GWTC-4.0: An Introduction to Version 4.0 of the Gravitational-Wave Transient Catalog - IOPscience

GWTC-4.0: An Introduction to Version 4.0 of the Gravitational-Wave Transient Catalog - IOPscience
The American Astronomical Society (AAS)
, established in 1899 and based in Washington, DC, is the major organization of professional astronomers in North America. Its membership of about 7,000 individuals also includes physicists, mathematicians, geologists, engineers, and others whose research and educational interests lie within the broad spectrum of subjects comprising contemporary astronomy. The mission of the AAS is to enhance and share humanity's scientific understanding of the universe.
The following article is
Open access
GWTC-4.0: An Introduction to Version 4.0 of the Gravitational-Wave Transient Catalog
A. G. Abac
I. Abouelfettouh
F. Acernese
K. Ackley
S. Adhicary
D. Adhikari
N. Adhikari
R. X. Adhikari
V. K. Adkins
S. Afroz
Published 2025 December 9
© 2025. The Author(s). Published by the American Astronomical Society.
The Astrophysical Journal Letters
Number 1
Citation
A. G. Abac
et al
2025
ApJL
995
L18
DOI
10.3847/2041-8213/ae0c06
Article
PDF
Article
ePub
You need an eReader or compatible software to experience
the benefits of the ePub3 file format
A. G. Abac
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
I. Abouelfettouh
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
F. Acernese
AFFILIATIONS
Dipartimento di Farmacia, Università di Salerno, I-84084 Fisciano, Salerno, Italy
INFN, Sezione di Napoli, I-80126 Napoli, Italy
K. Ackley
AFFILIATIONS
University of Warwick, Coventry CV 4 7AL, UK
S. Adhicary
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
D. Adhikari
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
N. Adhikari
AFFILIATIONS
University of Wisconsin–Milwaukee, Milwaukee, WI 53201, USA
R. X. Adhikari
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
V. K. Adkins
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
S. Afroz
AFFILIATIONS
Tata Institute of Fundamental Research, Mumbai 400005, India
D. Agarwal
AFFILIATIONS
Université catholique de Louvain, B-1348 Louvain-la-Neuve, Belgium
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
M. Agathos
AFFILIATIONS
Queen Mary University of London, London E1 4NS, UK
M. Aghaei Abchouyeh
AFFILIATIONS
Department of Physics and Astronomy, Sejong University, 209 Neungdong-ro, Gwangjin-gu, Seoul 143-747, Republic of Korea
O. D. Aguiar
AFFILIATIONS
Instituto Nacional de Pesquisas Espaciais, 12227-010 São José dos Campos, São Paulo, Brazil
S. Ahmadzadeh
AFFILIATIONS
SUPA, University of the West of Scotland, Paisley PA1 2BE, UK
L. Aiello
AFFILIATIONS
Università di Roma Tor Vergata, I-00133 Roma, Italy
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
A. Ain
AFFILIATIONS
Universiteit Antwerpen, 2000 Antwerpen, Belgium
P. Ajith
AFFILIATIONS
International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bengaluru 560089, India
S. Akcay
AFFILIATIONS
University College Dublin, Belfield, Dublin 4, Ireland
T. Akutsu
AFFILIATIONS
Gravitational Wave Science Project, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan
Advanced Technology Center, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan
S. Albanesi
AFFILIATIONS
Theoretisch-Physikalisches Institut, Friedrich-Schiller-Universität Jena, D-07743 Jena, Germany
INFN Sezione di Torino, I-10125 Torino, Italy
R. A. Alfaidi
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
A. Al-Jodah
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
C. Alléné
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
A. Allocca
AFFILIATIONS
INFN, Sezione di Napoli, I-80126 Napoli, Italy
Università di Napoli “Federico II,” I-80126 Napoli, Italy
S. Al-Shammari
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
P. A. Altin
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
S. Alvarez-Lopez
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
O. Amarasinghe
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
A. Amato
AFFILIATIONS
Maastricht University, 6200 MD Maastricht, The Netherlands
Nikhef, 1098 XG Amsterdam, The Netherlands
C. Amra
AFFILIATIONS
Aix Marseille Univ, CNRS, Centrale Med, Institut Fresnel, F-13013 Marseille, France
A. Ananyeva
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
S. B. Anderson
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
W. G. Anderson
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
M. Andia
AFFILIATIONS
Université Paris-Saclay, CNRS/IN2P3, IJCLab, 91405 Orsay, France
M. Ando
AFFILIATIONS
Department of Physics, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
University of Tokyo, Tokyo, 113-0033, Japan
T. Andrade
AFFILIATIONS
Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (UB), c. Martí i Franquès, 1, 08028 Barcelona, Spain
M. Andrés-Carcasona
AFFILIATIONS
Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra (Barcelona), Spain
T. Andrić
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
J. Anglin
AFFILIATIONS
University of Florida, Gainesville, FL 32611, USA
S. Ansoldi
AFFILIATIONS
Dipartimento di Scienze Matematiche, Informatiche e Fisiche, Università di Udine, I-33100 Udine, Italy
INFN, Sezione di Trieste, I-34127 Trieste, Italy
J. M. Antelis
AFFILIATIONS
Tecnologico de Monterrey, Escuela de Ingeniería y Ciencias, Monterrey 64849, Mexico
S. Antier
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
M. Aoumi
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
E. Z. Appavuravther
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
Università di Camerino, I-62032 Camerino, Italy
S. Appert
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
S. K. Apple
AFFILIATIONS
University of Washington, Seattle, WA 98195, USA
K. Arai
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
A. Araya
AFFILIATIONS
Earthquake Research Institute, The University of Tokyo, 1-1-1 Yayoi, Bunkyo-ku, Tokyo 113-0032, Japan
M. C. Araya
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
M. Arca Sedda
AFFILIATIONS
Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
J. S. Areeda
AFFILIATIONS
California State University Fullerton, Fullerton, CA 92831, USA
L. Argianas
AFFILIATIONS
Villanova University, Villanova, PA 19085, USA
N. Aritomi
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
F. Armato
AFFILIATIONS
INFN, Sezione di Genova, I-16146 Genova, Italy
Dipartimento di Fisica, Università degli Studi di Genova, I-16146 Genova, Italy
S. Armstrong
AFFILIATIONS
SUPA, University of Strathclyde, Glasgow G1 1XQ, UK
N. Arnaud
AFFILIATIONS
Université Paris-Saclay, CNRS/IN2P3, IJCLab, 91405 Orsay, France
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
M. Arogeti
AFFILIATIONS
Georgia Institute of Technology, Atlanta, GA 30332, USA
S. M. Aronson
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
G. Ashton
AFFILIATIONS
Royal Holloway, University of London, London TW20 0EX, UK
Y. Aso
AFFILIATIONS
Gravitational Wave Science Project, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan
Astronomical course, The Graduate University for Advanced Studies (SOKENDAI), 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan
M. Assiduo
AFFILIATIONS
Università degli Studi di Urbino “Carlo Bo,” I-61029 Urbino, Italy
INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy
S. Assis de Souza Melo
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
S. M. Aston
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
P. Astone
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
F. Attadio
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
F. Aubin
AFFILIATIONS
Université de Strasbourg, CNRS, IPHC UMR 7178, F-67000 Strasbourg, France
K. AultONeal
AFFILIATIONS
Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA
G. Avallone
AFFILIATIONS
Dipartimento di Fisica “E.R. Caianiello,” Università di Salerno, I-84084 Fisciano, Salerno, Italy
S. Babak
AFFILIATIONS
Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
F. Badaracco
AFFILIATIONS
INFN, Sezione di Genova, I-16146 Genova, Italy
C. Badger
AFFILIATIONS
King’s College London, University of London, London WC2R 2LS, UK
S. Bae
AFFILIATIONS
Korea Institute of Science and Technology Information, Daejeon 34141, Republic of Korea
S. Bagnasco
AFFILIATIONS
INFN Sezione di Torino, I-10125 Torino, Italy
E. Bagui
AFFILIATIONS
Université libre de Bruxelles, 1050 Bruxelles, Belgium
L. Baiotti
AFFILIATIONS
International College, Osaka University, 1-1 Machikaneyama-cho, Toyonaka City, Osaka 560-0043, Japan
R. Bajpai
AFFILIATIONS
Gravitational Wave Science Project, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan
T. Baka
AFFILIATIONS
Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, 3584 CC Utrecht, Netherlands
T. Baker
AFFILIATIONS
University of Portsmouth, Portsmouth, PO1 3FX, UK
M. Ball
AFFILIATIONS
University of Oregon, Eugene, OR 97403, USA
G. Ballardin
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
S. W. Ballmer
AFFILIATIONS
Syracuse University, Syracuse, NY 13244, USA
S. Banagiri
AFFILIATIONS
Northwestern University, Evanston, IL 60208, USA
B. Banerjee
AFFILIATIONS
Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
D. Bankar
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
T. M. Baptiste
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
P. Baral
AFFILIATIONS
University of Wisconsin–Milwaukee, Milwaukee, WI 53201, USA
J. C. Barayoga
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
B. C. Barish
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
D. Barker
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
N. Barman
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
P. Barneo
AFFILIATIONS
Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (UB), c. Martí i Franquès, 1, 08028 Barcelona, Spain
Departament de Física Quàntica i Astrofísica (FQA), Universitat de Barcelona (UB), c. Martí i Franqués, 1, 08028 Barcelona, Spain
F. Barone
AFFILIATIONS
INFN, Sezione di Napoli, I-80126 Napoli, Italy
Dipartimento di Medicina, Chirurgia e Odontoiatria “Scuola Medica Salernitana,” Università di Salerno, I-84081 Baronissi, Salerno, Italy
B. Barr
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
L. Barsotti
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
M. Barsuglia
AFFILIATIONS
Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
D. Barta
AFFILIATIONS
HUN-REN Wigner Research Centre for Physics, H-1121 Budapest, Hungary
A. M. Bartoletti
AFFILIATIONS
Concordia University Wisconsin, Mequon, WI 53097, USA
M. A. Barton
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
I. Bartos
AFFILIATIONS
University of Florida, Gainesville, FL 32611, USA
S. Basak
AFFILIATIONS
International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bengaluru 560089, India
A. Basalaev
AFFILIATIONS
Universität Hamburg, D-22761 Hamburg, Germany
R. Bassiri
AFFILIATIONS
Stanford University, Stanford, CA 94305, USA
A. Basti
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
D. E. Bates
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
M. Bawaj
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
Università di Perugia, I-06123 Perugia, Italy
P. Baxi
AFFILIATIONS
University of Michigan, Ann Arbor, MI 48109, USA
J. C. Bayley
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
A. C. Baylor
AFFILIATIONS
University of Wisconsin–Milwaukee, Milwaukee, WI 53201, USA
P. A. Baynard II
AFFILIATIONS
Georgia Institute of Technology, Atlanta, GA 30332, USA
M. Bazzan
AFFILIATIONS
Università di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy
INFN, Sezione di Padova, I-35131 Padova, Italy
V. M. Bedakihale
AFFILIATIONS
Institute for Plasma Research, Bhat, Gandhinagar 382428, India
F. Beirnaert
AFFILIATIONS
Universiteit Gent, B-9000 Gent, Belgium
M. Bejger
AFFILIATIONS
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, 00-716, Warsaw, Poland
D. Belardinelli
AFFILIATIONS
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
A. S. Bell
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
D. S. Bellie
AFFILIATIONS
Northwestern University, Evanston, IL 60208, USA
L. Bellizzi
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
W. Benoit
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
I. Bentara
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
J. D. Bentley
AFFILIATIONS
Universität Hamburg, D-22761 Hamburg, Germany
M. Ben Yaala
AFFILIATIONS
SUPA, University of Strathclyde, Glasgow G1 1XQ, UK
S. Bera
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
F. Bergamin
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
B. K. Berger
AFFILIATIONS
Stanford University, Stanford, CA 94305, USA
S. Bernuzzi
AFFILIATIONS
Theoretisch-Physikalisches Institut, Friedrich-Schiller-Universität Jena, D-07743 Jena, Germany
M. Beroiz
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
C. P. L. Berry
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
D. Bersanetti
AFFILIATIONS
INFN, Sezione di Genova, I-16146 Genova, Italy
A. Bertolini
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
J. Betzwieser
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
D. Beveridge
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
G. Bevilacqua
AFFILIATIONS
Università di Siena, I-53100 Siena, Italy
N. Bevins
AFFILIATIONS
Villanova University, Villanova, PA 19085, USA
R. Bhandare
AFFILIATIONS
RRCAT, Indore, Madhya Pradesh 452013, India
S. A. Bhat
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
R. Bhatt
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
D. Bhattacharjee
AFFILIATIONS
Kenyon College, Gambier, OH 43022, USA
Missouri University of Science and Technology, Rolla, MO 65409, USA
S. Bhaumik
AFFILIATIONS
University of Florida, Gainesville, FL 32611, USA
S. Bhowmick
AFFILIATIONS
Colorado State University, Fort Collins, CO 80523, USA
V. Biancalana
AFFILIATIONS
Università di Siena, I-53100 Siena, Italy
A. Bianchi
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Department of Physics and Astronomy, Vrije Universiteit Amsterdam, 1081 HV Amsterdam, Netherlands
I. A. Bilenko
AFFILIATIONS
Lomonosov Moscow State University, Moscow 119991, Russia
G. Billingsley
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
A. Binetti
AFFILIATIONS
Katholieke Universiteit Leuven, Oude Markt 13, 3000 Leuven, Belgium
S. Bini
AFFILIATIONS
Università di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy
INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy
C. Binu
AFFILIATIONS
Rochester Institute of Technology, Rochester, NY 14623, USA
O. Birnholtz
AFFILIATIONS
Bar-Ilan University, Ramat Gan, 5290002, Israel
S. Biscoveanu
AFFILIATIONS
Northwestern University, Evanston, IL 60208, USA
A. Bisht
AFFILIATIONS
Leibniz Universität Hannover, D-30167 Hannover, Germany
M. Bitossi
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
M.-A. Bizouard
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
S. Blaber
AFFILIATIONS
University of British Columbia, Vancouver, BC V6T 1Z4, Canada
J. K. Blackburn
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
L. A. Blagg
AFFILIATIONS
University of Oregon, Eugene, OR 97403, USA
C. D. Blair
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
LIGO Livingston Observatory, Livingston, LA 70754, USA
D. G. Blair
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
F. Bobba
AFFILIATIONS
Dipartimento di Fisica “E.R. Caianiello,” Università di Salerno, I-84084 Fisciano, Salerno, Italy
INFN, Sezione di Napoli, Gruppo Collegato di Salerno, I-80126 Napoli, Italy
N. Bode
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
G. Boileau
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
M. Boldrini
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
G. N. Bolingbroke
AFFILIATIONS
OzGrav, University of Adelaide, Adelaide, South Australia 5005, Australia
A. Bolliand
AFFILIATIONS
Aix Marseille Univ, CNRS, Centrale Med, Institut Fresnel, F-13013 Marseille, France
Centre national de la recherche scientifique, 75016 Paris, France
L. D. Bonavena
AFFILIATIONS
University of Florida, Gainesville, FL 32611, USA
Università di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy
R. Bondarescu
AFFILIATIONS
Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (UB), c. Martí i Franquès, 1, 08028 Barcelona, Spain
F. Bondu
AFFILIATIONS
Univ Rennes, CNRS, Institut FOTON - UMR 6082, F-35000 Rennes, France
E. Bonilla
AFFILIATIONS
Stanford University, Stanford, CA 94305, USA
M. S. Bonilla
AFFILIATIONS
California State University Fullerton, Fullerton, CA 92831, USA
A. Bonino
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
R. Bonnand
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
Centre national de la recherche scientifique, 75016 Paris, France
P. Booker
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
A. Borchers
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
S. Borhanian
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
V. Boschi
AFFILIATIONS
INFN, Sezione di Pisa, I-56127 Pisa, Italy
S. Bose
AFFILIATIONS
Washington State University, Pullman, WA 99164, USA
V. Bossilkov
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
A. Boudon
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
A. Bozzi
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
C. Bradaschia
AFFILIATIONS
INFN, Sezione di Pisa, I-56127 Pisa, Italy
P. R. Brady
AFFILIATIONS
University of Wisconsin–Milwaukee, Milwaukee, WI 53201, USA
A. Branch
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
M. Branchesi
AFFILIATIONS
Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
INFN, Laboratori Nazionali del Gran Sasso, I-67100 Assergi, Italy
I. Braun
AFFILIATIONS
Kenyon College, Gambier, OH 43022, USA
T. Briant
AFFILIATIONS
Laboratoire Kastler Brossel, Sorbonne Université, CNRS, ENS-Université PSL, Collège de France, F-75005 Paris, France
A. Brillet
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
M. Brinkmann
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
P. Brockill
AFFILIATIONS
University of Wisconsin–Milwaukee, Milwaukee, WI 53201, USA
E. Brockmueller
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
A. F. Brooks
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
B. C. Brown
AFFILIATIONS
University of Florida, Gainesville, FL 32611, USA
D. D. Brown
AFFILIATIONS
OzGrav, University of Adelaide, Adelaide, South Australia 5005, Australia
M. L. Brozzetti
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
Università di Perugia, I-06123 Perugia, Italy
S. Brunett
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
G. Bruno
AFFILIATIONS
Université catholique de Louvain, B-1348 Louvain-la-Neuve, Belgium
R. Bruntz
AFFILIATIONS
Christopher Newport University, Newport News, VA 23606, USA
J. Bryant
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
Y. Bu
AFFILIATIONS
OzGrav, University of Melbourne, Parkville, Victoria 3010, Australia
F. Bucci
AFFILIATIONS
INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy
J. Buchanan
AFFILIATIONS
Christopher Newport University, Newport News, VA 23606, USA
O. Bulashenko
AFFILIATIONS
Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (UB), c. Martí i Franquès, 1, 08028 Barcelona, Spain
Departament de Física Quàntica i Astrofísica (FQA), Universitat de Barcelona (UB), c. Martí i Franqués, 1, 08028 Barcelona, Spain
T. Bulik
AFFILIATIONS
Astronomical Observatory Warsaw University, 00-478 Warsaw, Poland
H. J. Bulten
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
A. Buonanno
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
University of Maryland, College Park, MD 20742, USA
K. Burtnyk
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
R. Buscicchio
AFFILIATIONS
Università degli Studi di Milano-Bicocca, I-20126 Milano, Italy
INFN, Sezione di Milano-Bicocca, I-20126 Milano, Italy
D. Buskulic
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
C. Buy
AFFILIATIONS
L2IT, Laboratoire des 2 Infinis - Toulouse, Université de Toulouse, CNRS/IN2P3, UPS, F-31062 Toulouse Cedex 9, France
R. L. Byer
AFFILIATIONS
Stanford University, Stanford, CA 94305, USA
G. S. Cabourn Davies
AFFILIATIONS
University of Portsmouth, Portsmouth, PO1 3FX, UK
G. Cabras
AFFILIATIONS
Dipartimento di Scienze Matematiche, Informatiche e Fisiche, Università di Udine, I-33100 Udine, Italy
INFN, Sezione di Trieste, I-34127 Trieste, Italy
R. Cabrita
AFFILIATIONS
Université catholique de Louvain, B-1348 Louvain-la-Neuve, Belgium
V. Cáceres-Barbosa
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
L. Cadonati
AFFILIATIONS
Georgia Institute of Technology, Atlanta, GA 30332, USA
G. Cagnoli
AFFILIATIONS
Université de Lyon, Université Claude Bernard Lyon 1, CNRS, Institut Lumière Matière, F-69622 Villeurbanne, France
C. Cahillane
AFFILIATIONS
Syracuse University, Syracuse, NY 13244, USA
A. Calafat
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
J. Calderón Bustillo
AFFILIATIONS
IGFAE, Universidade de Santiago de Compostela, 15782, Spain
T. A. Callister
AFFILIATIONS
University of Chicago, Chicago, IL 60637, USA
E. Calloni
AFFILIATIONS
INFN, Sezione di Napoli, I-80126 Napoli, Italy
Università di Napoli “Federico II,” I-80126 Napoli, Italy
M. Canepa
AFFILIATIONS
INFN, Sezione di Genova, I-16146 Genova, Italy
Dipartimento di Fisica, Università degli Studi di Genova, I-16146 Genova, Italy
G. Caneva Santoro
AFFILIATIONS
Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra (Barcelona), Spain
K. C. Cannon
AFFILIATIONS
University of Tokyo, Tokyo, 113-0033, Japan
H. Cao
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
L. A. Capistran
AFFILIATIONS
University of Arizona, Tucson, AZ 85721, USA
E. Capocasa
AFFILIATIONS
Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
E. Capote
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
G. Capurri
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
G. Carapella
AFFILIATIONS
Dipartimento di Fisica “E.R. Caianiello,” Università di Salerno, I-84084 Fisciano, Salerno, Italy
INFN, Sezione di Napoli, Gruppo Collegato di Salerno, I-80126 Napoli, Italy
F. Carbognani
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
M. Carlassara
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
J. B. Carlin
AFFILIATIONS
OzGrav, University of Melbourne, Parkville, Victoria 3010, Australia
T. K. Carlson
AFFILIATIONS
University of Massachusetts Dartmouth, North Dartmouth, MA 02747, USA
M. F. Carney
AFFILIATIONS
Kenyon College, Gambier, OH 43022, USA
M. Carpinelli
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
Università degli Studi di Milano-Bicocca, I-20126 Milano, Italy
INFN, Laboratori Nazionali del Sud, I-95125 Catania, Italy
G. Carrillo
AFFILIATIONS
University of Oregon, Eugene, OR 97403, USA
J. J. Carter
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
G. Carullo
AFFILIATIONS
Niels Bohr Institute, Copenhagen University, 2100 København, Denmark
J. Casanueva Diaz
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
C. Casentini
AFFILIATIONS
Università di Roma Tor Vergata, I-00133 Roma, Italy
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
Istituto di Astrofisica e Planetologia Spaziali di Roma, 00133 Roma, Italy
S. Y. Castro-Lucas
AFFILIATIONS
Colorado State University, Fort Collins, CO 80523, USA
S. Caudill
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, 3584 CC Utrecht, Netherlands
University of Massachusetts Dartmouth, North Dartmouth, MA 02747, USA
M. Cavaglià
AFFILIATIONS
Missouri University of Science and Technology, Rolla, MO 65409, USA
R. Cavalieri
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
G. Cella
AFFILIATIONS
INFN, Sezione di Pisa, I-56127 Pisa, Italy
P. Cerdá-Durán
AFFILIATIONS
Departamento de Astronomía y Astrofísica, Universitat de València, E-46100 Burjassot, València, Spain
Observatori Astronòmic, Universitat de València, E-46980 Paterna, València, Spain
E. Cesarini
AFFILIATIONS
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
W. Chaibi
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
P. Chakraborty
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
S. Chakraborty
AFFILIATIONS
RRCAT, Indore, Madhya Pradesh 452013, India
S. Chalathadka Subrahmanya
AFFILIATIONS
Universität Hamburg, D-22761 Hamburg, Germany
J. C. L. Chan
AFFILIATIONS
Niels Bohr Institute, University of Copenhagen, 2100 Kóbenhavn, Denmark
M. Chan
AFFILIATIONS
University of British Columbia, Vancouver, BC V6T 1Z4, Canada
R.-J. Chang
AFFILIATIONS
Department of Physics, National Cheng Kung University, No. 1, University Road, Tainan City 701, Taiwan
S. Chao
AFFILIATIONS
National Tsing Hua University, Hsinchu City 30013, Taiwan
National Central University, Taoyuan City 320317, Taiwan
E. L. Charlton
AFFILIATIONS
Christopher Newport University, Newport News, VA 23606, USA
P. Charlton
AFFILIATIONS
OzGrav, Charles Sturt University, Wagga Wagga, New South Wales 2678, Australia
E. Chassande-Mottin
AFFILIATIONS
Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
C. Chatterjee
AFFILIATIONS
Vanderbilt University, Nashville, TN 37235, USA
Debarati Chatterjee
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
Deep Chatterjee
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
M. Chaturvedi
AFFILIATIONS
RRCAT, Indore, Madhya Pradesh 452013, India
S. Chaty
AFFILIATIONS
Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
K. Chatziioannou
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
C. Checchia
AFFILIATIONS
Università di Siena, I-53100 Siena, Italy
A. Chen
AFFILIATIONS
Queen Mary University of London, London E1 4NS, UK
