - Araya, A.

AU - Araya, M. C.

AU - Areeda, J. S.

AU - Arene, M.

AU - Aritomi, N.

AU - Arnaud, N.

AU - Arogeti, M.

AU - Chaty, S.

PY - 2023/6/1

Y1 - 2023/6/1

N2 - We use 47 gravitational wave sources from the Third LIGO-Virgo-Kamioka Gravitational Wave Detector Gravitational Wave Transient Catalog (GWTC-3) to estimate the Hubble parameter H(z), including its current value, the Hubble constant H0. Each gravitational wave (GW) signal provides the luminosity distance to the source, and we estimate the corresponding redshift using two methods: the redshifted masses and a galaxy catalog. Using the binary black hole (BBH) redshifted masses, we simultaneously infer the source mass distribution and H(z). The source mass distribution displays a peak around 34Me, followed by a drop-off. Assuming this mass scale does not evolve with the redshift results in a H(z) measurement, yielding H0 = 68+12-8 km s-1 Mpc-1 (68% credible interval) when combined with the H0 measurement from GW170817 and its electromagnetic counterpart. This represents an improvement of 17% with respect to the H0 estimate from GWTC-1. The second method associates each GW event with its probable host galaxy in the catalog GLADE+, statistically marginalizing over the redshifts of each event's potential hosts. Assuming a fixed BBH population, we estimate a value of H0 = 68+8-6 km s-1 Mpc-1 with the galaxy catalog method, an improvement of 42% with respect to our GWTC-1 result and 20% with respect to recent H0 studies using GWTC-2 events. However, we show that this result is strongly impacted by assumptions about the BBH source mass distribution; the only event which is not strongly impacted by such assumptions (and is thus informative about H0) is the well-localized event GW190814.

AB - We use 47 gravitational wave sources from the Third LIGO-Virgo-Kamioka Gravitational Wave Detector Gravitational Wave Transient Catalog (GWTC-3) to estimate the Hubble parameter H(z), including its current value, the Hubble constant H0. Each gravitational wave (GW) signal provides the luminosity distance to the source, and we estimate the corresponding redshift using two methods: the redshifted masses and a galaxy catalog. Using the binary black hole (BBH) redshifted masses, we simultaneously infer the source mass distribution and H(z). The source mass distribution displays a peak around 34Me, followed by a drop-off. Assuming this mass scale does not evolve with the redshift results in a H(z) measurement, yielding H0 = 68+12-8 km s-1 Mpc-1 (68% credible interval) when combined with the H0 measurement from GW170817 and its electromagnetic counterpart. This represents an improvement of 17% with respect to the H0 estimate from GWTC-1. The second method associates each GW event with its probable host galaxy in the catalog GLADE+, statistically marginalizing over the redshifts of each event's potential hosts. Assuming a fixed BBH population, we estimate a value of H0 = 68+8-6 km s-1 Mpc-1 with the galaxy catalog method, an improvement of 42% with respect to our GWTC-1 result and 20% with respect to recent H0 studies using GWTC-2 events. However, we show that this result is strongly impacted by assumptions about the BBH source mass distribution; the only event which is not strongly impacted by such assumptions (and is thus informative about H0) is the well-localized event GW190814.

KW - Gravitational wave astronomy

KW - Gravitational wave sources

KW - Gravitational waves

UR - https://www.scopus.com/pages/publications/85163895637

U2 - 10.3847/1538-4357/ac74bb

DO - 10.3847/1538-4357/ac74bb

M3 - Article

AN - SCOPUS:85163895637

SN - 0004-637X

VL - 949

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 76

ER -

Constraints on the Cosmic Expansion History from GWTC-3

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