A. H.-Y. Chen
AFFILIATIONS
Department of Electrophysics, National Yang Ming Chiao Tung University, 101 University Street, Hsinchu, Taiwan
D. Chen
AFFILIATIONS
Kamioka Branch, National Astronomical Observatory of Japan, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
H. Chen
AFFILIATIONS
National Tsing Hua University, Hsinchu City 30013, Taiwan
H. Y. Chen
AFFILIATIONS
University of Texas, Austin, TX 78712, USA
S. Chen
AFFILIATIONS
Vanderbilt University, Nashville, TN 37235, USA
Y. Chen
AFFILIATIONS
National Tsing Hua University, Hsinchu City 30013, Taiwan
Yanbei Chen
AFFILIATIONS
CaRT, California Institute of Technology, Pasadena, CA 91125, USA
Yitian Chen
AFFILIATIONS
Cornell University, Ithaca, NY 14850, USA
H. P. Cheng
AFFILIATIONS
Northeastern University, Boston, MA 02115, USA
P. Chessa
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
Università di Perugia, I-06123 Perugia, Italy
H. T. Cheung
AFFILIATIONS
University of Michigan, Ann Arbor, MI 48109, USA
S. Y. Cheung
AFFILIATIONS
OzGrav, School of Physics & Astronomy, Monash University, Clayton 3800, Victoria, Australia
F. Chiadini
AFFILIATIONS
INFN, Sezione di Napoli, Gruppo Collegato di Salerno, I-80126 Napoli, Italy
Dipartimento di Ingegneria Industriale (DIIN), Università di Salerno, I-84084 Fisciano, Salerno, Italy
G. Chiarini
AFFILIATIONS
INFN, Sezione di Padova, I-35131 Padova, Italy
R. Chierici
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
A. Chincarini
AFFILIATIONS
INFN, Sezione di Genova, I-16146 Genova, Italy
M. L. Chiofalo
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
A. Chiummo
AFFILIATIONS
INFN, Sezione di Napoli, I-80126 Napoli, Italy
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
C. Chou
AFFILIATIONS
Department of Electrophysics, National Yang Ming Chiao Tung University, 101 University Street, Hsinchu, Taiwan
S. Choudhary
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
N. Christensen
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
S. S. Y. Chua
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
P. Chugh
AFFILIATIONS
OzGrav, School of Physics & Astronomy, Monash University, Clayton 3800, Victoria, Australia
G. Ciani
AFFILIATIONS
Università di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy
INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy
P. Ciecielag
AFFILIATIONS
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, 00-716, Warsaw, Poland
M. Cieślar
AFFILIATIONS
Astronomical Observatory Warsaw University, 00-478 Warsaw, Poland
M. Cifaldi
AFFILIATIONS
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
R. Ciolfi
AFFILIATIONS
INFN, Sezione di Padova, I-35131 Padova, Italy
INAF, Osservatorio Astronomico di Padova, I-35122 Padova, Italy
F. Clara
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
J. A. Clark
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
Georgia Institute of Technology, Atlanta, GA 30332, USA
J. Clarke
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
T. A. Clarke
AFFILIATIONS
OzGrav, School of Physics & Astronomy, Monash University, Clayton 3800, Victoria, Australia
P. Clearwater
AFFILIATIONS
OzGrav, Swinburne University of Technology, Hawthorn VIC 3122, Australia
S. Clesse
AFFILIATIONS
Université libre de Bruxelles, 1050 Bruxelles, Belgium
S. M. Clyne
AFFILIATIONS
University of Rhode Island, Kingston, RI 02881, USA
E. Coccia
AFFILIATIONS
Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra (Barcelona), Spain
Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
INFN, Laboratori Nazionali del Gran Sasso, I-67100 Assergi, Italy
E. Codazzo
AFFILIATIONS
INFN Cagliari, Physics Department, Università degli Studi di Cagliari, Cagliari 09042, Italy
P.-F. Cohadon
AFFILIATIONS
Laboratoire Kastler Brossel, Sorbonne Université, CNRS, ENS-Université PSL, Collège de France, F-75005 Paris, France
S. Colace
AFFILIATIONS
Dipartimento di Fisica, Università degli Studi di Genova, I-16146 Genova, Italy
E. Colangeli
AFFILIATIONS
University of Portsmouth, Portsmouth, PO1 3FX, UK
M. Colleoni
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
C. G. Collette
AFFILIATIONS
Université Libre de Bruxelles, Brussels 1050, Belgium
J. Collins
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
S. Colloms
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
A. Colombo
AFFILIATIONS
INFN, Sezione di Milano-Bicocca, I-20126 Milano, Italy
INAF, Osservatorio Astronomico di Brera sede di Merate, I-23807 Merate, Lecco, Italy
C. M. Compton
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
G. Connolly
AFFILIATIONS
University of Oregon, Eugene, OR 97403, USA
L. Conti
AFFILIATIONS
INFN, Sezione di Padova, I-35131 Padova, Italy
T. R. Corbitt
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
I. Cordero-Carrión
AFFILIATIONS
Departamento de Matemáticas, Universitat de València, E-46100 Burjassot, València, Spain
S. Corezzi
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
Università di Perugia, I-06123 Perugia, Italy
N. J. Cornish
AFFILIATIONS
Montana State University, Bozeman, MT 59717, USA
A. Corsi
AFFILIATIONS
Johns Hopkins University, Baltimore, MD 21218, USA
S. Cortese
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
R. Cottingham
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
M. W. Coughlin
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
A. Couineaux
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
J.-P. Coulon
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
J.-F. Coupechoux
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
P. Couvares
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
Georgia Institute of Technology, Atlanta, GA 30332, USA
D. M. Coward
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
R. Coyne
AFFILIATIONS
University of Rhode Island, Kingston, RI 02881, USA
K. Craig
AFFILIATIONS
SUPA, University of Strathclyde, Glasgow G1 1XQ, UK
J. D. E. Creighton
AFFILIATIONS
University of Wisconsin–Milwaukee, Milwaukee, WI 53201, USA
T. D. Creighton
AFFILIATIONS
The University of Texas Rio Grande Valley, Brownsville, TX 78520, USA
P. Cremonese
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
A. W. Criswell
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
S. Crook
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
R. Crouch
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
J. Csizmazia
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
J. R. Cudell
AFFILIATIONS
Université de Liège, B-4000 Liège, Belgium
T. J. Cullen
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
A. Cumming
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
E. Cuoco
AFFILIATIONS
DIFA- Alma Mater Studiorum Università di Bologna, Via Zamboni, 33 - 40126 Bologna, Italy
Istituto Nazionale Di Fisica Nucleare - Sezione di Bologna, viale Carlo Berti Pichat 6/2, Bologna, Italy
M. Cusinato
AFFILIATIONS
Departamento de Astronomía y Astrofísica, Universitat de València, E-46100 Burjassot, València, Spain
P. Dabadie
AFFILIATIONS
Université de Lyon, Université Claude Bernard Lyon 1, CNRS, Institut Lumière Matière, F-69622 Villeurbanne, France
L. V. Da Conceição
AFFILIATIONS
University of Manitoba, Winnipeg, MB R3T 2N2, Canada
T. Dal Canton
AFFILIATIONS
Université Paris-Saclay, CNRS/IN2P3, IJCLab, 91405 Orsay, France
S. Dall’Osso
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
S. Dal Pra
AFFILIATIONS
INFN-CNAF - Bologna, Viale Carlo Berti Pichat, 6/2, 40127 Bologna BO, Italy
G. Dálya
AFFILIATIONS
L2IT, Laboratoire des 2 Infinis - Toulouse, Université de Toulouse, CNRS/IN2P3, UPS, F-31062 Toulouse Cedex 9, France
B. D’Angelo
AFFILIATIONS
INFN, Sezione di Genova, I-16146 Genova, Italy
S. Danilishin
AFFILIATIONS
Maastricht University, 6200 MD Maastricht, The Netherlands
Nikhef, 1098 XG Amsterdam, The Netherlands
S. D’Antonio
AFFILIATIONS
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
K. Danzmann
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
K. E. Darroch
AFFILIATIONS
Christopher Newport University, Newport News, VA 23606, USA
L. P. Dartez
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
A. Dasgupta
AFFILIATIONS
Institute for Plasma Research, Bhat, Gandhinagar 382428, India
S. Datta
AFFILIATIONS
Chennai Mathematical Institute, Chennai 603103, India
V. Dattilo
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
A. Daumas
AFFILIATIONS
Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
N. Davari
AFFILIATIONS
INFN, Laboratori Nazionali del Sud, I-95125 Catania, Italy
Università degli Studi di Sassari, I-07100 Sassari, Italy
I. Dave
AFFILIATIONS
RRCAT, Indore, Madhya Pradesh 452013, India
A. Davenport
AFFILIATIONS
Colorado State University, Fort Collins, CO 80523, USA
M. Davier
AFFILIATIONS
Université Paris-Saclay, CNRS/IN2P3, IJCLab, 91405 Orsay, France
T. F. Davies
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
D. Davis
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
L. Davis
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
M. C. Davis
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
P. Davis
AFFILIATIONS
Université de Normandie, ENSICAEN, UNICAEN, CNRS/IN2P3, LPC Caen, F-14000 Caen, France
Laboratoire de Physique Corpusculaire Caen, 6 boulevard du maréchal Juin, F-14050 Caen, France
M. Dax
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
J. De Bolle
AFFILIATIONS
Universiteit Gent, B-9000 Gent, Belgium
M. Deenadayalan
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
J. Degallaix
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, Laboratoire des Matériaux Avancés (LMA), IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
U. Deka
AFFILIATIONS
International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bengaluru 560089, India
M. De Laurentis
AFFILIATIONS
INFN, Sezione di Napoli, I-80126 Napoli, Italy
Università di Napoli “Federico II,” I-80126 Napoli, Italy
S. Deléglise
AFFILIATIONS
Laboratoire Kastler Brossel, Sorbonne Université, CNRS, ENS-Université PSL, Collège de France, F-75005 Paris, France
F. De Lillo
AFFILIATIONS
Universiteit Antwerpen, 2000 Antwerpen, Belgium
D. Dell’Aquila
AFFILIATIONS
INFN, Laboratori Nazionali del Sud, I-95125 Catania, Italy
Università degli Studi di Sassari, I-07100 Sassari, Italy
F. Della Valle
AFFILIATIONS
Università di Siena, I-53100 Siena, Italy
W. Del Pozzo
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
F. De Marco
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
G. Demasi
AFFILIATIONS
INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy
Università di Firenze, Sesto Fiorentino I-50019, Italy
F. De Matteis
AFFILIATIONS
Università di Roma Tor Vergata, I-00133 Roma, Italy
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
V. D’Emilio
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
N. Demos
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
A. Depasse
AFFILIATIONS
Université catholique de Louvain, B-1348 Louvain-la-Neuve, Belgium
N. DePergola
AFFILIATIONS
Villanova University, Villanova, PA 19085, USA
R. De Pietri
AFFILIATIONS
Dipartimento di Scienze Matematiche, Fisiche e Informatiche, Università di Parma, I-43124 Parma, Italy
INFN, Sezione di Milano Bicocca, Gruppo Collegato di Parma, I-43124 Parma, Italy
R. De Rosa
AFFILIATIONS
INFN, Sezione di Napoli, I-80126 Napoli, Italy
Università di Napoli “Federico II,” I-80126 Napoli, Italy
C. De Rossi
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
M. Desai
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
R. DeSalvo
AFFILIATIONS
University of Sannio at Benevento, I-82100 Benevento, Italy and INFN, Sezione di Napoli, I-80100 Napoli, Italy
A. DeSimone
AFFILIATIONS
Marquette University, Milwaukee, WI 53233, USA
R. De Simone
AFFILIATIONS
Dipartimento di Ingegneria Industriale (DIIN), Università di Salerno, I-84084 Fisciano, Salerno, Italy
A. Dhani
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
R. Diab
AFFILIATIONS
University of Florida, Gainesville, FL 32611, USA
M. C. Díaz
AFFILIATIONS
The University of Texas Rio Grande Valley, Brownsville, TX 78520, USA
M. Di Cesare
AFFILIATIONS
INFN, Sezione di Napoli, I-80126 Napoli, Italy
Università di Napoli “Federico II,” I-80126 Napoli, Italy
G. Dideron
AFFILIATIONS
Perimeter Institute, Waterloo, ON N2L 2Y5, Canada
N. A. Didio
AFFILIATIONS
Syracuse University, Syracuse, NY 13244, USA
T. Dietrich
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
L. Di Fiore
AFFILIATIONS
INFN, Sezione di Napoli, I-80126 Napoli, Italy
C. Di Fronzo
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
M. Di Giovanni
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
T. Di Girolamo
AFFILIATIONS
INFN, Sezione di Napoli, I-80126 Napoli, Italy
Università di Napoli “Federico II,” I-80126 Napoli, Italy
D. Diksha
AFFILIATIONS
Maastricht University, 6200 MD Maastricht, The Netherlands
Nikhef, 1098 XG Amsterdam, The Netherlands
A. Di Michele
AFFILIATIONS
Università di Perugia, I-06123 Perugia, Italy
J. Ding
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
Corps des Mines, Mines Paris, Université PSL, 60 Bd Saint-Michel, 75272 Paris, France
S. Di Pace
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
I. Di Palma
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
F. Di Renzo
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
Divyajyoti
AFFILIATIONS
Indian Institute of Technology Madras, Chennai 600036, India
A. Dmitriev
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
Z. Doctor
AFFILIATIONS
Northwestern University, Evanston, IL 60208, USA
N. Doerksen
AFFILIATIONS
University of Manitoba, Winnipeg, MB R3T 2N2, Canada
E. Dohmen
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
D. Dominguez
AFFILIATIONS
Graduate School of Science, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan
L. D’Onofrio
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
F. Donovan
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
K. L. Dooley
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
T. Dooney
AFFILIATIONS
Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, 3584 CC Utrecht, Netherlands
S. Doravari
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
O. Dorosh
AFFILIATIONS
National Center for Nuclear Research, 05-400 Świerk-Otwock, Poland
M. Drago
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
J. C. Driggers
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
J.-G. Ducoin
AFFILIATIONS
Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
Institut d’Astrophysique de Paris, Sorbonne Université, CNRS, UMR 7095, 75014 Paris, France
L. Dunn
AFFILIATIONS
OzGrav, University of Melbourne, Parkville, Victoria 3010, Australia
U. Dupletsa
AFFILIATIONS
Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
D. D’Urso
AFFILIATIONS
INFN Cagliari, Physics Department, Università degli Studi di Cagliari, Cagliari 09042, Italy
Università degli Studi di Sassari, I-07100 Sassari, Italy
H. Duval
AFFILIATIONS
Vrije Universiteit Brussel, 1050 Brussel, Belgium
S. E. Dwyer
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
C. Eassa
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
M. Ebersold
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
T. Eckhardt
AFFILIATIONS
Universität Hamburg, D-22761 Hamburg, Germany
G. Eddolls
AFFILIATIONS
Syracuse University, Syracuse, NY 13244, USA
B. Edelman
AFFILIATIONS
University of Oregon, Eugene, OR 97403, USA
T. B. Edo
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
O. Edy
AFFILIATIONS
University of Portsmouth, Portsmouth, PO1 3FX, UK
A. Effler
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
J. Eichholz
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
H. Einsle
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
M. Eisenmann
AFFILIATIONS
Gravitational Wave Science Project, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan
R. A. Eisenstein
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
A. Ejlli
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
M. Emma
AFFILIATIONS
Royal Holloway, University of London, London TW20 0EX, UK
K. Endo
AFFILIATIONS
Faculty of Science, University of Toyama, 3190 Gofuku, Toyama City, Toyama 930-8555, Japan
R. Enficiaud
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
A. J. Engl
AFFILIATIONS
Stanford University, Stanford, CA 94305, USA
L. Errico
AFFILIATIONS
INFN, Sezione di Napoli, I-80126 Napoli, Italy
Università di Napoli “Federico II,” I-80126 Napoli, Italy
R. Espinosa
AFFILIATIONS
The University of Texas Rio Grande Valley, Brownsville, TX 78520, USA
M. Esposito
AFFILIATIONS
INFN, Sezione di Napoli, I-80126 Napoli, Italy
Università di Napoli “Federico II,” I-80126 Napoli, Italy
R. C. Essick
AFFILIATIONS
Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada
H. Estellés
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
T. Etzel
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
M. Evans
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
T. Evstafyeva
AFFILIATIONS
University of Cambridge, Cambridge CB2 1TN, UK
B. E. Ewing
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
J. M. Ezquiaga
AFFILIATIONS
Niels Bohr Institute, University of Copenhagen, 2100 Kóbenhavn, Denmark
F. Fabrizi
AFFILIATIONS
Università degli Studi di Urbino “Carlo Bo,” I-61029 Urbino, Italy
INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy
F. Faedi
AFFILIATIONS
Università degli Studi di Urbino “Carlo Bo,” I-61029 Urbino, Italy
INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy
V. Fafone
AFFILIATIONS
Università di Roma Tor Vergata, I-00133 Roma, Italy
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
S. Fairhurst
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
A. M. Farah
AFFILIATIONS
University of Chicago, Chicago, IL 60637, USA
B. Farr
AFFILIATIONS
University of Oregon, Eugene, OR 97403, USA
W. M. Farr
AFFILIATIONS
Stony Brook University, Stony Brook, NY 11794, USA
Center for Computational Astrophysics, Flatiron Institute, New York, NY 10010, USA
G. Favaro
AFFILIATIONS
Università di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy
M. Favata
AFFILIATIONS
Montclair State University, Montclair, NJ 07043, USA
M. Fays
AFFILIATIONS
Université de Liège, B-4000 Liège, Belgium
M. Fazio
AFFILIATIONS
SUPA, University of Strathclyde, Glasgow G1 1XQ, UK
J. Feicht
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
M. M. Fejer
AFFILIATIONS
Stanford University, Stanford, CA 94305, USA
R. Felicetti
AFFILIATIONS
Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy
E. Fenyvesi
AFFILIATIONS
HUN-REN Wigner Research Centre for Physics, H-1121 Budapest, Hungary
HUN-REN Institute for Nuclear Research, H-4026 Debrecen, Hungary
D. L. Ferguson
AFFILIATIONS
University of Texas, Austin, TX 78712, USA
T. Fernandes
AFFILIATIONS
Departamento de Astronomía y Astrofísica, Universitat de València, E-46100 Burjassot, València, Spain
Centro de Física das Universidades do Minho e do Porto, Universidade do Minho, PT-4710-057 Braga, Portugal
D. Fernando
AFFILIATIONS
Rochester Institute of Technology, Rochester, NY 14623, USA
S. Ferraiuolo
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
Centre de Physique des Particules de Marseille, 163, avenue de Luminy, 13288 Marseille cedex 09, France
I. Ferrante
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
T. A. Ferreira
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
F. Fidecaro
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
P. Figura
AFFILIATIONS
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, 00-716, Warsaw, Poland
A. Fiori
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
I. Fiori
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
M. Fishbach
AFFILIATIONS
Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada
R. P. Fisher
AFFILIATIONS
Christopher Newport University, Newport News, VA 23606, USA
R. Fittipaldi
AFFILIATIONS
INFN, Sezione di Napoli, Gruppo Collegato di Salerno, I-80126 Napoli, Italy
CNR-SPIN, I-84084 Fisciano, Salerno, Italy
V. Fiumara
AFFILIATIONS
INFN, Sezione di Napoli, Gruppo Collegato di Salerno, I-80126 Napoli, Italy
Scuola di Ingegneria, Università della Basilicata, I-85100 Potenza, Italy
R. Flaminio
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
S. M. Fleischer
AFFILIATIONS
Western Washington University, Bellingham, WA 98225, USA
L. S. Fleming
AFFILIATIONS
SUPA, University of the West of Scotland, Paisley PA1 2BE, UK
E. Floden
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
H. Fong
AFFILIATIONS
University of British Columbia, Vancouver, BC V6T 1Z4, Canada
J. A. Font
AFFILIATIONS
Departamento de Astronomía y Astrofísica, Universitat de València, E-46100 Burjassot, València, Spain
Observatori Astronòmic, Universitat de València, E-46980 Paterna, València, Spain
C. Foo
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
B. Fornal
AFFILIATIONS
Barry University, Miami Shores, FL 33168, USA
P. W. F. Forsyth
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
K. Franceschetti
AFFILIATIONS
Dipartimento di Scienze Matematiche, Fisiche e Informatiche, Università di Parma, I-43124 Parma, Italy
N. Franchini
AFFILIATIONS
Centro de Astrofísica e Gravitação, Departamento de Física, Instituto Superior Técnico - IST, Universidade de Lisboa - UL, Av. Rovisco Pais 1, 1049-001 Lisboa, Portugal
S. Frasca
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
F. Frasconi
AFFILIATIONS
INFN, Sezione di Pisa, I-56127 Pisa, Italy
A. Frattale Mascioli
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
Z. Frei
AFFILIATIONS
Eötvös University, Budapest 1117, Hungary
A. Freise
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Department of Physics and Astronomy, Vrije Universiteit Amsterdam, 1081 HV Amsterdam, Netherlands
O. Freitas
AFFILIATIONS
Departamento de Astronomía y Astrofísica, Universitat de València, E-46100 Burjassot, València, Spain
Centro de Física das Universidades do Minho e do Porto, Universidade do Minho, PT-4710-057 Braga, Portugal
R. Frey
AFFILIATIONS
University of Oregon, Eugene, OR 97403, USA
W. Frischhertz
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
P. Fritschel
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
V. V. Frolov
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
G. G. Fronzé
AFFILIATIONS
INFN Sezione di Torino, I-10125 Torino, Italy
M. Fuentes-Garcia
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
S. Fujii
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8582, Japan
T. Fujimori
AFFILIATIONS
Nambu Yoichiro Institute of Theoretical and Experimental Physics (NITEP), Osaka Metropolitan University, 3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka City, Osaka 558-8585, Japan
P. Fulda
AFFILIATIONS
University of Florida, Gainesville, FL 32611, USA
M. Fyffe
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
B. Gadre
AFFILIATIONS
Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, 3584 CC Utrecht, Netherlands
J. R. Gair
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
S. Galaudage
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Lagrange, F-06304 Nice, France
V. Galdi
AFFILIATIONS
University of Sannio at Benevento, I-82100 Benevento, Italy and INFN, Sezione di Napoli, I-80100 Napoli, Italy
H. Gallagher
AFFILIATIONS
Rochester Institute of Technology, Rochester, NY 14623, USA
B. Gallego
AFFILIATIONS
California State University, Los Angeles, Los Angeles, CA 90032, USA
R. Gamba
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
Theoretisch-Physikalisches Institut, Friedrich-Schiller-Universität Jena, D-07743 Jena, Germany
A. Gamboa
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
D. Ganapathy
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
A. Ganguly
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
B. Garaventa
AFFILIATIONS
INFN, Sezione di Genova, I-16146 Genova, Italy
Dipartimento di Fisica, Università degli Studi di Genova, I-16146 Genova, Italy
J. García-Bellido
AFFILIATIONS
Instituto de Fisica Teorica UAM-CSIC, Universidad Autonoma de Madrid, 28049 Madrid, Spain
C. García Núñez
AFFILIATIONS
SUPA, University of the West of Scotland, Paisley PA1 2BE, UK
C. García-Quirós
AFFILIATIONS
University of Zurich, Winterthurerstrasse 190, 8057 Zurich, Switzerland
J. W. Gardner
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
K. A. Gardner
AFFILIATIONS
University of British Columbia, Vancouver, BC V6T 1Z4, Canada
J. Gargiulo
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
A. Garron
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
F. Garufi
AFFILIATIONS
INFN, Sezione di Napoli, I-80126 Napoli, Italy
Università di Napoli “Federico II,” I-80126 Napoli, Italy
P. A. Garver
AFFILIATIONS
Stanford University, Stanford, CA 94305, USA
C. Gasbarra
AFFILIATIONS
Università di Roma Tor Vergata, I-00133 Roma, Italy
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
B. Gateley
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
F. Gautier
AFFILIATIONS
Laboratoire d’Acoustique de l’Université du Mans, UMR CNRS 6613, F-72085 Le Mans, France
V. Gayathri
AFFILIATIONS
University of Wisconsin–Milwaukee, Milwaukee, WI 53201, USA
T. Gayer
AFFILIATIONS
Syracuse University, Syracuse, NY 13244, USA
G. Gemme
AFFILIATIONS
INFN, Sezione di Genova, I-16146 Genova, Italy
A. Gennai
AFFILIATIONS
INFN, Sezione di Pisa, I-56127 Pisa, Italy
V. Gennari
AFFILIATIONS
L2IT, Laboratoire des 2 Infinis - Toulouse, Université de Toulouse, CNRS/IN2P3, UPS, F-31062 Toulouse Cedex 9, France
J. George
AFFILIATIONS
RRCAT, Indore, Madhya Pradesh 452013, India
R. George
AFFILIATIONS
University of Texas, Austin, TX 78712, USA
O. Gerberding
AFFILIATIONS
Universität Hamburg, D-22761 Hamburg, Germany
L. Gergely
AFFILIATIONS
University of Szeged, Dóm tér 9, Szeged 6720, Hungary
Archisman Ghosh
AFFILIATIONS
Universiteit Gent, B-9000 Gent, Belgium
Sayantan Ghosh
AFFILIATIONS
Indian Institute of Technology Bombay, Powai, Mumbai 400 076, India
Shaon Ghosh
AFFILIATIONS
Montclair State University, Montclair, NJ 07043, USA
Shrobana Ghosh
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
Suprovo Ghosh
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
Tathagata Ghosh
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
J. A. Giaime
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
LIGO Livingston Observatory, Livingston, LA 70754, USA
K. D. Giardina
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
D. R. Gibson
AFFILIATIONS
SUPA, University of the West of Scotland, Paisley PA1 2BE, UK
D. T. Gibson
AFFILIATIONS
University of Cambridge, Cambridge CB2 1TN, UK
C. Gier
AFFILIATIONS
SUPA, University of Strathclyde, Glasgow G1 1XQ, UK
S. Gkaitatzis
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
J. Glanzer
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
F. Glotin
AFFILIATIONS
Université Paris-Saclay, CNRS/IN2P3, IJCLab, 91405 Orsay, France
J. Godfrey
AFFILIATIONS
University of Oregon, Eugene, OR 97403, USA
P. Godwin
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
A. S. Goettel
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
E. Goetz
AFFILIATIONS
University of British Columbia, Vancouver, BC V6T 1Z4, Canada
J. Golomb
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
S. Gomez Lopez
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
B. Goncharov
AFFILIATIONS
Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
Y. Gong
AFFILIATIONS
School of Physics and Technology, Wuhan University, Bayi Road 299, Wuchang District, Wuhan, Hubei, 430072, People’s Republic of China
G. González
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
P. Goodarzi
AFFILIATIONS
University of California, Riverside, Riverside, CA 92521, USA
S. Goode
AFFILIATIONS
OzGrav, School of Physics & Astronomy, Monash University, Clayton 3800, Victoria, Australia
A. W. Goodwin-Jones
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
M. Gosselin
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
R. Gouaty
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
D. W. Gould
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
K. Govorkova
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
S. Goyal
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
B. Grace
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
A. Grado
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
Università di Perugia, I-06123 Perugia, Italy
V. Graham
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
A. E. Granados
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
M. Granata
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, Laboratoire des Matériaux Avancés (LMA), IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
V. Granata
AFFILIATIONS
Dipartimento di Fisica “E.R. Caianiello,” Università di Salerno, I-84084 Fisciano, Salerno, Italy
S. Gras
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
P. Grassia
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
A. Gray
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
C. Gray
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
R. Gray
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
G. Greco
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
A. C. Green
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Department of Physics and Astronomy, Vrije Universiteit Amsterdam, 1081 HV Amsterdam, Netherlands
S. M. Green
AFFILIATIONS
University of Portsmouth, Portsmouth, PO1 3FX, UK
S. R. Green
AFFILIATIONS
University of Nottingham NG7 2RD, UK
A. M. Gretarsson
AFFILIATIONS
Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA
E. M. Gretarsson
AFFILIATIONS
Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA
D. Griffith
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
W. L. Griffiths
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
H. L. Griggs
AFFILIATIONS
Georgia Institute of Technology, Atlanta, GA 30332, USA
G. Grignani
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
Università di Perugia, I-06123 Perugia, Italy
C. Grimaud
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
H. Grote
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
S. Grunewald
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
D. Guerra
AFFILIATIONS
Departamento de Astronomía y Astrofísica, Universitat de València, E-46100 Burjassot, València, Spain
D. Guetta
AFFILIATIONS
Ariel University, Ramat HaGolan St 65, Ari’el, Israel
G. M. Guidi
AFFILIATIONS
Università degli Studi di Urbino “Carlo Bo,” I-61029 Urbino, Italy
INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy
A. R. Guimaraes
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
H. K. Gulati
AFFILIATIONS
Institute for Plasma Research, Bhat, Gandhinagar 382428, India
F. Gulminelli
AFFILIATIONS
Université de Normandie, ENSICAEN, UNICAEN, CNRS/IN2P3, LPC Caen, F-14000 Caen, France
Laboratoire de Physique Corpusculaire Caen, 6 boulevard du maréchal Juin, F-14050 Caen, France
A. M. Gunny
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
H. Guo
AFFILIATIONS
University of the Chinese Academy of Sciences / International Centre for Theoretical Physics Asia-Pacific, Bejing 100049, People’s Republic of China
W. Guo
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
Y. Guo
AFFILIATIONS
Maastricht University, 6200 MD Maastricht, The Netherlands
Nikhef, 1098 XG Amsterdam, The Netherlands
Anchal Gupta
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
Anuradha Gupta
AFFILIATIONS
The University of Mississippi, University, MS 38677, USA
I. Gupta
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
N. C. Gupta
AFFILIATIONS
Institute for Plasma Research, Bhat, Gandhinagar 382428, India
P. Gupta
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, 3584 CC Utrecht, Netherlands
S. K. Gupta
AFFILIATIONS
University of Florida, Gainesville, FL 32611, USA
T. Gupta
AFFILIATIONS
Montana State University, Bozeman, MT 59717, USA
V. Gupta
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
N. Gupte
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
J. Gurs
AFFILIATIONS
Universität Hamburg, D-22761 Hamburg, Germany
N. Gutierrez
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, Laboratoire des Matériaux Avancés (LMA), IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
F. Guzman
AFFILIATIONS
University of Arizona, Tucson, AZ 85721, USA
D. Haba
AFFILIATIONS
Graduate School of Science, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan
M. Haberland
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
S. Haino
AFFILIATIONS
Institute of Physics, Academia Sinica, 128 Sec. 2, Academia Rd., Nankang, Taipei 11529, Taiwan
E. D. Hall
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
R. Hamburg
AFFILIATIONS
Science and Technology Institute, Universities Space Research Association, Huntsville, AL 35805, USA
E. Z. Hamilton
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
G. Hammond
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
W.-B. Han
AFFILIATIONS
Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, People’s Republic of China
M. Haney
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
University of Zurich, Winterthurerstrasse 190, 8057 Zurich, Switzerland
J. Hanks
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
C. Hanna
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
M. D. Hannam
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
O. A. Hannuksela
AFFILIATIONS
The Chinese University of Hong Kong, Shatin, NT, Hong Kong
A. G. Hanselman
AFFILIATIONS
University of Chicago, Chicago, IL 60637, USA
H. Hansen
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
J. Hanson
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
R. Harada
AFFILIATIONS
University of Tokyo, Tokyo, 113-0033, Japan
A. R. Hardison
AFFILIATIONS
Marquette University, Milwaukee, WI 53233, USA
S. Harikumar
AFFILIATIONS
National Center for Nuclear Research, 05-400 Świerk-Otwock, Poland
K. Haris
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, 3584 CC Utrecht, Netherlands
T. Harmark
AFFILIATIONS
Niels Bohr Institute, Copenhagen University, 2100 København, Denmark
J. Harms
AFFILIATIONS
Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
INFN, Laboratori Nazionali del Gran Sasso, I-67100 Assergi, Italy
G. M. Harry
AFFILIATIONS
American University, Washington, DC 20016, USA
I. W. Harry
AFFILIATIONS
University of Portsmouth, Portsmouth, PO1 3FX, UK
J. Hart
AFFILIATIONS
Kenyon College, Gambier, OH 43022, USA
B. Haskell
AFFILIATIONS
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, 00-716, Warsaw, Poland
C.-J. Haster
AFFILIATIONS
University of Nevada, Las Vegas, Las Vegas, NV 89154, USA
K. Haughian
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
H. Hayakawa
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
K. Hayama
AFFILIATIONS
Department of Applied Physics, Fukuoka University, 8-19-1 Nanakuma, Jonan, Fukuoka City, Fukuoka 814-0180, Japan
R. Hayes
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
M. C. Heintze
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
J. Heinze
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
J. Heinzel
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
H. Heitmann
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
A. Heffernan
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
F. Hellman
AFFILIATIONS
University of California, Berkeley, CA 94720, USA
A. F. Helmling-Cornell
AFFILIATIONS
University of Oregon, Eugene, OR 97403, USA
G. Hemming
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
O. Henderson-Sapir
AFFILIATIONS
OzGrav, University of Adelaide, Adelaide, South Australia 5005, Australia
M. Hendry
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
I. S. Heng
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
M. H. Hennig
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
C. Henshaw
AFFILIATIONS
Georgia Institute of Technology, Atlanta, GA 30332, USA
M. Heurs
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
A. L. Hewitt
AFFILIATIONS
University of Cambridge, Cambridge CB2 1TN, UK
University of Lancaster, Lancaster LA1 4YW, UK
J. Heyns
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
S. Higginbotham
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
S. Hild
AFFILIATIONS
Maastricht University, 6200 MD Maastricht, The Netherlands
Nikhef, 1098 XG Amsterdam, The Netherlands
S. Hill
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
Y. Himemoto
AFFILIATIONS
College of Industrial Technology, Nihon University, 1-2-1 Izumi, Narashino City, Chiba 275-8575, Japan
N. Hirata
AFFILIATIONS
Gravitational Wave Science Project, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan
C. Hirose
AFFILIATIONS
Faculty of Engineering, Niigata University, 8050 Ikarashi-2-no-cho, Nishi-ku, Niigata City, Niigata 950-2181, Japan
S. Hochheim
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
D. Hofman
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, Laboratoire des Matériaux Avancés (LMA), IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
N. A. Holland
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Department of Physics and Astronomy, Vrije Universiteit Amsterdam, 1081 HV Amsterdam, Netherlands
D. E. Holz
AFFILIATIONS
University of Chicago, Chicago, IL 60637, USA
L. Honet
AFFILIATIONS
Université libre de Bruxelles, 1050 Bruxelles, Belgium
C. Hong
AFFILIATIONS
Stanford University, Stanford, CA 94305, USA
S. Hoshino
AFFILIATIONS
Faculty of Engineering, Niigata University, 8050 Ikarashi-2-no-cho, Nishi-ku, Niigata City, Niigata 950-2181, Japan
J. Hough
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
S. Hourihane
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
N. T. Howard
AFFILIATIONS
Vanderbilt University, Nashville, TN 37235, USA
E. J. Howell
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
C. G. Hoy
AFFILIATIONS
University of Portsmouth, Portsmouth, PO1 3FX, UK
C. A. Hrishikesh
AFFILIATIONS
Università di Roma Tor Vergata, I-00133 Roma, Italy
H.-F. Hsieh
AFFILIATIONS
National Tsing Hua University, Hsinchu City 30013, Taiwan
H.-Y. Hsieh
AFFILIATIONS
National Tsing Hua University, Hsinchu City 30013, Taiwan
C. Hsiung
AFFILIATIONS
Department of Physics, Tamkang University, No. 151, Yingzhuan Road, Danshui District, New Taipei City 25137, Taiwan
W.-F. Hsu
AFFILIATIONS
Katholieke Universiteit Leuven, Oude Markt 13, 3000 Leuven, Belgium
Q. Hu
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
H. Y. Huang
AFFILIATIONS
National Central University, Taoyuan City 320317, Taiwan
Y. Huang
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
Y. T. Huang
AFFILIATIONS
Syracuse University, Syracuse, NY 13244, USA
A. D. Huddart
AFFILIATIONS
Rutherford Appleton Laboratory, Didcot OX11 0DE, UK
B. Hughey
AFFILIATIONS
Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA
D. C. Y. Hui
AFFILIATIONS
Department of Astronomy and Space Science, Chungnam National University, 9 Daehak-ro, Yuseong-gu, Daejeon 34134, Republic of Korea
V. Hui
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
S. Husa
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
R. Huxford
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
L. Iampieri
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
G. A. Iandolo
AFFILIATIONS
Maastricht University, 6200 MD Maastricht, The Netherlands
M. Ianni
AFFILIATIONS
Università di Roma Tor Vergata, I-00133 Roma, Italy
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
A. Ierardi
AFFILIATIONS
Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
A. Iess
AFFILIATIONS
INFN, Sezione di Pisa, I-56127 Pisa, Italy
Scuola Normale Superiore, I-56126 Pisa, Italy
H. Imafuku
AFFILIATIONS
University of Tokyo, Tokyo, 113-0033, Japan
K. Inayoshi
AFFILIATIONS
Kavli Institute for Astronomy and Astrophysics, Peking University, Yiheyuan Road 5, Haidian District, Beijing 100871, People’s Republic of China
Y. Inoue
AFFILIATIONS
National Central University, Taoyuan City 320317, Taiwan
G. Iorio
AFFILIATIONS
Università di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy
P. Iosif
AFFILIATIONS
INFN, Sezione di Trieste, I-34127 Trieste, Italy
Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy
M. H. Iqbal
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
J. Irwin
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
R. Ishikawa
AFFILIATIONS
Department of Physical Sciences, Aoyama Gakuin University, 5-10-1 Fuchinobe, Sagamihara City, Kanagawa 252-5258, Japan
M. Isi
AFFILIATIONS
Stony Brook University, Stony Brook, NY 11794, USA
Center for Computational Astrophysics, Flatiron Institute, New York, NY 10010, USA
Y. Itoh
AFFILIATIONS
Nambu Yoichiro Institute of Theoretical and Experimental Physics (NITEP), Osaka Metropolitan University, 3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka City, Osaka 558-8585, Japan
Department of Physics, Graduate School of Science, Osaka Metropolitan University, 3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka City, Osaka 558-8585, Japan
H. Iwanaga
AFFILIATIONS
Department of Physics, Graduate School of Science, Osaka Metropolitan University, 3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka City, Osaka 558-8585, Japan
M. Iwaya
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8582, Japan
B. R. Iyer
AFFILIATIONS
International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bengaluru 560089, India
C. Jacquet
AFFILIATIONS
L2IT, Laboratoire des 2 Infinis - Toulouse, Université de Toulouse, CNRS/IN2P3, UPS, F-31062 Toulouse Cedex 9, France
P.-E. Jacquet
AFFILIATIONS
Laboratoire Kastler Brossel, Sorbonne Université, CNRS, ENS-Université PSL, Collège de France, F-75005 Paris, France
S. J. Jadhav
AFFILIATIONS
Directorate of Construction, Services & Estate Management, Mumbai 400094, India
S. P. Jadhav
AFFILIATIONS
OzGrav, Swinburne University of Technology, Hawthorn VIC 3122, Australia
T. Jain
AFFILIATIONS
University of Cambridge, Cambridge CB2 1TN, UK
A. L. James
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
P. A. James
AFFILIATIONS
Christopher Newport University, Newport News, VA 23606, USA
R. Jamshidi
AFFILIATIONS
Université Libre de Bruxelles, Brussels 1050, Belgium
A. Jan
AFFILIATIONS
University of Texas, Austin, TX 78712, USA
K. Jani
AFFILIATIONS
Vanderbilt University, Nashville, TN 37235, USA
J. Janquart
AFFILIATIONS
Université catholique de Louvain, B-1348 Louvain-la-Neuve, Belgium
K. Janssens
AFFILIATIONS
Universiteit Antwerpen, 2000 Antwerpen, Belgium
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
N. N. Janthalur
AFFILIATIONS
Directorate of Construction, Services & Estate Management, Mumbai 400094, India
S. Jaraba
AFFILIATIONS
Instituto de Fisica Teorica UAM-CSIC, Universidad Autonoma de Madrid, 28049 Madrid, Spain
P. Jaranowski
AFFILIATIONS
Faculty of Physics, University of Białystok, 15-245 Białystok, Poland
R. Jaume
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
W. Javed
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
A. Jennings
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
W. Jia
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
J. Jiang
AFFILIATIONS
Northeastern University, Boston, MA 02115, USA
S. J. Jin
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
C. Johanson
AFFILIATIONS
University of Massachusetts Dartmouth, North Dartmouth, MA 02747, USA
G. R. Johns
AFFILIATIONS
Christopher Newport University, Newport News, VA 23606, USA
N. A. Johnson
AFFILIATIONS
University of Florida, Gainesville, FL 32611, USA
N. K. Johnson-McDaniel
AFFILIATIONS
The University of Mississippi, University, MS 38677, USA
M. C. Johnston
AFFILIATIONS
University of Nevada, Las Vegas, Las Vegas, NV 89154, USA
R. Johnston
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
N. Johny
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
D. H. Jones
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
D. I. Jones
AFFILIATIONS
University of Southampton, Southampton SO17 1BJ, UK
E. J. Jones
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
R. Jones
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
S. Jose
AFFILIATIONS
Indian Institute of Technology Madras, Chennai 600036, India
P. Joshi
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
S. K. Joshi
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
J. Ju
AFFILIATIONS
Sungkyunkwan University, Seoul 03063, Republic of Korea
L. Ju
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
K. Jung
AFFILIATIONS
Department of Physics, Ulsan National Institute of Science and Technology (UNIST), 50 UNIST-gil, Ulju-gun, Ulsan 44919, Republic of Korea
J. Junker
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
V. Juste
AFFILIATIONS
Université libre de Bruxelles, 1050 Bruxelles, Belgium
H. B. Kabagoz
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
T. Kajita
AFFILIATIONS
Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8582, Japan
I. Kaku
AFFILIATIONS
Department of Physics, Graduate School of Science, Osaka Metropolitan University, 3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka City, Osaka 558-8585, Japan
V. Kalogera
AFFILIATIONS
Northwestern University, Evanston, IL 60208, USA
M. Kalomenopoulos
AFFILIATIONS
University of Nevada, Las Vegas, Las Vegas, NV 89154, USA
M. Kamiizumi
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
N. Kanda
AFFILIATIONS
Nambu Yoichiro Institute of Theoretical and Experimental Physics (NITEP), Osaka Metropolitan University, 3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka City, Osaka 558-8585, Japan
Department of Physics, Graduate School of Science, Osaka Metropolitan University, 3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka City, Osaka 558-8585, Japan
S. Kandhasamy
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
G. Kang
AFFILIATIONS
Chung-Ang University, Seoul 06974, Republic of Korea
N. C. Kannachel
AFFILIATIONS
OzGrav, School of Physics & Astronomy, Monash University, Clayton 3800, Victoria, Australia
J. B. Kanner
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
S. J. Kapadia
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
D. P. Kapasi
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
S. Karat
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
R. Kashyap
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
M. Kasprzack
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
W. Kastaun
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
T. Kato
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8582, Japan
E. Katsavounidis
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
W. Katzman
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
R. Kaushik
AFFILIATIONS
RRCAT, Indore, Madhya Pradesh 452013, India
K. Kawabe
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
R. Kawamoto
AFFILIATIONS
Department of Physics, Graduate School of Science, Osaka Metropolitan University, 3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka City, Osaka 558-8585, Japan
A. Kazemi
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
D. Keitel
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
J. Kennington
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
R. Kesharwani
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
J. S. Key
AFFILIATIONS
University of Washington Bothell, Bothell, WA 98011, USA
R. Khadela
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
S. Khadka
AFFILIATIONS
Stanford University, Stanford, CA 94305, USA
F. Y. Khalili
AFFILIATIONS
Lomonosov Moscow State University, Moscow 119991, Russia
F. Khan
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
I. Khan
AFFILIATIONS
Aix Marseille Univ, CNRS, Centrale Med, Institut Fresnel, F-13013 Marseille, France
Aix Marseille Université, Jardin du Pharo, 58 Boulevard Charles Livon, 13007 Marseille, France
T. Khanam
AFFILIATIONS
Johns Hopkins University, Baltimore, MD 21218, USA
M. Khursheed
AFFILIATIONS
RRCAT, Indore, Madhya Pradesh 452013, India
N. M. Khusid
AFFILIATIONS
Stony Brook University, Stony Brook, NY 11794, USA
Center for Computational Astrophysics, Flatiron Institute, New York, NY 10010, USA
W. Kiendrebeogo
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
Laboratoire de Physique et de Chimie de l’Environnement, Université Joseph KI-ZERBO, 9GH2+3V5, Ouagadougou, Burkina Faso
N. Kijbunchoo
AFFILIATIONS
OzGrav, University of Adelaide, Adelaide, South Australia 5005, Australia
C. Kim
AFFILIATIONS
Ewha Womans University, Seoul 03760, Republic of Korea
J. C. Kim
AFFILIATIONS
Seoul National University, Seoul 08826, Republic of Korea
K. Kim
AFFILIATIONS
Korea Astronomy and Space Science Institute, Daejeon 34055, Republic of Korea
M. H. Kim
AFFILIATIONS
Sungkyunkwan University, Seoul 03063, Republic of Korea
S. Kim
AFFILIATIONS
Department of Astronomy and Space Science, Chungnam National University, 9 Daehak-ro, Yuseong-gu, Daejeon 34134, Republic of Korea
Y.-M. Kim
AFFILIATIONS
Korea Astronomy and Space Science Institute, Daejeon 34055, Republic of Korea
C. Kimball
AFFILIATIONS
Northwestern University, Evanston, IL 60208, USA
M. Kinley-Hanlon
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
M. Kinnear
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
J. S. Kissel
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
S. Klimenko
AFFILIATIONS
University of Florida, Gainesville, FL 32611, USA
A. M. Knee
AFFILIATIONS
University of British Columbia, Vancouver, BC V6T 1Z4, Canada
N. Knust
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
K. Kobayashi
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8582, Japan
P. Koch
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
S. M. Koehlenbeck
AFFILIATIONS
Stanford University, Stanford, CA 94305, USA
G. Koekoek
AFFILIATIONS
Maastricht University, 6200 MD Maastricht, The Netherlands
Nikhef, 1098 XG Amsterdam, The Netherlands
K. Kohri
AFFILIATIONS
Institute of Particle and Nuclear Studies (IPNS), High Energy Accelerator Research Organization (KEK), 1-1 Oho, Tsukuba City, Ibaraki 305-0801, Japan
Division of Science, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan
K. Kokeyama
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
S. Koley
AFFILIATIONS
Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
P. Kolitsidou
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
K. Komori
AFFILIATIONS
Department of Physics, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
University of Tokyo, Tokyo, 113-0033, Japan
A. K. H. Kong
AFFILIATIONS
National Tsing Hua University, Hsinchu City 30013, Taiwan
A. Kontos
AFFILIATIONS
Bard College, Annandale-On-Hudson, NY 12504, USA
M. Korobko
AFFILIATIONS
Universität Hamburg, D-22761 Hamburg, Germany
R. V. Kossak
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
X. Kou
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
A. Koushik
AFFILIATIONS
Universiteit Antwerpen, 2000 Antwerpen, Belgium
N. Kouvatsos
AFFILIATIONS
King’s College London, University of London, London WC2R 2LS, UK
M. Kovalam
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
D. B. Kozak
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
S. L. Kranzhoff
AFFILIATIONS
Maastricht University, 6200 MD Maastricht, The Netherlands
Nikhef, 1098 XG Amsterdam, The Netherlands
V. Kringel
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
N. V. Krishnendu
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
A. Królak
AFFILIATIONS
National Center for Nuclear Research, 05-400 Świerk-Otwock, Poland
Institute of Mathematics, Polish Academy of Sciences, 00656 Warsaw, Poland
K. Kruska
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
J. Kubisz
AFFILIATIONS
Astronomical Observatory, Jagiellonian University, 31-007 Cracow, Poland
G. Kuehn
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
S. Kulkarni
AFFILIATIONS
The University of Mississippi, University, MS 38677, USA
A. Kulur Ramamohan
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
A. Kumar
AFFILIATIONS
Directorate of Construction, Services & Estate Management, Mumbai 400094, India
Praveen Kumar
AFFILIATIONS
IGFAE, Universidade de Santiago de Compostela, 15782, Spain
Prayush Kumar
AFFILIATIONS
International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bengaluru 560089, India
Rahul Kumar
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
Rakesh Kumar
AFFILIATIONS
Institute for Plasma Research, Bhat, Gandhinagar 382428, India
J. Kume
AFFILIATIONS
University of Tokyo, Tokyo, 113-0033, Japan
Department of Physics and Astronomy, University of Padova, Via Marzolo, 8-35151 Padova, Italy
Sezione di Padova, Istituto Nazionale di Fisica Nucleare (INFN), Via Marzolo, 8-35131 Padova, Italy
K. Kuns
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
N. Kuntimaddi
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
S. Kuroyanagi
AFFILIATIONS
Instituto de Fisica Teorica UAM-CSIC, Universidad Autonoma de Madrid, 28049 Madrid, Spain
Department of Physics, Nagoya University, ES building, Furocho, Chikusa-ku, Nagoya, Aichi 464-8602, Japan
S. Kuwahara
AFFILIATIONS
University of Tokyo, Tokyo, 113-0033, Japan
K. Kwak
AFFILIATIONS
Department of Physics, Ulsan National Institute of Science and Technology (UNIST), 50 UNIST-gil, Ulju-gun, Ulsan 44919, Republic of Korea
K. Kwan
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
J. Kwok
AFFILIATIONS
University of Cambridge, Cambridge CB2 1TN, UK
G. Lacaille
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
P. Lagabbe
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
Università di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy
D. Laghi
AFFILIATIONS
L2IT, Laboratoire des 2 Infinis - Toulouse, Université de Toulouse, CNRS/IN2P3, UPS, F-31062 Toulouse Cedex 9, France
S. Lai
AFFILIATIONS
Department of Electrophysics, National Yang Ming Chiao Tung University, 101 University Street, Hsinchu, Taiwan
E. Lalande
AFFILIATIONS
Université de Montréal/Polytechnique, Montreal, QC H3T 1J4, Canada
M. Lalleman
AFFILIATIONS
Universiteit Antwerpen, 2000 Antwerpen, Belgium
P. C. Lalremruati
AFFILIATIONS
Indian Institute of Science Education and Research, Kolkata, Mohanpur, West Bengal 741252, India
M. Landry
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
B. B. Lane
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
R. N. Lang
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
J. Lange
AFFILIATIONS
University of Texas, Austin, TX 78712, USA
R. Langgin
AFFILIATIONS
University of Nevada, Las Vegas, Las Vegas, NV 89154, USA
B. Lantz
AFFILIATIONS
Stanford University, Stanford, CA 94305, USA
A. La Rana
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
I. L. Rosa
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
J. Larsen
AFFILIATIONS
Western Washington University, Bellingham, WA 98225, USA
A. Lartaux-Vollard
AFFILIATIONS
Université Paris-Saclay, CNRS/IN2P3, IJCLab, 91405 Orsay, France
P. D. Lasky
AFFILIATIONS
OzGrav, School of Physics & Astronomy, Monash University, Clayton 3800, Victoria, Australia
J. Lawrence
AFFILIATIONS
The University of Texas Rio Grande Valley, Brownsville, TX 78520, USA
Texas Tech University, Lubbock, TX 79409, USA
M. N. Lawrence
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
M. Laxen
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
C. Lazarte
AFFILIATIONS
Departamento de Astronomía y Astrofísica, Universitat de València, E-46100 Burjassot, València, Spain
A. Lazzarini
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
C. Lazzaro
AFFILIATIONS
INFN Cagliari, Physics Department, Università degli Studi di Cagliari, Cagliari 09042, Italy
Università degli Studi di Cagliari, Via Università 40, 09124 Cagliari, Italy
P. Leaci
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
L. Leali
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
Y. K. Lecoeuche
AFFILIATIONS
University of British Columbia, Vancouver, BC V6T 1Z4, Canada
H. M. Lee
AFFILIATIONS
Seoul National University, Seoul 08826, Republic of Korea
H. W. Lee
AFFILIATIONS
Inje University Gimhae, South Gyeongsang 50834, Republic of Korea
J. Lee
AFFILIATIONS
Syracuse University, Syracuse, NY 13244, USA
K. Lee
AFFILIATIONS
Sungkyunkwan University, Seoul 03063, Republic of Korea
R.-K. Lee
AFFILIATIONS
National Tsing Hua University, Hsinchu City 30013, Taiwan
R. Lee
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
Sungho Lee
AFFILIATIONS
Technology Center for Astronomy and Space Science, Korea Astronomy and Space Science Institute (KASI), 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of Korea
Sunjae Lee
AFFILIATIONS
Sungkyunkwan University, Seoul 03063, Republic of Korea
Y. Lee
AFFILIATIONS
National Central University, Taoyuan City 320317, Taiwan
I. N. Legred
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
J. Lehmann
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
L. Lehner
AFFILIATIONS
Perimeter Institute, Waterloo, ON N2L 2Y5, Canada
M. Le Jean
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, Laboratoire des Matériaux Avancés (LMA), IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
A. Lemaître
AFFILIATIONS
NAVIER, École des Ponts, Univ Gustave Eiffel, CNRS. Marne-la-Vallée, France
M. Lenti
AFFILIATIONS
INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy
Università di Firenze, Sesto Fiorentino I-50019, Italy
M. Leonardi
AFFILIATIONS
Gravitational Wave Science Project, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan
Università di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy
INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy
M. Lequime
AFFILIATIONS
Aix Marseille Univ, CNRS, Centrale Med, Institut Fresnel, F-13013 Marseille, France
N. Leroy
AFFILIATIONS
Université Paris-Saclay, CNRS/IN2P3, IJCLab, 91405 Orsay, France
M. Lesovsky
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
N. Letendre
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
M. Lethuillier
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
Y. Levin
AFFILIATIONS
OzGrav, School of Physics & Astronomy, Monash University, Clayton 3800, Victoria, Australia
K. Leyde
AFFILIATIONS
Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
University of Portsmouth, Portsmouth, PO1 3FX, UK
A. K. Y. Li
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
K. L. Li
AFFILIATIONS
Department of Physics, National Cheng Kung University, No. 1, University Road, Tainan City 701, Taiwan
T. G. F. Li
AFFILIATIONS
Katholieke Universiteit Leuven, Oude Markt 13, 3000 Leuven, Belgium
X. Li
AFFILIATIONS
CaRT, California Institute of Technology, Pasadena, CA 91125, USA
Y. Li
AFFILIATIONS
Northwestern University, Evanston, IL 60208, USA
Z. Li
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
A. Lihos
AFFILIATIONS
Christopher Newport University, Newport News, VA 23606, USA
C-Y. Lin
AFFILIATIONS
National Center for High-Performance Computing, National Applied Research Laboratories, No. 7, R&D 6th Road, Hsinchu Science Park, Hsinchu City 30076, Taiwan
E. T. Lin
AFFILIATIONS
National Tsing Hua University, Hsinchu City 30013, Taiwan
L. C.-C. Lin
AFFILIATIONS
Department of Physics, National Cheng Kung University, No. 1, University Road, Tainan City 701, Taiwan
Y.-C. Lin
AFFILIATIONS
National Tsing Hua University, Hsinchu City 30013, Taiwan
C. Lindsay
AFFILIATIONS
SUPA, University of the West of Scotland, Paisley PA1 2BE, UK
S. D. Linker
AFFILIATIONS
California State University, Los Angeles, Los Angeles, CA 90032, USA
T. B. Littenberg
AFFILIATIONS
NAS. Marshall Space Flight Center, Huntsville, AL 35811, USA
A. Liu
AFFILIATIONS
The Chinese University of Hong Kong, Shatin, NT, Hong Kong
G. C. Liu
AFFILIATIONS
Department of Physics, Tamkang University, No. 151, Yingzhuan Road, Danshui District, New Taipei City 25137, Taiwan
Jian Liu
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
F. Llamas Villarreal
AFFILIATIONS
The University of Texas Rio Grande Valley, Brownsville, TX 78520, USA
J. Llobera-Querol
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
R. K. L. Lo
AFFILIATIONS
Niels Bohr Institute, University of Copenhagen, 2100 Kóbenhavn, Denmark
J.-P. Locquet
AFFILIATIONS
Katholieke Universiteit Leuven, Oude Markt 13, 3000 Leuven, Belgium
M. R. Loizou
AFFILIATIONS
University of Massachusetts Dartmouth, North Dartmouth, MA 02747, USA
L. T. London
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
King’s College London, University of London, London WC2R 2LS, UK
A. Longo
AFFILIATIONS
Università degli Studi di Urbino “Carlo Bo,” I-61029 Urbino, Italy
INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy
D. Lopez
AFFILIATIONS
Université de Liège, B-4000 Liège, Belgium
University of Zurich, Winterthurerstrasse 190, 8057 Zurich, Switzerland
M. Lopez Portilla
AFFILIATIONS
Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, 3584 CC Utrecht, Netherlands
A. Lorenzo-Medina
AFFILIATIONS
IGFAE, Universidade de Santiago de Compostela, 15782, Spain
V. Loriette
AFFILIATIONS
Université Paris-Saclay, CNRS/IN2P3, IJCLab, 91405 Orsay, France
M. Lormand
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
G. Losurdo
AFFILIATIONS
INFN, Sezione di Pisa, I-56127 Pisa, Italy
Scuola Normale Superiore, I-56126 Pisa, Italy
E. Lotti
AFFILIATIONS
University of Massachusetts Dartmouth, North Dartmouth, MA 02747, USA
T. P. Lott IV
AFFILIATIONS
Georgia Institute of Technology, Atlanta, GA 30332, USA
J. D. Lough
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
H. A. Loughlin
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
C. O. Lousto
AFFILIATIONS
Rochester Institute of Technology, Rochester, NY 14623, USA
N. Low
AFFILIATIONS
OzGrav, University of Melbourne, Parkville, Victoria 3010, Australia
M. J. Lowry
AFFILIATIONS
Christopher Newport University, Newport News, VA 23606, USA
N. Lu
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
L. Lucchesi
AFFILIATIONS
INFN, Sezione di Pisa, I-56127 Pisa, Italy
H. Lück
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
D. Lumaca
AFFILIATIONS
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
A. P. Lundgren
AFFILIATIONS
University of Portsmouth, Portsmouth, PO1 3FX, UK
A. W. Lussier
AFFILIATIONS
Université de Montréal/Polytechnique, Montreal, QC H3T 1J4, Canada
L.-T. Ma
AFFILIATIONS
National Tsing Hua University, Hsinchu City 30013, Taiwan
S. Ma
AFFILIATIONS
Perimeter Institute, Waterloo, ON N2L 2Y5, Canada
R. Macas
AFFILIATIONS
University of Portsmouth, Portsmouth, PO1 3FX, UK
A. Macedo
AFFILIATIONS
California State University Fullerton, Fullerton, CA 92831, USA
M. MacInnis
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
R. R. Maciy
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
D. M. Macleod
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
I. A. O. MacMillan
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
A. Macquet
AFFILIATIONS
Université Paris-Saclay, CNRS/IN2P3, IJCLab, 91405 Orsay, France
D. Macri
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
K. Maeda
AFFILIATIONS
Faculty of Science, University of Toyama, 3190 Gofuku, Toyama City, Toyama 930-8555, Japan
S. Maenaut
AFFILIATIONS
Katholieke Universiteit Leuven, Oude Markt 13, 3000 Leuven, Belgium
S. S. Magare
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
R. M. Magee
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
E. Maggio
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
R. Maggiore
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Department of Physics and Astronomy, Vrije Universiteit Amsterdam, 1081 HV Amsterdam, Netherlands
M. Magnozzi
AFFILIATIONS
INFN, Sezione di Genova, I-16146 Genova, Italy
Dipartimento di Fisica, Università degli Studi di Genova, I-16146 Genova, Italy
M. Mahesh
AFFILIATIONS
Universität Hamburg, D-22761 Hamburg, Germany
M. Maini
AFFILIATIONS
University of Rhode Island, Kingston, RI 02881, USA
S. Majhi
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
E. Majorana
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
C. N. Makarem
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
D. Malakar
AFFILIATIONS
Missouri University of Science and Technology, Rolla, MO 65409, USA
J. A. Malaquias-Reis
AFFILIATIONS
Instituto Nacional de Pesquisas Espaciais, 12227-010 São José dos Campos, São Paulo, Brazil
U. Mali
AFFILIATIONS
Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada
S. Maliakal
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
A. Malik
AFFILIATIONS
RRCAT, Indore, Madhya Pradesh 452013, India
L. Mallick
AFFILIATIONS
University of Manitoba, Winnipeg, MB R3T 2N2, Canada
Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada
A. Malz
AFFILIATIONS
Royal Holloway, University of London, London TW20 0EX, UK
N. Man
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
V. Mandic
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
V. Mangano
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
B. Mannix
AFFILIATIONS
University of Oregon, Eugene, OR 97403, USA
G. L. Mansell
AFFILIATIONS
Syracuse University, Syracuse, NY 13244, USA
G. Mansingh
AFFILIATIONS
American University, Washington, DC 20016, USA
M. Manske
AFFILIATIONS
University of Wisconsin–Milwaukee, Milwaukee, WI 53201, USA
M. Mantovani
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
M. Mapelli
AFFILIATIONS
Università di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy
INFN, Sezione di Padova, I-35131 Padova, Italy
Institut fuer Theoretische Astrophysik, Zentrum fuer Astronomie Heidelberg, Universitaet Heidelberg, Albert Ueberle Str. 2, 69120 Heidelberg, Germany
F. Marchesoni
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
Università di Camerino, I-62032 Camerino, Italy
School of Physics Science and Engineering, Tongji University, Shanghai 200092, People’s Republic of China
C. Marinelli
AFFILIATIONS
Università di Siena, I-53100 Siena, Italy
D. Marín Pina
AFFILIATIONS
Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (UB), c. Martí i Franquès, 1, 08028 Barcelona, Spain
Departament de Física Quàntica i Astrofísica (FQA), Universitat de Barcelona (UB), c. Martí i Franqués, 1, 08028 Barcelona, Spain
Institut d’Estudis Espacials de Catalunya, c. Gran Capità, 2-4, 08034 Barcelona, Spain
F. Marion
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
S. Márka
AFFILIATIONS
Columbia University, New York, NY 10027, USA
Z. Márka
AFFILIATIONS
Columbia University, New York, NY 10027, USA
A. S. Markosyan
AFFILIATIONS
Stanford University, Stanford, CA 94305, USA
A. Markowitz
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
E. Maros
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
S. Marsat
AFFILIATIONS
L2IT, Laboratoire des 2 Infinis - Toulouse, Université de Toulouse, CNRS/IN2P3, UPS, F-31062 Toulouse Cedex 9, France
F. Martelli
AFFILIATIONS
Università degli Studi di Urbino “Carlo Bo,” I-61029 Urbino, Italy
INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy
I. W. Martin
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
R. M. Martin
AFFILIATIONS
Montclair State University, Montclair, NJ 07043, USA
B. B. Martinez
AFFILIATIONS
University of Arizona, Tucson, AZ 85721, USA
M. Martinez
AFFILIATIONS
Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra (Barcelona), Spain
Institucio Catalana de Recerca i Estudis Avançats (ICREA), Passeig de Lluís Companys, 23, 08010 Barcelona, Spain
V. Martinez
AFFILIATIONS
Université de Lyon, Université Claude Bernard Lyon 1, CNRS, Institut Lumière Matière, F-69622 Villeurbanne, France
A. Martini
AFFILIATIONS
Università di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy
INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy
J. C. Martins
AFFILIATIONS
Instituto Nacional de Pesquisas Espaciais, 12227-010 São José dos Campos, São Paulo, Brazil
D. V. Martynov
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
E. J. Marx
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
L. Massaro
AFFILIATIONS
Maastricht University, 6200 MD Maastricht, The Netherlands
Nikhef, 1098 XG Amsterdam, The Netherlands
A. Masserot
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
M. Masso-Reid
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
M. Mastrodicasa
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
S. Mastrogiovanni
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
T. Matcovich
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
M. Matiushechkina
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
M. Matsuyama
AFFILIATIONS
Department of Physics, Graduate School of Science, Osaka Metropolitan University, 3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka City, Osaka 558-8585, Japan
N. Mavalvala
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
N. Maxwell
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
G. McCarrol
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
R. McCarthy
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
D. E. McClelland
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
S. McCormick
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
L. McCuller
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
S. McEachin
AFFILIATIONS
Christopher Newport University, Newport News, VA 23606, USA
C. McElhenny
AFFILIATIONS
Christopher Newport University, Newport News, VA 23606, USA
G. I. McGhee
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
J. McGinn
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
K. B. M. McGowan
AFFILIATIONS
Vanderbilt University, Nashville, TN 37235, USA
J. McIver
AFFILIATIONS
University of British Columbia, Vancouver, BC V6T 1Z4, Canada
A. McLeod
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
T. McRae
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
D. Meacher
AFFILIATIONS
University of Wisconsin–Milwaukee, Milwaukee, WI 53201, USA
Q. Meijer
AFFILIATIONS
Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, 3584 CC Utrecht, Netherlands
A. Melatos
AFFILIATIONS
OzGrav, University of Melbourne, Parkville, Victoria 3010, Australia
M. Melching
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
S. Mellaerts
AFFILIATIONS
Katholieke Universiteit Leuven, Oude Markt 13, 3000 Leuven, Belgium
C. S. Menoni
AFFILIATIONS
Colorado State University, Fort Collins, CO 80523, USA
F. Mera
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
R. A. Mercer
AFFILIATIONS
University of Wisconsin–Milwaukee, Milwaukee, WI 53201, USA
L. Mereni
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, Laboratoire des Matériaux Avancés (LMA), IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
K. Merfeld
AFFILIATIONS
Johns Hopkins University, Baltimore, MD 21218, USA
E. L. Merilh
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
J. R. Mérou
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
J. D. Merritt
AFFILIATIONS
University of Oregon, Eugene, OR 97403, USA
M. Merzougui
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
C. Messenger
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
C. Messick
AFFILIATIONS
University of Wisconsin–Milwaukee, Milwaukee, WI 53201, USA
B. Mestichelli
AFFILIATIONS
Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
M. Meyer-Conde
AFFILIATIONS
Research Center for Space Science, Advanced Research Laboratories, Tokyo City University, 3-3-1 Ushikubo-Nishi, Tsuzuki-Ku, Yokohama, Kanagawa 224-8551, Japan
F. Meylahn
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
A. Mhaske
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
A. Miani
AFFILIATIONS
Università di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy
INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy
H. Miao
AFFILIATIONS
Tsinghua University, Beijing 100084, People’S Republic of China
I. Michaloliakos
AFFILIATIONS
University of Florida, Gainesville, FL 32611, USA
C. Michel
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, Laboratoire des Matériaux Avancés (LMA), IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
Y. Michimura
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
University of Tokyo, Tokyo, 113-0033, Japan
H. Middleton
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
S. J. Miller
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
M. Millhouse
AFFILIATIONS
Georgia Institute of Technology, Atlanta, GA 30332, USA
E. Milotti
AFFILIATIONS
INFN, Sezione di Trieste, I-34127 Trieste, Italy
Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy
V. Milotti
AFFILIATIONS
Università di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy
Y. Minenkov
AFFILIATIONS
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
N. Mio
AFFILIATIONS
Institute for Photon Science and Technology, The University of Tokyo, 2-11-16 Yayoi, Bunkyo-ku, Tokyo 113-8656, Japan
Ll. M. Mir
AFFILIATIONS
Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra (Barcelona), Spain
L. Mirasola
AFFILIATIONS
INFN Cagliari, Physics Department, Università degli Studi di Cagliari, Cagliari 09042, Italy
Università degli Studi di Cagliari, Via Università 40, 09124 Cagliari, Italy
M. Miravet-Tenés
AFFILIATIONS
Departamento de Astronomía y Astrofísica, Universitat de València, E-46100 Burjassot, València, Spain
C.-A. Miritescu
AFFILIATIONS
Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra (Barcelona), Spain
A. K. Mishra
AFFILIATIONS
International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bengaluru 560089, India
A. Mishra
AFFILIATIONS
International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bengaluru 560089, India
C. Mishra
AFFILIATIONS
Indian Institute of Technology Madras, Chennai 600036, India
T. Mishra
AFFILIATIONS
University of Florida, Gainesville, FL 32611, USA
A. L. Mitchell
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Department of Physics and Astronomy, Vrije Universiteit Amsterdam, 1081 HV Amsterdam, Netherlands
J. G. Mitchell
AFFILIATIONS
Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA
S. Mitra
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
V. P. Mitrofanov
AFFILIATIONS
Lomonosov Moscow State University, Moscow 119991, Russia
R. Mittleman
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
O. Miyakawa
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
S. Miyamoto
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8582, Japan
S. Miyoki
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
G. Mo
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
L. Mobilia
AFFILIATIONS
Università degli Studi di Urbino “Carlo Bo,” I-61029 Urbino, Italy
INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy
S. R. P. Mohapatra
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
S. R. Mohite
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
M. Molina- Ruiz
AFFILIATIONS
University of California, Berkeley, CA 94720, USA
C. Mondal
AFFILIATIONS
Université de Normandie, ENSICAEN, UNICAEN, CNRS/IN2P3, LPC Caen, F-14000 Caen, France
M. Mondin
AFFILIATIONS
California State University, Los Angeles, Los Angeles, CA 90032, USA
M. Montani
AFFILIATIONS
Università degli Studi di Urbino “Carlo Bo,” I-61029 Urbino, Italy
INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy
C. J. Moore
AFFILIATIONS
University of Cambridge, Cambridge CB2 1TN, UK
D. Moraru
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
A. More
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
S. More
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
E. A. Moreno
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
G. Moreno
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
S. Morisaki
AFFILIATIONS
University of Tokyo, Tokyo, 113-0033, Japan
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8582, Japan
Y. Moriwaki
AFFILIATIONS
Faculty of Science, University of Toyama, 3190 Gofuku, Toyama City, Toyama 930-8555, Japan
G. Morras
AFFILIATIONS
Instituto de Fisica Teorica UAM-CSIC, Universidad Autonoma de Madrid, 28049 Madrid, Spain
A. Moscatello
AFFILIATIONS
Università di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy
M. Mould
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
P. Mourier
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
School of Physical & Chemical Sciences, University of Canterbury, Private Bag 4800, Christchurch 8041, New Zealand
B. Mours
AFFILIATIONS
Université de Strasbourg, CNRS, IPHC UMR 7178, F-67000 Strasbourg, France
C. M. Mow-Lowry
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Department of Physics and Astronomy, Vrije Universiteit Amsterdam, 1081 HV Amsterdam, Netherlands
F. Muciaccia
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
D. Mukherjee
AFFILIATIONS
NAS. Marshall Space Flight Center, Huntsville, AL 35811, USA
Samanwaya Mukherjee
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
Soma Mukherjee
AFFILIATIONS
The University of Texas Rio Grande Valley, Brownsville, TX 78520, USA
Subroto Mukherjee
AFFILIATIONS
Institute for Plasma Research, Bhat, Gandhinagar 382428, India
Suvodip Mukherjee
AFFILIATIONS
Tata Institute of Fundamental Research, Mumbai 400005, India
Perimeter Institute, Waterloo, ON N2L 2Y5, Canada
GRAPPA, Anton Pannekoek Institute for Astronomy and Institute for High-Energy Physics, University of Amsterdam, 1098 XH Amsterdam, The Netherlands
N. Mukund
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
A. Mullavey
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
H. Mullock
AFFILIATIONS
University of British Columbia, Vancouver, BC V6T 1Z4, Canada
J. Munch
AFFILIATIONS
OzGrav, University of Adelaide, Adelaide, South Australia 5005, Australia
J. Mundi
AFFILIATIONS
American University, Washington, DC 20016, USA
C. L. Mungioli
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
Y. Murakami
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8582, Japan
M. Murakoshi
AFFILIATIONS
Department of Physical Sciences, Aoyama Gakuin University, 5-10-1 Fuchinobe, Sagamihara City, Kanagawa 252-5258, Japan
P. G. Murray
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
S. Muusse
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
D. Nabari
AFFILIATIONS
Università di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy
INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy
S. L. Nadji
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
A. Nagar
AFFILIATIONS
INFN Sezione di Torino, I-10125 Torino, Italy
Institut des Hautes Etudes Scientifiques, F-91440 Bures-sur-Yvette, France
N. Nagarajan
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
K. Nakagaki
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
K. Nakamura
AFFILIATIONS
Gravitational Wave Science Project, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan
H. Nakano
AFFILIATIONS
Faculty of Law, Ryukoku University, 67 Fukakusa Tsukamoto-cho, Fushimi-ku, Kyoto City, Kyoto 612-8577, Japan
M. Nakano
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
D. Nanadoumgar-Lacroze
AFFILIATIONS
Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra (Barcelona), Spain
D. Nandi
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
V. Napolano
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
P. Narayan
AFFILIATIONS
The University of Mississippi, University, MS 38677, USA
I. Nardecchia
AFFILIATIONS
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
T. Narikawa
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8582, Japan
H. Narola
AFFILIATIONS
Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, 3584 CC Utrecht, Netherlands
L. Naticchioni
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
R. K. Nayak
AFFILIATIONS
Indian Institute of Science Education and Research, Kolkata, Mohanpur, West Bengal 741252, India
A. Nela
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
A. Nelson
AFFILIATIONS
University of Arizona, Tucson, AZ 85721, USA
T. J. N. Nelson
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
M. Nery
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
A. Neunzert
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
S. Ng
AFFILIATIONS
California State University Fullerton, Fullerton, CA 92831, USA
L. Nguyen Quynh
AFFILIATIONS
Department of Physics and Astronomy, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556, USA
Phenikaa Institute for Advanced Study (PIAS), Phenikaa University, To Huu street Yen Nghia Ward, Ha Dong District, Hanoi, Vietnam
S. A. Nichols
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
A. B. Nielsen
AFFILIATIONS
University of Stavanger, 4021 Stavanger, Norway
G. Nieradka
AFFILIATIONS
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, 00-716, Warsaw, Poland
Y. Nishino
AFFILIATIONS
Gravitational Wave Science Project, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan
Department of Astronomy, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
A. Nishizawa
AFFILIATIONS
Physics Program, Graduate School of Advanced Science and Engineering, Hiroshima University, 1-3-1 Kagamiyama, Higashihiroshima City, Hiroshima 903-0213, Japan
S. Nissanke
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
GRAPPA, Anton Pannekoek Institute for Astronomy and Institute for High-Energy Physics, University of Amsterdam, 1098 XH Amsterdam, The Netherlands
E. Nitoglia
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
W. Niu
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
F. Nocera
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
M. Norman
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
C. North
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
J. Novak
AFFILIATIONS
Centre national de la recherche scientifique, 75016 Paris, France
Observatoire Astronomique de Strasbourg, 11 Rue de l’Université, 67000 Strasbourg, France
Observatoire de Paris, 75014 Paris, France
J. F. Nuño Siles
AFFILIATIONS
Instituto de Fisica Teorica UAM-CSIC, Universidad Autonoma de Madrid, 28049 Madrid, Spain
L. K. Nuttall
AFFILIATIONS
University of Portsmouth, Portsmouth, PO1 3FX, UK
K. Obayashi
AFFILIATIONS
Department of Physical Sciences, Aoyama Gakuin University, 5-10-1 Fuchinobe, Sagamihara City, Kanagawa 252-5258, Japan
J. Oberling
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
J. O’Dell
AFFILIATIONS
Rutherford Appleton Laboratory, Didcot OX11 0DE, UK
M. Oertel
AFFILIATIONS
Centre national de la recherche scientifique, 75016 Paris, France
Observatoire Astronomique de Strasbourg, 11 Rue de l’Université, 67000 Strasbourg, France
Observatoire de Paris, 75014 Paris, France
Laboratoire Univers et Théories, Observatoire de Paris, 92190 Meudon, France
A. Offermans
AFFILIATIONS
Katholieke Universiteit Leuven, Oude Markt 13, 3000 Leuven, Belgium
G. Oganesyan
AFFILIATIONS
Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
INFN, Laboratori Nazionali del Gran Sasso, I-67100 Assergi, Italy
J. J. Oh
AFFILIATIONS
National Institute for Mathematical Sciences, Daejeon 34047, Republic of Korea
K. Oh
AFFILIATIONS
Department of Astronomy and Space Science, Chungnam National University, 9 Daehak-ro, Yuseong-gu, Daejeon 34134, Republic of Korea
T. O’Hanlon
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
M. Ohashi
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
M. Ohkawa
AFFILIATIONS
Faculty of Engineering, Niigata University, 8050 Ikarashi-2-no-cho, Nishi-ku, Niigata City, Niigata 950-2181, Japan
F. Ohme
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
R. Oliveri
AFFILIATIONS
Centre national de la recherche scientifique, 75016 Paris, France
Observatoire de Paris, 75014 Paris, France
Laboratoire Univers et Théories, Observatoire de Paris, 92190 Meudon, France
R. Omer
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
B. O’Neal
AFFILIATIONS
Christopher Newport University, Newport News, VA 23606, USA
K. Oohara
AFFILIATIONS
Graduate School of Science and Technology, Niigata University, 8050 Ikarashi-2-no-cho, Nishi-ku, Niigata City, Niigata 950-2181, Japan
Niigata Study Center, The Open University of Japan, 754 Ichibancho, Asahimachi-dori, Chuo-ku, Niigata City, Niigata 951-8122, Japan
B. O’Reilly
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
R. Oram
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
N. D. Ormsby
AFFILIATIONS
Christopher Newport University, Newport News, VA 23606, USA
M. Orselli
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
Università di Perugia, I-06123 Perugia, Italy
R. O’Shaughnessy
AFFILIATIONS
Rochester Institute of Technology, Rochester, NY 14623, USA
S. O’Shea
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
Y. Oshima
AFFILIATIONS
Department of Physics, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
S. Oshino
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
C. Osthelder
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
I. Ota
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
D. J. Ottaway
AFFILIATIONS
OzGrav, University of Adelaide, Adelaide, South Australia 5005, Australia
A. Ouzriat
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
H. Overmier
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
B. J. Owen
AFFILIATIONS
University of Maryland, Baltimore County, Baltimore, MD 21250, USA
A. E. Pace
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
R. Pagano
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
M. A. Page
AFFILIATIONS
Gravitational Wave Science Project, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan
A. Pai
AFFILIATIONS
Indian Institute of Technology Bombay, Powai, Mumbai 400 076, India
L. Paiella
AFFILIATIONS
Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
A. Pal
AFFILIATIONS
CSIR-Central Glass and Ceramic Research Institute, Kolkata, West Bengal 700032, India
S. Pal
AFFILIATIONS
Indian Institute of Science Education and Research, Kolkata, Mohanpur, West Bengal 741252, India
M. A. Palaia
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
M. Pálfi
AFFILIATIONS
Eötvös University, Budapest 1117, Hungary
P. P. Palma
AFFILIATIONS
Università di Roma Tor Vergata, I-00133 Roma, Italy
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
C. Palomba
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
P. Palud
AFFILIATIONS
Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
J. Pan
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
K. C. Pan
AFFILIATIONS
National Tsing Hua University, Hsinchu City 30013, Taiwan
R. Panai
AFFILIATIONS
Università di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy
INFN Cagliari, Physics Department, Università degli Studi di Cagliari, Cagliari 09042, Italy
P. K. Panda
AFFILIATIONS
Directorate of Construction, Services & Estate Management, Mumbai 400094, India
Shiksha Pandey
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
Swadha Pandey
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
P. T. H. Pang
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, 3584 CC Utrecht, Netherlands
F. Pannarale
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
K. A. Pannone
AFFILIATIONS
California State University Fullerton, Fullerton, CA 92831, USA
B. C. Pant
AFFILIATIONS
RRCAT, Indore, Madhya Pradesh 452013, India
F. H. Panther
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
F. Paoletti
AFFILIATIONS
INFN, Sezione di Pisa, I-56127 Pisa, Italy
A. Paolone
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Consiglio Nazionale delle Ricerche - Istituto dei Sistemi Complessi, I-00185 Roma, Italy
A. Papadopoulos
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
E. E. Papalexakis
AFFILIATIONS
University of California, Riverside, Riverside, CA 92521, USA
L. Papalini
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
G. Papigkiotis
AFFILIATIONS
Department of Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece
A. Paquis
AFFILIATIONS
Université Paris-Saclay, CNRS/IN2P3, IJCLab, 91405 Orsay, France
A. Parisi
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
Università di Perugia, I-06123 Perugia, Italy
B.-J. Park
AFFILIATIONS
Technology Center for Astronomy and Space Science, Korea Astronomy and Space Science Institute (KASI), 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of Korea
J. Park
AFFILIATIONS
Department of Astronomy, Yonsei University, 50 Yonsei-Ro, Seodaemun-Gu, Seoul 03722, Republic of Korea
W. Parker
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
G. Pascale
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
D. Pascucci
AFFILIATIONS
Universiteit Gent, B-9000 Gent, Belgium
A. Pasqualetti
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
R. Passaquieti
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
L. Passenger
AFFILIATIONS
OzGrav, School of Physics & Astronomy, Monash University, Clayton 3800, Victoria, Australia
D. Passuello
AFFILIATIONS
INFN, Sezione di Pisa, I-56127 Pisa, Italy
O. Patane
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
D. Pathak
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
L. Pathak
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
A. Patra
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
B. Patricelli
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
A. S. Patron
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
B. G. Patterson
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
K. Paul
AFFILIATIONS
Indian Institute of Technology Madras, Chennai 600036, India
S. Paul
AFFILIATIONS
University of Oregon, Eugene, OR 97403, USA
E. Payne
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
T. Pearce
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
M. Pedraza
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
A. Pele
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
F. E. Pe na Arellano
AFFILIATIONS
Department of Physics, University of Guadalajara, Av. Revolucion 1500, Colonia Olimpica C.P. 44430, Guadalajara, Jalisco, Mexico
S. Penn
AFFILIATIONS
Hobart and William Smith Colleges, Geneva, NY 14456, USA
M. D. Penuliar
AFFILIATIONS
California State University Fullerton, Fullerton, CA 92831, USA
A. Perego
AFFILIATIONS
Università di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy
INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy
Z. Pereira
AFFILIATIONS
University of Massachusetts Dartmouth, North Dartmouth, MA 02747, USA
J. J. Perez
AFFILIATIONS
University of Florida, Gainesville, FL 32611, USA
C. Périgois
AFFILIATIONS
Università di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy
INFN, Sezione di Padova, I-35131 Padova, Italy
INAF, Osservatorio Astronomico di Padova, I-35122 Padova, Italy
G. Perna
AFFILIATIONS
Università di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy
A. Perreca
AFFILIATIONS
Università di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy
INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy
J. Perret
AFFILIATIONS
Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
S. Perriès
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
J. W. Perry
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Department of Physics and Astronomy, Vrije Universiteit Amsterdam, 1081 HV Amsterdam, Netherlands
D. Pesios
AFFILIATIONS
Department of Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece
S. Petracca
AFFILIATIONS
University of Sannio at Benevento, I-82100 Benevento, Italy and INFN, Sezione di Napoli, I-80100 Napoli, Italy
C. Petrillo
AFFILIATIONS
Università di Perugia, I-06123 Perugia, Italy
H. P. Pfeiffer
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
H. Pham
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
K. A. Pham
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
K. S. Phukon
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
H. Phurailatpam
AFFILIATIONS
The Chinese University of Hong Kong, Shatin, NT, Hong Kong
M. Piarulli
AFFILIATIONS
L2IT, Laboratoire des 2 Infinis - Toulouse, Université de Toulouse, CNRS/IN2P3, UPS, F-31062 Toulouse Cedex 9, France
L. Piccari
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
O. J. Piccinni
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
M. Pichot
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
M. Piendibene
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
F. Piergiovanni
AFFILIATIONS
Università degli Studi di Urbino “Carlo Bo,” I-61029 Urbino, Italy
INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy
L. Pierini
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
G. Pierra
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
V. Pierro
AFFILIATIONS
INFN, Sezione di Napoli, Gruppo Collegato di Salerno, I-80126 Napoli, Italy
Dipartimento di Ingegneria, Università del Sannio, I-82100 Benevento, Italy
M. Pietrzak
AFFILIATIONS
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, 00-716, Warsaw, Poland
M. Pillas
AFFILIATIONS
Université de Liège, B-4000 Liège, Belgium
F. Pilo
AFFILIATIONS
INFN, Sezione di Pisa, I-56127 Pisa, Italy
L. Pinard
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, Laboratoire des Matériaux Avancés (LMA), IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
I. M. Pinto
AFFILIATIONS
Università di Napoli “Federico II,” I-80126 Napoli, Italy
INFN, Sezione di Napoli, Gruppo Collegato di Salerno, I-80126 Napoli, Italy
Dipartimento di Ingegneria, Università del Sannio, I-82100 Benevento, Italy
Museo Storico della Fisica e Centro Studi e Ricerche “Enrico Fermi,” I-00184 Roma, Italy
M. Pinto
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
B. J. Piotrzkowski
AFFILIATIONS
University of Wisconsin–Milwaukee, Milwaukee, WI 53201, USA
M. Pirello
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
M. D. Pitkin
AFFILIATIONS
University of Cambridge, Cambridge CB2 1TN, UK
University of Lancaster, Lancaster LA1 4YW, UK
A. Placidi
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
E. Placidi
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
M. L. Planas
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
W. Plastino
AFFILIATIONS
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
Dipartimento di Ingegneria Industriale, Elettronica e Meccanica, Università degli Studi Roma Tre, I-00146 Roma, Italy
C. Plunkett
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
R. Poggiani
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
E. Polini
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
L. Pompili
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
J. Poon
AFFILIATIONS
The Chinese University of Hong Kong, Shatin, NT, Hong Kong
E. Porcelli
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
E. K. Porter
AFFILIATIONS
Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
C. Posnansky
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
R. Poulton
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
J. Powell
AFFILIATIONS
OzGrav, Swinburne University of Technology, Hawthorn VIC 3122, Australia
M. Pracchia
AFFILIATIONS
Université de Liège, B-4000 Liège, Belgium
B. K. Pradhan
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
T. Pradier
AFFILIATIONS
Université de Strasbourg, CNRS, IPHC UMR 7178, F-67000 Strasbourg, France
A. K. Prajapati
AFFILIATIONS
Institute for Plasma Research, Bhat, Gandhinagar 382428, India
K. Prasai
AFFILIATIONS
Stanford University, Stanford, CA 94305, USA
R. Prasanna
AFFILIATIONS
Directorate of Construction, Services & Estate Management, Mumbai 400094, India
P. Prasia
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
G. Pratten
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
G. Principe
AFFILIATIONS
INFN, Sezione di Trieste, I-34127 Trieste, Italy
Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy
M. Principe
AFFILIATIONS
University of Sannio at Benevento, I-82100 Benevento, Italy and INFN, Sezione di Napoli, I-80100 Napoli, Italy
G. A. Prodi
AFFILIATIONS
Università di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy
INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy
L. Prokhorov
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
P. Prosperi
AFFILIATIONS
INFN, Sezione di Pisa, I-56127 Pisa, Italy
P. Prosposito
AFFILIATIONS
Università di Roma Tor Vergata, I-00133 Roma, Italy
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
A. C. Providence
AFFILIATIONS
Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA
A. Puecher
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, 3584 CC Utrecht, Netherlands
J. Pullin
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
M. Punturo
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
P. Puppo
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
M. Pürrer
AFFILIATIONS
University of Rhode Island, Kingston, RI 02881, USA
H. Qi
AFFILIATIONS
Queen Mary University of London, London E1 4NS, UK
J. Qin
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
G. Quéméner
AFFILIATIONS
Centre national de la recherche scientifique, 75016 Paris, France
Laboratoire de Physique Corpusculaire Caen, 6 boulevard du maréchal Juin, F-14050 Caen, France
V. Quetschke
AFFILIATIONS
The University of Texas Rio Grande Valley, Brownsville, TX 78520, USA
P. J. Quinonez
AFFILIATIONS
Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA
F. J. Raab
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
I. Rainho
AFFILIATIONS
Departamento de Astronomía y Astrofísica, Universitat de València, E-46100 Burjassot, València, Spain
S. Raja
AFFILIATIONS
RRCAT, Indore, Madhya Pradesh 452013, India
C. Rajan
AFFILIATIONS
RRCAT, Indore, Madhya Pradesh 452013, India
B. Rajbhandari
AFFILIATIONS
Rochester Institute of Technology, Rochester, NY 14623, USA
K. E. Ramirez
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
F. A. Ramis Vidal
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
A. Ramos-Buades
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
Nikhef, 1098 XG Amsterdam, The Netherlands
D. Rana
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
S. Ranjan
AFFILIATIONS
Georgia Institute of Technology, Atlanta, GA 30332, USA
K. Ransom
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
P. Rapagnani
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
B. Ratto
AFFILIATIONS
Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA
A. Ray
AFFILIATIONS
University of Wisconsin–Milwaukee, Milwaukee, WI 53201, USA
V. Raymond
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
M. Razzano
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
J. Read
AFFILIATIONS
California State University Fullerton, Fullerton, CA 92831, USA
M. Recaman Payo
AFFILIATIONS
Katholieke Universiteit Leuven, Oude Markt 13, 3000 Leuven, Belgium
T. Regimbau
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
L. Rei
AFFILIATIONS
INFN, Sezione di Genova, I-16146 Genova, Italy
S. Reid
AFFILIATIONS
SUPA, University of Strathclyde, Glasgow G1 1XQ, UK
D. H. Reitze
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
P. Relton
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
A. I. Renzini
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
Università degli Studi di Milano-Bicocca, I-20126 Milano, Italy
B. Revenu
AFFILIATIONS
Université Paris-Saclay, CNRS/IN2P3, IJCLab, 91405 Orsay, France
Subatech, CNRS/IN2P3 - IMT Atlantique - Nantes Université, 4 rue Alfred Kastler BP 20722 44307 Nantes CÉDEX 03, France
R. Reyes
AFFILIATIONS
California State University, Los Angeles, Los Angeles, CA 90032, USA
A. S. Rezaei
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
F. Ricci
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
M. Ricci
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
A. Ricciardone
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
J. W. Richardson
AFFILIATIONS
University of California, Riverside, Riverside, CA 92521, USA
M. Richardson
AFFILIATIONS
OzGrav, University of Adelaide, Adelaide, South Australia 5005, Australia
A. Rijal
AFFILIATIONS
Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA
K. Riles
AFFILIATIONS
University of Michigan, Ann Arbor, MI 48109, USA
H. K. Riley
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
S. Rinaldi
AFFILIATIONS
Università di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy
Institut fuer Theoretische Astrophysik, Zentrum fuer Astronomie Heidelberg, Universitaet Heidelberg, Albert Ueberle Str. 2, 69120 Heidelberg, Germany
J. Rittmeyer
AFFILIATIONS
Universität Hamburg, D-22761 Hamburg, Germany
C. Robertson
AFFILIATIONS
Rutherford Appleton Laboratory, Didcot OX11 0DE, UK
F. Robinet
AFFILIATIONS
Université Paris-Saclay, CNRS/IN2P3, IJCLab, 91405 Orsay, France
M. Robinson
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
A. Rocchi
AFFILIATIONS
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
L. Rolland
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
J. G. Rollins
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
A. E. Romano
AFFILIATIONS
Universidad de Antioquia, Medellín, Colombia
R. Romano
AFFILIATIONS
Dipartimento di Farmacia, Università di Salerno, I-84084 Fisciano, Salerno, Italy
INFN, Sezione di Napoli, I-80126 Napoli, Italy
A. Romero
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
I. M. Romero-Shaw
AFFILIATIONS
University of Cambridge, Cambridge CB2 1TN, UK
J. H. Romie
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
S. Ronchini
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
INFN, Laboratori Nazionali del Gran Sasso, I-67100 Assergi, Italy
T. J. Roocke
AFFILIATIONS
OzGrav, University of Adelaide, Adelaide, South Australia 5005, Australia
L. Rosa
AFFILIATIONS
INFN, Sezione di Napoli, I-80126 Napoli, Italy
Università di Napoli “Federico II,” I-80126 Napoli, Italy
T. J. Rosauer
AFFILIATIONS
University of California, Riverside, Riverside, CA 92521, USA
C. A. Rose
AFFILIATIONS
Georgia Institute of Technology, Atlanta, GA 30332, USA
D. Rosińska
AFFILIATIONS
Astronomical Observatory Warsaw University, 00-478 Warsaw, Poland
M. P. Ross
AFFILIATIONS
University of Washington, Seattle, WA 98195, USA
M. Rossello-Sastre
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
S. Rowan
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
S. Roy
AFFILIATIONS
Université catholique de Louvain, B-1348 Louvain-la-Neuve, Belgium
S. K. Roy
AFFILIATIONS
Stony Brook University, Stony Brook, NY 11794, USA
Center for Computational Astrophysics, Flatiron Institute, New York, NY 10010, USA
D. Rozza
AFFILIATIONS
Università degli Studi di Milano-Bicocca, I-20126 Milano, Italy
INFN, Sezione di Milano-Bicocca, I-20126 Milano, Italy
P. Ruggi
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
N. Ruhama
AFFILIATIONS
Department of Physics, Ulsan National Institute of Science and Technology (UNIST), 50 UNIST-gil, Ulju-gun, Ulsan 44919, Republic of Korea
E. Ruiz Morales
AFFILIATIONS
Instituto de Fisica Teorica UAM-CSIC, Universidad Autonoma de Madrid, 28049 Madrid, Spain
Departamento de Física - ETSIDI, Universidad Politécnica de Madrid, 28012 Madrid, Spain
K. Ruiz-Rocha
AFFILIATIONS
Vanderbilt University, Nashville, TN 37235, USA
S. Sachdev
AFFILIATIONS
Georgia Institute of Technology, Atlanta, GA 30332, USA
T. Sadecki
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
J. Sadiq
AFFILIATIONS
IGFAE, Universidade de Santiago de Compostela, 15782, Spain
P. Saffarieh
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Department of Physics and Astronomy, Vrije Universiteit Amsterdam, 1081 HV Amsterdam, Netherlands
S. Safi-Harb
AFFILIATIONS
University of Manitoba, Winnipeg, MB R3T 2N2, Canada
M. R. Sah
AFFILIATIONS
Tata Institute of Fundamental Research, Mumbai 400005, India
S. Saha
AFFILIATIONS
National Tsing Hua University, Hsinchu City 30013, Taiwan
T. Sainrat
AFFILIATIONS
Université de Strasbourg, CNRS, IPHC UMR 7178, F-67000 Strasbourg, France
S. Sajith Menon
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
Ariel University, Ramat HaGolan St 65, Ari’el, Israel
K. Sakai
AFFILIATIONS
Department of Electronic Control Engineering, National Institute of Technology, Nagaoka College, 888 Nishikatakai, Nagaoka City, Niigata 940-8532, Japan
M. Sakellariadou
AFFILIATIONS
King’s College London, University of London, London WC2R 2LS, UK
S. Sakon
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
O. S. Salafia
AFFILIATIONS
Università degli Studi di Milano-Bicocca, I-20126 Milano, Italy
INFN, Sezione di Milano-Bicocca, I-20126 Milano, Italy
INAF, Osservatorio Astronomico di Brera sede di Merate, I-23807 Merate, Lecco, Italy
F. Salces-Carcoba
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
L. Salconi
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
M. Saleem
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
F. Salemi
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
M. Sallé
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
S. U. Salunkhe
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
S. Salvador
AFFILIATIONS
Université de Normandie, ENSICAEN, UNICAEN, CNRS/IN2P3, LPC Caen, F-14000 Caen, France
Laboratoire de Physique Corpusculaire Caen, 6 boulevard du maréchal Juin, F-14050 Caen, France
A. Samajdar
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, 3584 CC Utrecht, Netherlands
A. Sanchez
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
E. J. Sanchez
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
J. H. Sanchez
AFFILIATIONS
Northwestern University, Evanston, IL 60208, USA
L. E. Sanchez
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
N. Sanchis-Gual
AFFILIATIONS
Departamento de Astronomía y Astrofísica, Universitat de València, E-46100 Burjassot, València, Spain
J. R. Sanders
AFFILIATIONS
Marquette University, Milwaukee, WI 53233, USA
E. M. Sänger
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
F. Santoliquido
AFFILIATIONS
Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
F. Sarandrea
AFFILIATIONS
INFN Sezione di Torino, I-10125 Torino, Italy
T. R. Saravanan
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
N. Sarin
AFFILIATIONS
OzGrav, School of Physics & Astronomy, Monash University, Clayton 3800, Victoria, Australia
P. Sarkar
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
S. Sasaoka
AFFILIATIONS
Graduate School of Science, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan
A. Sasli
AFFILIATIONS
Department of Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece
P. Sassi
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
Università di Perugia, I-06123 Perugia, Italy
B. Sassolas
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, Laboratoire des Matériaux Avancés (LMA), IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
B. S. Sathyaprakash
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
Cardiff University, Cardiff CF24 3AA, UK
R. Sato
AFFILIATIONS
Faculty of Engineering, Niigata University, 8050 Ikarashi-2-no-cho, Nishi-ku, Niigata City, Niigata 950-2181, Japan
Y. Sato
AFFILIATIONS
Faculty of Science, University of Toyama, 3190 Gofuku, Toyama City, Toyama 930-8555, Japan
O. Sauter
AFFILIATIONS
University of Florida, Gainesville, FL 32611, USA
R. L. Savage
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
T. Sawada
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
H. L. Sawant
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
S. Sayah
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
V. Scacco
AFFILIATIONS
Università di Roma Tor Vergata, I-00133 Roma, Italy
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
D. Schaetzl
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
M. Scheel
AFFILIATIONS
CaRT, California Institute of Technology, Pasadena, CA 91125, USA
A. Schiebelbein
AFFILIATIONS
Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada
M. G. Schiworski
AFFILIATIONS
Syracuse University, Syracuse, NY 13244, USA
P. Schmidt
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
S. Schmidt
AFFILIATIONS
Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, 3584 CC Utrecht, Netherlands
R. Schnabel
AFFILIATIONS
Universität Hamburg, D-22761 Hamburg, Germany
M. Schneewind
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
R. M. S. Schofield
AFFILIATIONS
University of Oregon, Eugene, OR 97403, USA
K. Schouteden
AFFILIATIONS
Katholieke Universiteit Leuven, Oude Markt 13, 3000 Leuven, Belgium
B. W. Schulte
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
B. F. Schutz
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
Cardiff University, Cardiff CF24 3AA, UK
E. Schwartz
AFFILIATIONS
Stanford University, Stanford, CA 94305, USA
M. Scialpi
AFFILIATIONS
Dipartimento di Fisica e Scienze della Terra, Università Degli Studi di Ferrara, Via Saragat, 1, 44121 Ferrara FE, Italy
J. Scott
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
S. M. Scott
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
R. M. Sedas
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
T. C. Seetharamu
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
M. Seglar-Arroyo
AFFILIATIONS
Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra (Barcelona), Spain
Y. Sekiguchi
AFFILIATIONS
Faculty of Science, Toho University, 2-2-1 Miyama, Funabashi City, Chiba 274-8510, Japan
D. Sellers
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
A. S. Sengupta
AFFILIATIONS
Indian Institute of Technology, Palaj, Gandhinagar, Gujarat 382355, India
D. Sentenac
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
E. G. Seo
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
J. W. Seo
AFFILIATIONS
Katholieke Universiteit Leuven, Oude Markt 13, 3000 Leuven, Belgium
V. Sequino
AFFILIATIONS
INFN, Sezione di Napoli, I-80126 Napoli, Italy
Università di Napoli “Federico II,” I-80126 Napoli, Italy
M. Serra
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
G. Servignat
AFFILIATIONS
Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
Laboratoire Univers et Théories, Observatoire de Paris, 92190 Meudon, France
A. Sevrin
AFFILIATIONS
Vrije Universiteit Brussel, 1050 Brussel, Belgium
T. Shaffer
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
U. S. Shah
AFFILIATIONS
Georgia Institute of Technology, Atlanta, GA 30332, USA
M. S. Shahriar
AFFILIATIONS
Northwestern University, Evanston, IL 60208, USA
M. A. Shaikh
AFFILIATIONS
Seoul National University, Seoul 08826, Republic of Korea
L. Shao
AFFILIATIONS
Kavli Institute for Astronomy and Astrophysics, Peking University, Yiheyuan Road 5, Haidian District, Beijing 100871, People’s Republic of China
A. Sharma
AFFILIATIONS
Indian Institute of Technology, Palaj, Gandhinagar, Gujarat 382355, India
A. K. Sharma
AFFILIATIONS
International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bengaluru 560089, India
P. Sharma
AFFILIATIONS
RRCAT, Indore, Madhya Pradesh 452013, India
S. Sharma Chaudhary
AFFILIATIONS
Missouri University of Science and Technology, Rolla, MO 65409, USA
M. R. Shaw
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
P. Shawhan
AFFILIATIONS
University of Maryland, College Park, MD 20742, USA
N. S. Shcheblanov
AFFILIATIONS
NAVIER, École des Ponts, Univ Gustave Eiffel, CNRS. Marne-la-Vallée, France
Laboratoire MSME, Cité Descartes, 5 Boulevard Descartes, Champs-sur-Marne, 77454 Marne-la-Vallée Cedex 2, France
Y. Shikano
AFFILIATIONS
University of Tsukuba, 1-1-1, Tennodai, Tsukuba, Ibaraki 305-8573, Japan
Institute for Quantum Studies, Chapman University, 1 University Drive, Orange, CA 92866, USA
M. Shikauchi
AFFILIATIONS
University of Tokyo, Tokyo, 113-0033, Japan
K. Shimode
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
H. Shinkai
AFFILIATIONS
Faculty of Information Science and Technology, Osaka Institute of Technology, 1-79-1 Kitayama, Hirakata City, Osaka 573-0196, Japan
J. Shiota
AFFILIATIONS
Department of Physical Sciences, Aoyama Gakuin University, 5-10-1 Fuchinobe, Sagamihara City, Kanagawa 252-5258, Japan
S. Shirke
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
D. H. Shoemaker
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
D. M. Shoemaker
AFFILIATIONS
University of Texas, Austin, TX 78712, USA
R. W. Short
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
S. ShyamSundar
AFFILIATIONS
RRCAT, Indore, Madhya Pradesh 452013, India
A. Sider
AFFILIATIONS
Université Libre de Bruxelles, Brussels 1050, Belgium
H. Siegel
AFFILIATIONS
Stony Brook University, Stony Brook, NY 11794, USA
Center for Computational Astrophysics, Flatiron Institute, New York, NY 10010, USA
D. Sigg
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
L. Silenzi
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
Università di Camerino, I-62032 Camerino, Italy
M. Simmonds
AFFILIATIONS
OzGrav, University of Adelaide, Adelaide, South Australia 5005, Australia
L. P. Singer
AFFILIATIONS
NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
A. Singh
AFFILIATIONS
The University of Mississippi, University, MS 38677, USA
D. Singh
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
M. K. Singh
AFFILIATIONS
International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bengaluru 560089, India
N. Singh
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
S. Singh
AFFILIATIONS
Astronomical course, The Graduate University for Advanced Studies (SOKENDAI), 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan
Graduate School of Science, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan
A. Singha
AFFILIATIONS
Maastricht University, 6200 MD Maastricht, The Netherlands
Nikhef, 1098 XG Amsterdam, The Netherlands
A. M. Sintes
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
V. Sipala
AFFILIATIONS
INFN Cagliari, Physics Department, Università degli Studi di Cagliari, Cagliari 09042, Italy
Università degli Studi di Sassari, I-07100 Sassari, Italy
V. Skliris
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
B. J. J. Slagmolen
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
D. A. Slater
AFFILIATIONS
Western Washington University, Bellingham, WA 98225, USA
T. J. Slaven-Blair
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
J. Smetana
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
J. R. Smith
AFFILIATIONS
California State University Fullerton, Fullerton, CA 92831, USA
L. Smith
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy
R. J. E. Smith
AFFILIATIONS
OzGrav, School of Physics & Astronomy, Monash University, Clayton 3800, Victoria, Australia
W. J. Smith
AFFILIATIONS
Vanderbilt University, Nashville, TN 37235, USA
K. Somiya
AFFILIATIONS
Graduate School of Science, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan
I. Song
AFFILIATIONS
National Tsing Hua University, Hsinchu City 30013, Taiwan
K. Soni
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
S. Soni
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
V. Sordini
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
F. Sorrentino
AFFILIATIONS
INFN, Sezione di Genova, I-16146 Genova, Italy
H. Sotani
AFFILIATIONS
iTHEMS (Interdisciplinary Theoretical and Mathematical Sciences Program), RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan
A. Southgate
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
F. Spada
AFFILIATIONS
INFN, Sezione di Pisa, I-56127 Pisa, Italy
V. Spagnuolo
AFFILIATIONS
Maastricht University, 6200 MD Maastricht, The Netherlands
Nikhef, 1098 XG Amsterdam, The Netherlands
A. P. Spencer
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
M. Spera
AFFILIATIONS
INFN, Sezione di Trieste, I-34127 Trieste, Italy
Scuola Internazionale Superiore di Studi Avanzati, Via Bonomea, 265, I-34136, Trieste TS, Italy
P. Spinicelli
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
C. A. Sprague
AFFILIATIONS
Department of Physics and Astronomy, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556, USA
A. K. Srivastava
AFFILIATIONS
Institute for Plasma Research, Bhat, Gandhinagar 382428, India
F. Stachurski
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
D. A. Steer
AFFILIATIONS
Laboratoire de Physique de l’École Normale Supérieure, ENS, (CNRS, Université PSL, Sorbonne Université, Université Paris Cité), F-75005 Paris, France
N. Steinle
AFFILIATIONS
University of Manitoba, Winnipeg, MB R3T 2N2, Canada
J. Steinlechner
AFFILIATIONS
Maastricht University, 6200 MD Maastricht, The Netherlands
Nikhef, 1098 XG Amsterdam, The Netherlands
S. Steinlechner
AFFILIATIONS
Maastricht University, 6200 MD Maastricht, The Netherlands
Nikhef, 1098 XG Amsterdam, The Netherlands
N. Stergioulas
AFFILIATIONS
Department of Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece
P. Stevens
AFFILIATIONS
Université Paris-Saclay, CNRS/IN2P3, IJCLab, 91405 Orsay, France
S. P. Stevenson
AFFILIATIONS
OzGrav, Swinburne University of Technology, Hawthorn VIC 3122, Australia
F. Stolzi
AFFILIATIONS
Università di Siena, I-53100 Siena, Italy
M. StPierre
AFFILIATIONS
University of Rhode Island, Kingston, RI 02881, USA
G. Stratta
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Istituto di Astrofisica e Planetologia Spaziali di Roma, 00133 Roma, Italy
Institut für Theoretische Physik, Johann Wolfgang Goethe-Universität, Max-von-Laue-Str. 1, 60438 Frankfurt am Main, Germany
INAF, Osservatorio di Astrofisica e Scienza dello Spazio, I-40129 Bologna, Italy
M. D. Strong
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
A. Strunk
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
R. Sturani
AFFILIATIONS
Universidade Estadual Paulista, 01140-070 São Paulo, Brazil
A. L. Stuver
AFFILIATIONS
Villanova University, Villanova, PA 19085, USA
Author notes
Deceased, 2024 September.
M. Suchenek
AFFILIATIONS
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, 00-716, Warsaw, Poland
S. Sudhagar
AFFILIATIONS
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, 00-716, Warsaw, Poland
N. Sueltmann
AFFILIATIONS
Universität Hamburg, D-22761 Hamburg, Germany
L. Suleiman
AFFILIATIONS
California State University Fullerton, Fullerton, CA 92831, USA
J.M. Sullivan
AFFILIATIONS
Georgia Institute of Technology, Atlanta, GA 30332, USA
K. D. Sullivan
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
J. Sun
AFFILIATIONS
Chung-Ang University, Seoul 06974, Republic of Korea
L. Sun
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
S. Sunil
AFFILIATIONS
Institute for Plasma Research, Bhat, Gandhinagar 382428, India
J. Suresh
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
B. J. Sutton
AFFILIATIONS
King’s College London, University of London, London WC2R 2LS, UK
P. J. Sutton
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
T. Suzuki
AFFILIATIONS
Faculty of Engineering, Niigata University, 8050 Ikarashi-2-no-cho, Nishi-ku, Niigata City, Niigata 950-2181, Japan
Y. Suzuki
AFFILIATIONS
Department of Physical Sciences, Aoyama Gakuin University, 5-10-1 Fuchinobe, Sagamihara City, Kanagawa 252-5258, Japan
B. L. Swinkels
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
A. Syx
AFFILIATIONS
Université de Strasbourg, CNRS, IPHC UMR 7178, F-67000 Strasbourg, France
M. J. Szczepańczyk
AFFILIATIONS
University of Florida, Gainesville, FL 32611, USA
Faculty of Physics, University of Warsaw, Ludwika Pasteura 5, 02-093 Warszawa, Poland
P. Szewczyk
AFFILIATIONS
Astronomical Observatory Warsaw University, 00-478 Warsaw, Poland
M. Tacca
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
H. Tagoshi
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8582, Japan
S. C. Tait
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
H. Takahashi
AFFILIATIONS
Research Center for Space Science, Advanced Research Laboratories, Tokyo City University, 3-3-1 Ushikubo-Nishi, Tsuzuki-Ku, Yokohama, Kanagawa 224-8551, Japan
R. Takahashi
AFFILIATIONS
Gravitational Wave Science Project, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan
A. Takamori
AFFILIATIONS
Earthquake Research Institute, The University of Tokyo, 1-1-1 Yayoi, Bunkyo-ku, Tokyo 113-0032, Japan
T. Takase
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
K. Takatani
AFFILIATIONS
Department of Physics, Graduate School of Science, Osaka Metropolitan University, 3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka City, Osaka 558-8585, Japan
H. Takeda
AFFILIATIONS
Department of Physics, Kyoto University, Kita-Shirakawa Oiwake-cho, Sakyou-ku, Kyoto City, Kyoto 606-8502, Japan
K. Takeshita
AFFILIATIONS
Graduate School of Science, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan
C. Talbot
AFFILIATIONS
University of Chicago, Chicago, IL 60637, USA
M. Tamaki
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8582, Japan
N. Tamanini
AFFILIATIONS
L2IT, Laboratoire des 2 Infinis - Toulouse, Université de Toulouse, CNRS/IN2P3, UPS, F-31062 Toulouse Cedex 9, France
D. Tanabe
AFFILIATIONS
National Central University, Taoyuan City 320317, Taiwan
K. Tanaka
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
S. J. Tanaka
AFFILIATIONS
Department of Physical Sciences, Aoyama Gakuin University, 5-10-1 Fuchinobe, Sagamihara City, Kanagawa 252-5258, Japan
T. Tanaka
AFFILIATIONS
Department of Physics, Kyoto University, Kita-Shirakawa Oiwake-cho, Sakyou-ku, Kyoto City, Kyoto 606-8502, Japan
D. Tang
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
S. Tanioka
AFFILIATIONS
Syracuse University, Syracuse, NY 13244, USA
D. B. Tanner
AFFILIATIONS
University of Florida, Gainesville, FL 32611, USA
W. Tanner
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
L. Tao
AFFILIATIONS
University of California, Riverside, Riverside, CA 92521, USA
R. D. Tapia
AFFILIATIONS
The Pennsylvania State University, University Park, PA 16802, USA
E. N. Tapia San Martín
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
R. Tarafder
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
C. Taranto
AFFILIATIONS
Università di Roma Tor Vergata, I-00133 Roma, Italy
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
A. Taruya
AFFILIATIONS
Yukawa Institute for Theoretical Physics (YITP), Kyoto University, Kita-Shirakawa Oiwake-cho, Sakyou-ku, Kyoto City, Kyoto 606-8502, Japan
J. D. Tasson
AFFILIATIONS
Carleton College, Northfield, MN 55057, USA
J. G. Tau
AFFILIATIONS
Rochester Institute of Technology, Rochester, NY 14623, USA
R. Tenorio
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
H. Themann
AFFILIATIONS
California State University, Los Angeles, Los Angeles, CA 90032, USA
A. Theodoropoulos
AFFILIATIONS
Departamento de Astronomía y Astrofísica, Universitat de València, E-46100 Burjassot, València, Spain
M. P. Thirugnanasambandam
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
L. M. Thomas
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
M. Thomas
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
P. Thomas
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
J. E. Thompson
AFFILIATIONS
University of Southampton, Southampton SO17 1BJ, UK
S. R. Thondapu
AFFILIATIONS
RRCAT, Indore, Madhya Pradesh 452013, India
K. A. Thorne
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
E. Thrane
AFFILIATIONS
OzGrav, School of Physics & Astronomy, Monash University, Clayton 3800, Victoria, Australia
S. Tibrewal
AFFILIATIONS
University of Texas, Austin, TX 78712, USA
J. Tissino
AFFILIATIONS
Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
A. Tiwari
AFFILIATIONS
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
P. Tiwari
AFFILIATIONS
Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
S. Tiwari
AFFILIATIONS
University of Zurich, Winterthurerstrasse 190, 8057 Zurich, Switzerland
V. Tiwari
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
M. R. Todd
AFFILIATIONS
Syracuse University, Syracuse, NY 13244, USA
A. M. Toivonen
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
K. Toland
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
A. E. Tolley
AFFILIATIONS
University of Portsmouth, Portsmouth, PO1 3FX, UK
T. Tomaru
AFFILIATIONS
Gravitational Wave Science Project, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan
K. Tomita
AFFILIATIONS
Department of Physics, Graduate School of Science, Osaka Metropolitan University, 3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka City, Osaka 558-8585, Japan
V. Tommasini
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
T. Tomura
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
H. Tong
AFFILIATIONS
OzGrav, School of Physics & Astronomy, Monash University, Clayton 3800, Victoria, Australia
C. Tong-Yu
AFFILIATIONS
National Central University, Taoyuan City 320317, Taiwan
A. Toriyama
AFFILIATIONS
Department of Physical Sciences, Aoyama Gakuin University, 5-10-1 Fuchinobe, Sagamihara City, Kanagawa 252-5258, Japan
N. Toropov
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
A. Torres-Forné
AFFILIATIONS
Departamento de Astronomía y Astrofísica, Universitat de València, E-46100 Burjassot, València, Spain
Observatori Astronòmic, Universitat de València, E-46980 Paterna, València, Spain
C. I. Torrie
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
M. Toscani
AFFILIATIONS
L2IT, Laboratoire des 2 Infinis - Toulouse, Université de Toulouse, CNRS/IN2P3, UPS, F-31062 Toulouse Cedex 9, France
I. Tosta e Melo
AFFILIATIONS
University of Catania, Department of Physics and Astronomy, Via S. Sofia, 64, 95123 Catania CT, Italy
E. Tournefier
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
M. Trad Nery
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
A. Trapananti
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
Università di Camerino, I-62032 Camerino, Italy
F. Travasso
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
Università di Camerino, I-62032 Camerino, Italy
G. Traylor
AFFILIATIONS
LIGO Livingston Observatory, Livingston, LA 70754, USA
C. Trejo
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
M. Trevor
AFFILIATIONS
University of Maryland, College Park, MD 20742, USA
M. C. Tringali
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
A. Tripathee
AFFILIATIONS
University of Michigan, Ann Arbor, MI 48109, USA
G. Troian
AFFILIATIONS
INFN, Sezione di Trieste, I-34127 Trieste, Italy
Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy
A. Trovato
AFFILIATIONS
INFN, Sezione di Trieste, I-34127 Trieste, Italy
Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy
L. Trozzo
AFFILIATIONS
INFN, Sezione di Napoli, I-80126 Napoli, Italy
R. J. Trudeau
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
T. T. L. Tsang
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
S. Tsuchida
AFFILIATIONS
National Institute of Technology, Fukui College, Geshi-cho, Sabae-shi, Fukui 916-8507, Japan
L. Tsukada
AFFILIATIONS
University of Nevada, Las Vegas, Las Vegas, NV 89154, USA
K. Turbang
AFFILIATIONS
Universiteit Antwerpen, 2000 Antwerpen, Belgium
Vrije Universiteit Brussel, 1050 Brussel, Belgium
M. Turconi
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
C. Turski
AFFILIATIONS
Universiteit Gent, B-9000 Gent, Belgium
H. Ubach
AFFILIATIONS
Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (UB), c. Martí i Franquès, 1, 08028 Barcelona, Spain
Departament de Física Quàntica i Astrofísica (FQA), Universitat de Barcelona (UB), c. Martí i Franqués, 1, 08028 Barcelona, Spain
N. Uchikata
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8582, Japan
T. Uchiyama
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
R. P. Udall
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
T. Uehara
AFFILIATIONS
Department of Communications Engineering, National Defense Academy of Japan, 1-10-20 Hashirimizu, Yokosuka City, Kanagawa 239-8686, Japan
M. Uematsu
AFFILIATIONS
Department of Physics, Graduate School of Science, Osaka Metropolitan University, 3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka City, Osaka 558-8585, Japan
S. Ueno
AFFILIATIONS
Department of Physical Sciences, Aoyama Gakuin University, 5-10-1 Fuchinobe, Sagamihara City, Kanagawa 252-5258, Japan
V. Undheim
AFFILIATIONS
University of Stavanger, 4021 Stavanger, Norway
T. Ushiba
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
M. Vacatello
AFFILIATIONS
Università di Pisa, I-56127 Pisa, Italy
INFN, Sezione di Pisa, I-56127 Pisa, Italy
H. Vahlbruch
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
G. Vajente
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
A. Vajpeyi
AFFILIATIONS
OzGrav, School of Physics & Astronomy, Monash University, Clayton 3800, Victoria, Australia
G. Valdes
AFFILIATIONS
Texas A&M University, College Station, TX 77843, USA
J. Valencia
AFFILIATIONS
IAC3–IEEC, Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
A. F. Valentini
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
M. Valentini
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Department of Physics and Astronomy, Vrije Universiteit Amsterdam, 1081 HV Amsterdam, Netherlands
S. A. Vallejo-Peña
AFFILIATIONS
Universidad de Antioquia, Medellín, Colombia
S. Vallero
AFFILIATIONS
INFN Sezione di Torino, I-10125 Torino, Italy
V. Valsan
AFFILIATIONS
University of Wisconsin–Milwaukee, Milwaukee, WI 53201, USA
N. van Bakel
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
M. van Beuzekom
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
M. van Dael
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Eindhoven University of Technology, 5600 MB Eindhoven, The Netherlands
J. F. J. van den Brand
AFFILIATIONS
Maastricht University, 6200 MD Maastricht, The Netherlands
Nikhef, 1098 XG Amsterdam, The Netherlands
Department of Physics and Astronomy, Vrije Universiteit Amsterdam, 1081 HV Amsterdam, Netherlands
C. Van Den Broeck
AFFILIATIONS
Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, 3584 CC Utrecht, Netherlands
Nikhef, 1098 XG Amsterdam, The Netherlands
D. C. Vander-Hyde
AFFILIATIONS
Syracuse University, Syracuse, NY 13244, USA
M. van der Sluys
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, 3584 CC Utrecht, Netherlands
A. Van de Walle
AFFILIATIONS
Université Paris-Saclay, CNRS/IN2P3, IJCLab, 91405 Orsay, France
J. van Dongen
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Department of Physics and Astronomy, Vrije Universiteit Amsterdam, 1081 HV Amsterdam, Netherlands
K. Vandra
AFFILIATIONS
Villanova University, Villanova, PA 19085, USA
H. van Haevermaet
AFFILIATIONS
Universiteit Antwerpen, 2000 Antwerpen, Belgium
J. V. van Heijningen
AFFILIATIONS
Nikhef, 1098 XG Amsterdam, The Netherlands
Department of Physics and Astronomy, Vrije Universiteit Amsterdam, 1081 HV Amsterdam, Netherlands
P. Van Hove
AFFILIATIONS
Université de Strasbourg, CNRS, IPHC UMR 7178, F-67000 Strasbourg, France
J. Vanier
AFFILIATIONS
Université de Montréal/Polytechnique, Montreal, QC H3T 1J4, Canada
M. VanKeuren
AFFILIATIONS
Kenyon College, Gambier, OH 43022, USA
J. Vanosky
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
M. H. P. M. van Putten
AFFILIATIONS
Department of Physics and Astronomy, Sejong University, 209 Neungdong-ro, Gwangjin-gu, Seoul 143-747, Republic of Korea
Z. Van Ranst
AFFILIATIONS
Maastricht University, 6200 MD Maastricht, The Netherlands
Nikhef, 1098 XG Amsterdam, The Netherlands
N. van Remortel
AFFILIATIONS
Universiteit Antwerpen, 2000 Antwerpen, Belgium
M. Vardaro
AFFILIATIONS
Maastricht University, 6200 MD Maastricht, The Netherlands
Nikhef, 1098 XG Amsterdam, The Netherlands
A. F. Vargas
AFFILIATIONS
OzGrav, University of Melbourne, Parkville, Victoria 3010, Australia
J. J. Varghese
AFFILIATIONS
Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA
V. Varma
AFFILIATIONS
University of Massachusetts Dartmouth, North Dartmouth, MA 02747, USA
A. N. Vazquez
AFFILIATIONS
Stanford University, Stanford, CA 94305, USA
A. Vecchio
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
G. Vedovato
AFFILIATIONS
INFN, Sezione di Padova, I-35131 Padova, Italy
J. Veitch
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
P. J. Veitch
AFFILIATIONS
OzGrav, University of Adelaide, Adelaide, South Australia 5005, Australia
S. Venikoudis
AFFILIATIONS
Université catholique de Louvain, B-1348 Louvain-la-Neuve, Belgium
J. Venneberg
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
P. Verdier
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
M. Vereecken
AFFILIATIONS
Université catholique de Louvain, B-1348 Louvain-la-Neuve, Belgium
D. Verkindt
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
B. Verma
AFFILIATIONS
University of Massachusetts Dartmouth, North Dartmouth, MA 02747, USA
P. Verma
AFFILIATIONS
National Center for Nuclear Research, 05-400 Świerk-Otwock, Poland
Y. Verma
AFFILIATIONS
RRCAT, Indore, Madhya Pradesh 452013, India
S. M. Vermeulen
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
F. Vetrano
AFFILIATIONS
Università degli Studi di Urbino “Carlo Bo,” I-61029 Urbino, Italy
A. Veutro
AFFILIATIONS
INFN, Sezione di Roma, I-00185 Roma, Italy
Università di Roma “La Sapienza”, I-00185 Roma, Italy
A. M. Vibhute
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
A. Viceré
AFFILIATIONS
Università degli Studi di Urbino “Carlo Bo,” I-61029 Urbino, Italy
INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy
S. Vidyant
AFFILIATIONS
Syracuse University, Syracuse, NY 13244, USA
A. D. Viets
AFFILIATIONS
Concordia University Wisconsin, Mequon, WI 53097, USA
A. Vijaykumar
AFFILIATIONS
Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada
A. Vilkha
AFFILIATIONS
Rochester Institute of Technology, Rochester, NY 14623, USA
V. Villa-Ortega
AFFILIATIONS
IGFAE, Universidade de Santiago de Compostela, 15782, Spain
E. T. Vincent
AFFILIATIONS
Georgia Institute of Technology, Atlanta, GA 30332, USA
J.-Y. Vinet
AFFILIATIONS
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis, F-06304 Nice, France
S. Viret
AFFILIATIONS
Université Claude Bernard Lyon 1, CNRS, IP2I Lyon / IN2P3, UMR 5822, F-69622 Villeurbanne, France
A. Virtuoso
AFFILIATIONS
INFN, Sezione di Trieste, I-34127 Trieste, Italy
S. Vitale
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
A. Vives
AFFILIATIONS
University of Oregon, Eugene, OR 97403, USA
H. Vocca
AFFILIATIONS
INFN, Sezione di Perugia, I-06123 Perugia, Italy
Università di Perugia, I-06123 Perugia, Italy
D. Voigt
AFFILIATIONS
Universität Hamburg, D-22761 Hamburg, Germany
E. R. G. von Reis
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
J. S. A. von Wrangel
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
L. Vujeva
AFFILIATIONS
Niels Bohr Institute, University of Copenhagen, 2100 Kóbenhavn, Denmark
S. P. Vyatchanin
AFFILIATIONS
Lomonosov Moscow State University, Moscow 119991, Russia
J. Wack
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
L. E. Wade
AFFILIATIONS
Kenyon College, Gambier, OH 43022, USA
M. Wade
AFFILIATIONS
Kenyon College, Gambier, OH 43022, USA
K. J. Wagner
AFFILIATIONS
Rochester Institute of Technology, Rochester, NY 14623, USA
A. Wajid
AFFILIATIONS
INFN, Sezione di Genova, I-16146 Genova, Italy
Dipartimento di Fisica, Università degli Studi di Genova, I-16146 Genova, Italy
M. Walker
AFFILIATIONS
Christopher Newport University, Newport News, VA 23606, USA
G. S. Wallace
AFFILIATIONS
SUPA, University of Strathclyde, Glasgow G1 1XQ, UK
L. Wallace
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
E. J. Wang
AFFILIATIONS
Stanford University, Stanford, CA 94305, USA
H. Wang
AFFILIATIONS
Department of Physics, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
J. Z. Wang
AFFILIATIONS
University of Michigan, Ann Arbor, MI 48109, USA
W. H. Wang
AFFILIATIONS
The University of Texas Rio Grande Valley, Brownsville, TX 78520, USA
Y. F. Wang
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
Z. Wang
AFFILIATIONS
National Central University, Taoyuan City 320317, Taiwan
G. Waratkar
AFFILIATIONS
Indian Institute of Technology Bombay, Powai, Mumbai 400 076, India
J. Warner
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
M. Was
AFFILIATIONS
Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, F-74000 Annecy, France
T. Washimi
AFFILIATIONS
Gravitational Wave Science Project, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka City, Tokyo 181-8588, Japan
N. Y. Washington
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
D. Watarai
AFFILIATIONS
University of Tokyo, Tokyo, 113-0033, Japan
K. E. Wayt
AFFILIATIONS
Kenyon College, Gambier, OH 43022, USA
B. R. Weaver
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
B. Weaver
AFFILIATIONS
LIGO Hanford Observatory, Richland, WA 99352, USA
C. R. Weaving
AFFILIATIONS
University of Portsmouth, Portsmouth, PO1 3FX, UK
S. A. Webster
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
N. L. Weickhardt
AFFILIATIONS
Universität Hamburg, D-22761 Hamburg, Germany
M. Weinert
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
A. J. Weinstein
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
R. Weiss
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
Author notes
Deceased, 2025 August.
F. Wellmann
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
L. Wen
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
P. Wessels
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
K. Wette
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
J. T. Whelan
AFFILIATIONS
Rochester Institute of Technology, Rochester, NY 14623, USA
B. F. Whiting
AFFILIATIONS
University of Florida, Gainesville, FL 32611, USA
C. Whittle
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
E. G. Wickens
AFFILIATIONS
University of Portsmouth, Portsmouth, PO1 3FX, UK
J. B. Wildberger
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam, Germany
D. Wilken
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
D. J. Willadsen
AFFILIATIONS
Concordia University Wisconsin, Mequon, WI 53097, USA
K. Willetts
AFFILIATIONS
Cardiff University, Cardiff CF24 3AA, UK
D. Williams
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
M. J. Williams
AFFILIATIONS
University of Portsmouth, Portsmouth, PO1 3FX, UK
N. S. Williams
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
J. L. Willis
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
B. Willke
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
M. Wils
AFFILIATIONS
Katholieke Universiteit Leuven, Oude Markt 13, 3000 Leuven, Belgium
C. W. Winborn
AFFILIATIONS
Missouri University of Science and Technology, Rolla, MO 65409, USA
J. Winterflood
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
C. C. Wipf
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
G. Woan
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
J. Woehler
AFFILIATIONS
Maastricht University, 6200 MD Maastricht, The Netherlands
Nikhef, 1098 XG Amsterdam, The Netherlands
N. E. Wolfe
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
H. T. Wong
AFFILIATIONS
National Central University, Taoyuan City 320317, Taiwan
I. C. F. Wong
AFFILIATIONS
Katholieke Universiteit Leuven, Oude Markt 13, 3000 Leuven, Belgium
The Chinese University of Hong Kong, Shatin, NT, Hong Kong
J. L. Wright
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
M. Wright
AFFILIATIONS
SUPA, University of Glasgow, Glasgow G12 8QQ, UK
C. Wu
AFFILIATIONS
National Tsing Hua University, Hsinchu City 30013, Taiwan
D. S. Wu
AFFILIATIONS
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany
Leibniz Universität Hannover, D-30167 Hannover, Germany
H. Wu
AFFILIATIONS
National Tsing Hua University, Hsinchu City 30013, Taiwan
E. Wuchner
AFFILIATIONS
California State University Fullerton, Fullerton, CA 92831, USA
D. M. Wysocki
AFFILIATIONS
University of Wisconsin–Milwaukee, Milwaukee, WI 53201, USA
V. A. Xu
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
Y. Xu
AFFILIATIONS
University of Zurich, Winterthurerstrasse 190, 8057 Zurich, Switzerland
N. Yadav
AFFILIATIONS
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, 00-716, Warsaw, Poland
H. Yamamoto
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
K. Yamamoto
AFFILIATIONS
Faculty of Science, University of Toyama, 3190 Gofuku, Toyama City, Toyama 930-8555, Japan
T. S. Yamamoto
AFFILIATIONS
University of Tokyo, Tokyo, 113-0033, Japan
T. Yamamoto
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
S. Yamamura
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8582, Japan
R. Yamazaki
AFFILIATIONS
Department of Physical Sciences, Aoyama Gakuin University, 5-10-1 Fuchinobe, Sagamihara City, Kanagawa 252-5258, Japan
T. Yan
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
F. W. Yang
AFFILIATIONS
The University of Utah, Salt Lake City, UT 84112, USA
F. Yang
AFFILIATIONS
Columbia University, New York, NY 10027, USA
K. Z. Yang
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
Y. Yang
AFFILIATIONS
Department of Electrophysics, National Yang Ming Chiao Tung University, 101 University Street, Hsinchu, Taiwan
Z. Yarbrough
AFFILIATIONS
Louisiana State University, Baton Rouge, LA 70803, USA
H. Yasui
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
S.-W. Yeh
AFFILIATIONS
National Tsing Hua University, Hsinchu City 30013, Taiwan
A. B. Yelikar
AFFILIATIONS
Rochester Institute of Technology, Rochester, NY 14623, USA
X. Yin
AFFILIATIONS
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
J. Yokoyama
AFFILIATIONS
Department of Physics, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
University of Tokyo, Tokyo, 113-0033, Japan
Kavli Institute for the Physics and Mathematics of the Universe, WPI, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa City, Chiba 277-8583, Japan
T. Yokozawa
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
J. Yoo
AFFILIATIONS
Cornell University, Ithaca, NY 14850, USA
H. Yu
AFFILIATIONS
CaRT, California Institute of Technology, Pasadena, CA 91125, USA
S. Yuan
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
H. Yuzurihara
AFFILIATIONS
Institute for Cosmic Ray Research, KAGRA Observatory, The University of Tokyo, 238 Higashi-Mozumi, Kamioka-cho, Hida City, Gifu 506-1205, Japan
A. Zadrożny
AFFILIATIONS
National Center for Nuclear Research, 05-400 Świerk-Otwock, Poland
M. Zanolin
AFFILIATIONS
Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA
M. Zeeshan
AFFILIATIONS
Rochester Institute of Technology, Rochester, NY 14623, USA
T. Zelenova
AFFILIATIONS
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
J.-P. Zendri
AFFILIATIONS
INFN, Sezione di Padova, I-35131 Padova, Italy
M. Zeoli
AFFILIATIONS
Université catholique de Louvain, B-1348 Louvain-la-Neuve, Belgium
M. Zerrad
AFFILIATIONS
Aix Marseille Univ, CNRS, Centrale Med, Institut Fresnel, F-13013 Marseille, France
M. Zevin
AFFILIATIONS
Northwestern University, Evanston, IL 60208, USA
A. C. Zhang
AFFILIATIONS
Columbia University, New York, NY 10027, USA
L. Zhang
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
R. Zhang
AFFILIATIONS
Northeastern University, Boston, MA 02115, USA
T. Zhang
AFFILIATIONS
University of Birmingham, Birmingham B15 2TT, UK
Y. Zhang
AFFILIATIONS
OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia
C. Zhao
AFFILIATIONS
OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia
Yue Zhao
AFFILIATIONS
The University of Utah, Salt Lake City, UT 84112, USA
Yuhang Zhao
AFFILIATIONS
Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
Y. Zheng
AFFILIATIONS
Missouri University of Science and Technology, Rolla, MO 65409, USA
H. Zhong
AFFILIATIONS
University of Minnesota, Minneapolis, MN 55455, USA
R. Zhou
AFFILIATIONS
University of California, Berkeley, CA 94720, USA
X.-J. Zhu
AFFILIATIONS
Department of Astronomy, Beijing Normal University, Xinjiekouwai Street 19, Haidian District, Beijing 100875, People’s Republic of China
Z.-H. Zhu
AFFILIATIONS
School of Physics and Technology, Wuhan University, Bayi Road 299, Wuchang District, Wuhan, Hubei, 430072, People’s Republic of China
Department of Astronomy, Beijing Normal University, Xinjiekouwai Street 19, Haidian District, Beijing 100875, People’s Republic of China
A. B. Zimmerman
AFFILIATIONS
University of Texas, Austin, TX 78712, USA
M. E. Zucker
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
J. Zweizig
AFFILIATIONS
LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration
Notes
Article metrics
5792
Total downloads
Video abstract views
Share this article
Dates
Received
2025 August 26
Revised
2025 September 23
Accepted
2025 September 26
Published
2025 December 9
Unified Astronomy Thesaurus concepts
Gravitational wave astronomy
Gravitational wave detectors
Gravitational wave sources
Stellar mass black holes
Neutron stars
Journal RSS
Create or edit your corridor alerts
What are corridors?
2041-8205/995/1/L18
Abstract
The Gravitational-Wave Transient Catalog (GWTC) is a collection of short-duration (transient) gravitational-wave signals identified by the LIGO–Virgo–KAGRA Collaboration in gravitational-wave data produced by the eponymous detectors. The catalog provides information about the identified candidates, such as the arrival time and amplitude of the signal and properties of the signal’s source as inferred from the observational data. GWTC is the data release of this dataset, and version 4.0 extends the catalog to include observations made during the first part of the fourth LIGO–Virgo–KAGRA observing run up until 2024 January 31. This Letter marks an introduction to a collection of articles related to this version of the catalog, GWTC-4.0. The collection of articles accompanying the catalog provides documentation of the methods used to analyze the data, summaries of the catalog of events, observational measurements drawn from the population, and detailed discussions of selected candidates.
Export citation and abstract
BibTeX
RIS
Previous
article in issue
Next
article in issue
NASA ADS Record
About Related Links
Original content from this work may be used under the terms of the
Creative Commons Attribution 4.0 licence
. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.
1. Overview
The Laser Interferometer Gravitational-Wave Observatory (LIGO; J. Aasi et al.
2015a
) and the Virgo (F. Acernese et al.
2015
) and KAGRA (T. Akutsu et al.
2021
) observatories form an international network of ground-based gravitational-wave (GW) detectors. This Letter is an introduction to the collection of articles describing the contents of the LIGO–Virgo–KAGRA Collaboration (LVK) Gravitational-Wave Transient Catalog (GWTC) version 4.0, hereafter GWTC-4.0, along with reviews of the methods used in various aspects in the construction of this catalog, astrophysical and cosmological implications of the observations, and tests of general relativity (GR) that are performed on the observed transients. This Letter provides details on the network of GW detectors, the observing runs, observatory evolution, and a review of the transient signals that have been identified. In addition, we describe conventions and notations that are used throughout the collection of articles accompanying the catalog.
1.1. The GWTC Sources and Science
Transient GW signals may be produced by a variety of astrophysical sources, including compact binary coalescences (CBCs) of compact objects such as black holes (BHs) and neutron stars (NSs), core-collapse supernovae, and other explosive phenomena (B. P. Abbott et al.
2020a
). The first observed GW transient, GW150914, was a binary BH (BBH) coalescence (B. P. Abbott et al.
2016a
), and we have since observed a binary NS (BNS) coalescence (B. P. Abbott et al.
2017a
) that had associated electromagnetic counterparts (B. P. Abbott et al.
2017b
) and NS–BH binary (NSBH) coalescences (R. Abbott et al.
2020d
).
This GWTC-4.0 collection of articles describes the GW transient candidates observed by the LVK from the observing run (O1) through the end of the fourth observing run (O4a) and the astrophysical implications of these observations. The article collection includes the following:
1.
“GWTC-4.0: Methods for Identifying and Characterizing Gravitational-wave Transients” (A. G. Abac et al.
2025a
) reviews the procedures used to go from the calibrated output of the detectors to a list of transient candidates that includes measurements of the statistical significance and inferences on each of the corresponding astrophysical sources.
2.
“GWTC-4.0: Updating the Gravitational-Wave Transient Catalog with Observations from the First Part of the Fourth LIGO–Virgo–KAGRA Observing Run” (A. G. Abac et al.
2025b
) describes the primary observational results contained in GWTC-4.0: the significant GW transient candidates observed through the end of the O4a observing run and the inferred source parameters under the hypothesis that these transients arise from GWs emitted by CBCs (Section
5.2
).
3.
“GWTC-4.0: Population Properties of Merging Compact Binaries” (A. G. Abac et al.
2025c
) describes the underlying population of CBCs inferred using GWTC-4.0 data and related astrophysical implications.
4.
“GWTC-4.0: Tests of General Relativity I—Overview and General Tests” (A. G. Abac et al.
2025d
) presents an overview of the methods and tests of GR performed on the subset of signals suitable for such tests and focuses on the general and consistency tests.
5.
“GWTC-4.0: Tests of General Relativity II—Parameterized Tests” (A. G. Abac et al.
2025e
) describes the parameterized tests of GR performed on the signals.
6.
“GWTC-4.0: Tests of General Relativity III—Tests of the Remnant” (A. G. Abac et al.
2025f
) describes the tests of the coalescence remnants.
7.
“GWTC-4.0: Constraints on the Cosmic Expansion Rate and Modified Gravitational-wave Propagation” (A. G. Abac et al.
2025g
) describes the methods used to determine the Hubble constant and related parameters, including parameterized deviations from GR on cosmological scales, using GWTC-4.0 candidates.
8.
“GWTC-4.0: Searches for Gravitational Wave Lensing Signatures” (A. G. Abac et al.
2025h
) describes the searches for lensed GW signals in the geometric and wave optics regime in the GWTC-4.0 dataset. It also sets constraints on the merger rate at high redshift and the relative rate of strongly lensed signals compared to unlensed ones.
9.
“Open Data from LIGO, Virgo, and KAGRA through the First Part of the Fourth Observing Run” (A. G. Abac et al.
2025i
) describes the publicly accessible data and other science products that can be freely accessed through the Gravitational Wave Open Science Center (GWOSC). These data sets include the raw GW strain time series, details of the calibration and cleaning process, efforts to remove instrumental noise artifacts, and details of the online GWTC-4.0.
10.
“GW230814: Investigation of a Loud Gravitational-wave Signal Observed with a Single Detector” (A. G. Abac et al.
2025j
) describes the analysis of the loudest event in the GWTC-4.0 catalog, GW230814_230901, which was detected on 2023 August 14. This event is notable for its high signal-to-noise ratio (SNR) and its potential implications for our understanding of GW signals and GR.
11.
“GW231123: a Binary Black Hole Merger with Total Mass 190–265
” (A. G. Abac et al.
2025k
) describes the analysis of the candidate GW231123_135430, detected on 2023 November 23. The candidate’s source is exceptional, having the highest inferred total mass of any high-confidence BBH observations to date.
To reference the whole GWTC-4.0 collection, we encourage citing this introductory Letter.
1.2. The Electronic Catalog: GWTC
A. G. Abac et al. (
2025i
) document the released open data, including the GWTC dataset. The catalog contains candidates (sometimes called
events
) identified in observational data that are deemed likely to be caused by GW signals, as well as triggers corresponding to times selected by searches of the data for GW transient signals that potentially contain an identifiable signal but with lower confidence of being caused by a GW.
1.2.1. The Catalog Naming Convention
The LVK GWTC is a cumulative dataset containing data on all transient candidates reported by the LVK. Released versions of the catalog have major and minor numbers in the format
The major number is determined by the span of time containing all candidates in the catalog as described below.
Prior to GWTC-4.0, the minor number was routinely omitted when describing a catalog version when that minor number was 0, so GWTC-1.0, GWTC-2.0, and GWTC-3.0 were referred to as GWTC-1, GWTC-2, and GWTC-3 in the articles that described those catalog versions. In this Letter, and in the future, we will include the .0 when referring to those catalog versions. We also say that GWTC–<
major
> can refer to GWTC–<
major
>.<
minor
> for any minor version having that major version number.
Each catalog version is a superset of the previous one (apart from retracted candidates), so that, for example, GWTC-3.0 (R. Abbott et al.
2023
) contains all the candidates in GWTC-2.1 (R. Abbott et al.
2024
). Since GWTC-2.1 provided a deeper list of candidates observed over the same period as GWTC-2.0 (R. Abbott et al.
2021b
), the minor version numbers of these two releases differ while their major version numbers remain the same. In general:
1.
The major number is incremented when the span of time over which observational data were searched for transients is increased.
2.
The minor version resets to 0 when the major version number is increased.
3.
The minor version is incremented when there is a change in the data describing the transients (additional data, modified data, or removed data) contained in the catalog within the current time span covered.
The time span covering the transient candidates in the catalog indicated by the major number is as follows:
GWTC-1:
Contains candidates occurring in data taken before 2018 October 1 00:00:00. The GWTC-1.0 dataset is described in B. P. Abbott et al. (
2019a
).
GWTC-2:
Contains candidates occurring in data taken before 2019 October 1 15:00:00. The GWTC-2.0 dataset is described in R. Abbott et al. (
2021b
) and the GWTC-2.1 dataset in R. Abbott et al. (
2024
).
GWTC-3:
Contains candidates occurring in data taken before 2020 May 1 00:00:00. The GWTC-3.0 dataset is described in R. Abbott et al. (
2023
).
GWTC-4:
Contains candidates occurring in data taken before 2024 January 31 00:00:00. The GWTC-4.0 dataset is described in A. G. Abac et al. (
2025b
).
In addition to GWTC, other catalogs of GW transients include the Open Gravitational-wave Catalog (OGC), the most recent version 4-OGC contains observations from 2015 to 2020 (A. H. Nitz et al.
2023
), as well as catalogs of candidate signals identified by the IAS pipeline (T. Venumadhav et al.
2019
; S. Olsen et al.
2022
; D. Wadekar et al.
2024
; M. H.-Y. Cheung et al.
2025
). A. G. Abac et al. (
2025i
) provide details on the GWOSC event portal,
327
a database of published GW transient events, including Community Catalogs (J. Kanner et al.
2025
) containing catalog results from communities outside of the LVK.
1.2.2. Candidate Naming Conventions
The naming of our GW candidates follows the format
encoding the date and Coordinated Universal Time (UTC) of the signal. For example, GW200105_162426 was the transient observed on 2020 January 5 at 16:24:26 UTC. For transient signals spanning multiple-second intervals, the time assigned to a signal is an estimate of the time of peak GW amplitude.
GW candidates reported prior to the release of GWTC-2.0 were designated by the abbreviated form
including candidates first appearing in GWTC-1.0 (B. P. Abbott et al.
2019a
), as well as GW190412 (R. Abbott et al.
2020e
), GW190425 (B. P. Abbott et al.
2020b
), GW190521 (R. Abbott et al.
2020f
), and GW190814 (R. Abbott et al.
2020d
). These candidates retain their legacy names.
1.3. Outline
An outline of the remainder of this article is as follows: We briefly describe the network of ground-based GW detectors in Section
and their observing runs that have contributed to the GWTC-4.0 in Section
. These sections are followed by short reviews of the evolution of the various observatories in Section
and of the nature of the transient sources observed in Section
. A list of common acronyms is provided in Appendix
. Mathematical conventions used throughout the articles in this compendium are described in Appendix
2. The International GW Observatory Network
The international ground-based GW observatory network currently comprises four primary observatories employing laser interferometric GW detectors. The four observatories are the two US-based LIGO detectors, LIGO Hanford Observatory (LHO) in Washington and LIGO Livingston Observatory (LLO) in Louisiana (J. Aasi et al.
2015a
); the European Virgo detector (F. Acernese et al.
2015
); and the Japanese KAGRA detector (K. Somiya
2012
; Y. Aso et al.
2013
; T. Akutsu et al.
2021
). All these detectors are enhanced Michelson interferometers that sense relative changes in the lengths
and
of their two 3 km to 4 km long arms caused by passing GWs in the high-frequency band ∼10 Hz to ∼1000 Hz (K. S. Thorne
1987
). Other GW frequency bands include the very low frequency band ∼1 nHz to ∼100 nHz observed by pulsar timing arrays such as the European Pulsar Timing Array (EPTA; G. Desvignes et al.
2016
), the North American Nanohertz Observatory for Gravitational Waves (NANOGrav; A. Brazier et al.
2019
), the Parkes Pulsar Timing Array (PPTA; M. Kerr et al.
2020
), the Indian Pulsar Timing Array (InPTA; B. C. Joshi et al.
2018
), and their combined consortium the International Pulsar Timing Array (IPTA; J. P. W. Verbiest et al.
2016
); and the low-frequency band ∼0.1 mHz to ∼10 mHz that will be observed by the Laser Interferometer Space Antenna (LISA; M. Colpi et al.
2024
).
The fractional change in the relative lengths of the two optical paths of interferometric detectors, Δ(
), induced by a GW is known as the detector strain,
= Δ(
)/
, where
is the average arm length (Section
5.1
). The sensitivity of ground-based detectors is fundamentally limited below ∼1 Hz by ground motion noise (P. R. Saulson
1984
) and at high frequencies by shot noise (R. L. Forward
1978
; A. Krolak et al.
1991
). Significant noise sources at intermediate frequencies include thermal noise in the optics and their suspensions and quantum readout noise (A. Buonanno & Y.-b. Chen
2001
; P. R. Saulson
2017
; R. Weiss
2022
). In the frequency domain, the overall detector sensitivity is characterized by the (one-sided) noise power spectral density (PSD) in strain-equivalent units,
), with dimensions of time (Appendix
).
The GEO600 GW detector (GEO) is a British–German instrument with 600 m arms located near Hannover, Germany (H. Luck et al.
2010
; C. Affeldt et al.
2014
; K. L. Dooley et al.
2016
). This instrument is a laboratory for prototyping advanced interferometry techniques, but it also is operated in data-taking
astrowatch
mode when not being used for instrument science research (H. Grote
2010
; K. L. Dooley et al.
2016
). Astrowatch provides GW observing coverage for times when the larger detectors are not observing between observing runs and when the detectors are not taking scientific data, e.g., GEO data were used to constrain post-merger signals following the first BNS detection (B. P. Abbott et al.
2017c
).
3. Observing Runs
The GW observing schedule is divided into observing runs, downtime for construction and commissioning, and transitional engineering runs between commissioning and observing runs (B. P. Abbott et al.
2020a
). Figure
shows a timeline of GW observations up to the end date of the time period covered by GWTC-4.0. Indicated are the observing periods of each observing run and the times when each detector was in operation. Also shown are the times when GW transient signals were detected.
Figure 1.
The timeline of observing runs covering a time span starting from 2015 and lasting up to the beginning of O4b on 2024 April 10. The periods in which the various detectors in the network were observing are shown in this timeline, along with the typical BNS inspiral ranges for those detectors during the observing run. GEO astrowatch observing periods are shown in light gray. KAGRA observing periods during O4a, also shown in light gray, were not used for GW observational analyses. In O1 and O4a, only LHO and LLO were participating. Virgo joined these two detectors for the last month of O2 and was observing alongside them throughout O3a and O3b. At the end of O3 there was a short joint observing run, O3GK, which included GEO and KAGRA. Also shown is a timeline of the observed candidates contained in GWTC-1.0, GWTC-2.1, GWTC-3.0, and GWTC-4.0 with a probability of astrophysical origin greater than or equal to 50%. The time intervals covered by the various versions of the GWTC are bounded from above but not from below, as indicated by the arrows pointing left (see Section
1.2.1
).
Download figure:
Standard image
High-resolution image
In order to quickly compare sensitivities of detectors, the GW community uses a fiducial range, to which a typical BNS can generally be detected. This fiducial distance assumes that an SNR of at least 8 is needed for a detection, and it approximates the BNS inspiral waveform at Newtonian order (Section
5.2
). The BNS inspiral range is a volume-averaged measure of sensitivity to a signal from two 1.4
bodies in a quasi-circular inspiral at a single-detector SNR threshold of 8 (L. S. Finn & D. F. Chernoff
1993
; H.-Y. Chen et al.
2021
). When a homogeneous BNS population is assumed and cosmological effects are ignored, the BNS inspiral range for a detector is determined by its noise power spectrum as
and the sensitive volume of the detector (also when neglecting cosmological effects) is given by
= (4
/3)
(Appendix
). (This measure is taken as a simple figure of merit of sensitivity to CBCs; it does not attempt to account for the true underlying astrophysical distribution describing such systems.) If the number of BNS mergers per unit time per unit volume of space, the merger rate density of BNSs, is
, then the expected number of BNS signals seen with SNR greater than 8 in time
would be
. Figure
also gives the typical BNS inspiral range, as given in Equation (
), for each detector during each observing run.
The
amplitude
strain noise spectrum is the square root of the (one-sided) noise PSD in strain-equivalent units
having dimensions of time
1/2
. The amplitude strain noise spectra of LHO, LLO, and Virgo during the various observing runs are shown in Figure
. There is an overall reduction in the detector noise levels with successive observing runs resulting in increased sensitivity. Figure
also shows the fraction of the run duration during which different combinations of detectors were observing.
Figure 2.
Representative noise amplitude spectral densities for LHO, LLO, and Virgo during O1 (LHO, LLO: 2015 October 24), O2 (LHO: 2017 June 10; LLO: 2017 August 6; Virgo: from F. Acernese et al.
2023a
), O3 (LHO: 2020 January 4; LLO: 2019 April 29; Virgo: 2020 February 9), and O4a (LHO: 2024 January 11; LLO: 2023 November 19). The BNS inspiral ranges, defined by Equation (
), for these noise curves are given in the legend. Inset sunburst charts show the fraction of the run duration during which different combinations of detectors were observing. Gray regions in each ring indicate portions when a detector is not operating. The segments of the sunburst chart, clockwise from 12 o’clock, are LHO–LLO, LHO alone, LLO alone, and neither for observing runs involving only LHO and LLO; and LHO–LLO–Virgo, LHO–LLO, LHO– Virgo, LLO–Virgo, LHO alone, LLO alone, Virgo alone, and none for observing runs involving LHO, LLO, and Virgo.
Download figure:
Standard image
High-resolution image
Figure
shows the cumulative number of candidates detected versus the estimated effective time–volume hypervolume
VT
for the detector network. For the first two observing runs (described below), only data when two detectors were operating were searched for GWs. In this case the rate at which
VT
is accumulated at any observing time is given by the sensitive volume
for the
second
most sensitive instrument observing at that time. Beginning with the third observing run, periods during which only a single detector was observing were included in the search. During such time, the rate at which
VT
is accumulated is again given by the sensitive volume
= (4
/3)
, but where
is computed from Equation (
) divided by 1.5, representing an effective SNR threshold for detection of 12 rather than 8 for single-detector observation (R. Abbott et al.
2021b
). This simple estimate of
VT
, derived from the BNS inspiral range, is an approximate one done for a quick and convenient overview. In particular, it makes a crude approximation of whether a signal is detectable, and its numerical value is only representative of sensitivity to sources in a small region of mass space. Actual measured sensitive hypervolume 〈
VT
〉 values for various CBC mass regions and search methods are reported in A. G. Abac et al. (
2025b
).
Figure 3.
The number of CBC detection candidates with a probability of astrophysical origin greater than or equal to 50% vs. the detector network’s effective surveyed hypervolume for BNS coalescences (R. Abbott et al.
2021b
). The BNS effective surveyed hypervolume is a valid proxy for overall sensitivity to CBCs, though its scale is set to the case of canonical BNS signals. The colored bands indicate the different observing runs. The final data sets for O1, O2, O3a, O3b, and O4a consist of 49.0 day, 122.2 day, 149.6 day (177.1 day), 124.6 day (141.9 day) and 126.5 (196.8) days, respectively, with at least two detectors (one detector) observing. The cumulative number of probable candidates is indicated by the solid black line, while the blue line, dark-blue band, and light-blue band are the median, 50% confidence interval, and 90% confidence interval for a Poisson distribution fit to the number of candidates at the end of O4a, respectively.
Download figure:
Standard image
High-resolution image
3.1. O1: The First Observing Run
O1 consists of the time period from 2015 September 12 to 2016 January 19. O1 includes short time periods that were originally planned to be engineering time (2015 September 12 to 2015 September 18 and 2016 January 12 to 2016 January 19), but which were of sufficient quality to be included in O1. This was the first observing run with the Advanced LIGO (aLIGO) interferometers, in progress toward full aLIGO design sensitivity (B. P. Abbott et al.
2016b
2016c
), with LHO achieving a BNS range of 80 Mpc and LLO a range of 70 Mpc.
Of the 129.7-day duration of O1, there were only 49.0 days (38%) when both LHO and LLO were observing jointly, and there were 36.2 days (28%) when neither detector was observing. The largest nonobserving periods were due to locking, the time spent bringing the interferometers from an uncontrolled state to their low-noise configuration (A. Staley et al.
2014
), and environmental issues such as earthquakes, wind, and microseismic noise arising from ocean storms (A. Effler et al.
2015
; B. P. Abbott et al.
2016d
). Wind and microseismic noise have seasonal variation, as storms are more prevalent in winter months; LLO was more susceptible to these than LHO, mainly due to its local geophysical environment (E. J. Daw et al.
2004
).
Overall, a total effective hypervolume
VT
= 1.59 × 10
−4
Gpc
yr was accumulated during joint LHO–LLO observing during O1.
3.2. O2: The Second Observing Run
The O2 run was from 2016 November 30 to 2017 August 25. It was preceded by an engineering run that began on 2016 October 31 at LLO and on 2016 November 14 at LHO. The LHO and LLO detectors achieved a typical BNS range sensitivity of 80 Mpc and 100 Mpc, respectively (B. P. Abbott et al.
2017d
2019a
). However, on 2017 July 6 LHO was severely affected by a 5.8 mag earthquake in Montana, resulting in a post-earthquake sensitivity drop of approximately 10 Mpc in BNS range for the remainder of the run (B. P. Abbott et al.
2019a
).
The Advanced Virgo (AdV) interferometer (F. Acernese et al.
2015
) joined O2 on 2017 August 1, forming a three-detector network for the last month of the run. A vacuum contamination issue required AdV to use steel wires rather than fused silica fibers to suspend the test masses, limiting the sensitivity of AdV (B. P. Abbott et al.
2019a
). In O2, a 30 Mpc BNS range was achieved.
The LIGO detectors saw some improvement in duty factors during nonwinter months, with an almost 50% reduction in downtime due to environmental effects at both sites, though LLO lost over twice as much observing time as LHO to earthquakes, microseismic noise, and wind. O2 had a planned mid-run engineering break to effect needed repairs and to attempt improvements to the sensitivity. The Virgo instrument operated with a duty factor of approximately 85% after joining O2. There were 15 days of all three detectors observing simultaneously.
Overall, a total effective hypervolume
VT
= 3.52 × 10
−4
Gpc
yr was accumulated during O2; of this, 3.27 × 10
−4
Gpc
yr was accumulated during joint LHO–LLO observing, 2.41 × 10
−5
Gpc
yr was accumulated while all three detectors were observing, and only 3.62 × 10
−7
Gpc
yr and 4.80 × 10
−7
Gpc
yr were accumulated during joint LHO–Virgo and LLO–Virgo observing, respectively.
3.3. O3: The Third Observing Run
O3 started on 2019 April 1, with a commissioning break from 2019 October 1 to 2019 November 1. This observing run was planned to continue to 2020 April 30, but the COVID-19 pandemic resulted in a suspension of observing on 2020 March 27 (R. Abbott et al.
2023
). The period of O3 prior to the commissioning break is referred to as O3a, while the period after the break is referred to as O3b. KAGRA had intended to join LIGO and Virgo at the end of O3, but the early end made this impossible. Instead, KAGRA and GEO jointly observed for a 2-week period from 2020 April 7 to 2020 April 21 after LIGO and Virgo had suspended their observing. This joint GEO–KAGRA run (distinct from the O3 run described previously) is referred to as O3GK (R. Abbott et al.
2022
).
In O3, the LHO and LLO detectors achieved a BNS range of 110 Mpc and 140 Mpc, respectively (A. Buikema et al.
2020
). This increase in sensitivity arose from a variety of improvements, chief among them an increase in the input laser power, the addition of a squeezed vacuum source at the interferometer output (M. Tse et al.
2019
), and mitigation of noise arising from scattered light (S. Soni et al.
2020
). In addition, end-test-mass optics with lower-loss coatings, along with new reaction masses, were installed in each LIGO interferometer (S. M. Aston et al.
2012
; M. Granata et al.
2020
).
The steel wires in AdV were replaced with fused silica fibers in preparation for O3. Along with other improvements, such as reduction of technical noises, an increase in laser power, and the installation of a squeezed vacuum source, Virgo achieved a BNS range of 60 Mpc (F. Acernese et al.
2019
).
Over all of O3a and O3b, 361.1 days combined, there were 154.3 days (43%) of three-detector observation and only 42.1 days (12%) during which no detector was observing. The total effective hypervolume
VT
accumulated was 3.21 × 10
−3
Gpc
yr. Of this, 2.27 × 10
−3
Gpc
yr was accumulated during three-detector observations, 7.20 × 10
−4
Gpc
yr when LHO and LLO were observing, 4.09 × 10
−5
Gpc
yr when LHO and Virgo were observing, and 5.03 × 10
−5
Gpc
yr when LLO and Virgo were observing. The amount accumulated with only a single detector observing was 4.47 × 10
−5
Gpc
yr, 7.47 × 10
−5
Gpc
yr, and 9.72 × 10
−6
Gpc
yr for LHO, LLO, and Virgo, respectively.
The first operation of the KAGRA detector in an initial configuration with a simple Michelson interferometer occurred in 2016 March (T. Akutsu et al.
2018
). In 2019 August, the first lock of the Fabry–Perot Michelson interferometer was achieved, with power recycling accomplished in 2020 January. By the end of 2020 March, KAGRA obtained a BNS range of approximately 1 Mpc (H. Abe et al.
2023
), and although the LIGO and Virgo instruments had ended their O3 run, KAGRA was operated jointly with GEO, which had a comparable BNS range, in O3GK yielding 6.4 days of joint observing time.
3.4. O4: The Fourth Observing Run
O4 began on 2023 May 24 at 15:00:00 UTC. This run is again divided into parts: the fourth observing run (O4a) ended on 2024 January 16 at 16:00:00 UTC and was followed by a commissioning break; the fourth observing run (O4b) started on 2024 April 10 at 15:00:00 UTC. The O4b period continued until 2025 January 28 17:00:00 UTC, the original intended end of O4; however, it was decided to continue observing into a third part of the fourth observing run (O4c), which ended on 2025 November 18 at 16:00 UTC. The period covered by GWTC-4.0 contains events that occurred in O4a and earlier observing runs only (see Section
1.2.1
). O4b and O4c analyses are underway and will be included in future versions of the GWTC.
The two LIGO detectors were observing during O4a, both having a BNS range of approximately 160 Mpc. During the 237.0 days, there were 126.5 days (53%) of two-detector joint observation and 40.2 days (17%) when neither of the LIGO detectors was observing. Virgo did not join joint observation until O4b in order to continue commissioning to address a damaged mirror that limited performance and to improve sensitivity. KAGRA also continued commissioning to improve sensitivity, with the goal of joining O4 toward the end of the run.
During O4a, the total effective hypervolume
VT
accumulated was 5.28 × 10
−3
Gpc
yr. This is divided into 3.85 × 10
−4
Gpc
yr during which LHO alone was observing, 4.57 × 10
−4
Gpc
yr during which LLO alone was observing, and 4.44 × 10
−3
Gpc
yr during which both detectors were observing.
The timeline for O5 is being assessed in order to maximize the scientific output of the global network. Updates to the planned observing schedule will be provided as soon as such decisions are made.
328
4. Observatory Evolution
The advanced-detector era is characterized by a series of technological improvements from the initial detectors that deliver higher sensitivity and greater BNS range, which made possible the era of GW observation. Some of the key instrument science elements of the advanced era detectors are (i) increases in the input laser power entering the interferometer and to the circulating power in the interferometer cavities (a higher power in the arms produced a lower quantum-shot-noise-limited sensitivity above ∼200 Hz); (ii) increases in test-mass mirror size to accommodate larger beams, which mitigates coating thermal noise and heavier masses to reduce inertial and quantum back-action effects; (iii) implementation of signal recycling (B. J. Meers
1988
) in addition to power recycling (R. W. P. Drever
1983
), which alters the frequency band of the detectors’ sensitivity (typically to give broader-band sensitivity); (iv) implementation of monolithic test-mass suspensions, which reduces the suspension thermal noise in the detectors’ sensitivity band by using the same low mechanical loss material (fused silica for LIGO and Virgo) for the suspension fibers as for the mirror substrate, and low-loss jointing techniques and thermoelastic nulling (S. M. Aston et al.
2012
; F. Travasso
2018
); (v) improved passive and active seismic isolation systems and sensors to reduce ground motion coupling to the detector and to damp suspension modes (S. Braccini et al.
2005
; F. Matichard et al.
2015
; S. J. Cooper et al.
2023
); and (vi) improved low thermal noise, low-absorption, high-reflectivity mirror coatings (G. M. Harry et al.
2007
; M. Granata et al.
2020
).
Throughout the advanced-detector era of GW observation, the LIGO and Virgo detectors have undergone a series of performance-improving detector upgrades and commissioning activities, details of which are given in this section. Detector upgrades include the installation of new hardware or upgrades to existing hardware in a detector. Examples of detector upgrades include the installation of new laser systems to provide higher power into the interferometer, installation of baffles to mitigate scattered light, and the injection of squeezed light to manipulate the quantum-noise-limited sensitivity of the detectors (F. Acernese et al.
2019
; M. Tse et al.
2019
). Commissioning activities cover a range of improvements to sensitivity and observing uptime of the instruments from targeted noise-hunting activities that remove glitches, lines, and broadband noise, to improved control schemes that mitigate instabilities and improve detector robustness.
Alongside this has been the effort to build and commission the KAGRA detector utilizing advanced technologies such as cryogenic cooling of the test masses and an underground location. This schedule of planned upgrades and commissioning activities between observing runs ensures that the maximal science output is achieved from the network. In terms of valuable scientific output, a successful upgraded detector that has been offline for a period of time rapidly overtakes a non-upgraded detector in continuous observational mode in terms of number of significant detections and the resolution and sky localization of high-interest signals.
The aLIGO and AdV detectors are designed to be dual-recycled Fabry–Perot Michelson interferometers with orthogonal kilometer-scale arms (F. Acernese et al.
2015
; J. Aasi et al.
2015a
). Each arm contains a Fabry–Perot optical cavity, and a beam splitter at the corner between the arms forms a Michelson interferometer that measures the change in the relative phase of the light induced by changes in the lengths of these cavities (K. S. Thorne
1987
; J. Y. Vinet et al.
1988
). Additional power-recycling and signal-recycling cavities are created by adding mirrors in the symmetric and antisymmetric ports of the interferometer. These improve sensitivity by building up the light power on the beam splitter and beneficially modifying the response of the interferometer, respectively (B. J. Meers
1988
). The input and end mirrors on each of the Fabry–Perot cavities are the test masses whose separations are affected by GWs. The mirrors are isolated by multistage pendulums that suppress the ground motion by more than 10 orders of magnitude at frequencies around 10 Hz. Monolithic fused silica fibers are used on the bottom stage of the suspension system to suppress thermal noise, and the mirrors themselves are fused silica substrates with low-loss, highly reflective coatings (S. M. Aston et al.
2012
).
Ground-based interferometers generally have the same fundamental limiting noise sources (P. R. Saulson
2017
; R. Weiss
2022
), with the response of each detector and the exact extent to which each noise limits sensitivity being specific to the detailed design of each detector. At low observational frequency below ∼10 Hz the detectors are limited by a combination of seismic noise, gravity gradient noise, suspension thermal noise, and quantum radiation pressure noise. Thermal noise in the mirror optical coatings is a significant noise source at intermediate frequencies ∼50 Hz to ∼200 Hz (G. M. Harry et al.
2007
), and at high frequencies, above ∼200 Hz, sensitivity is limited by the quantum shot noise.
In addition to these fundamental noise sources, the detectors are also limited by technical noise. This includes scattered-light noise, which occurs when some fraction of light is deflected from the interferometer beam path and is incident on another moving surface, varying the phase of the light; this couples noise into the interferometer readout if part of this light is reflected back into the main beam (T. Accadia et al.
2010
; D. J. Ottaway et al.
2012
). Interferometer control-system noise is when signals couple between the multiple feedback loops that control the degrees of freedom of the interferometer and requires complicated optimization of control loop parameters to mitigate (A. Buikema et al.
2020
). Laser noise due to fluctuations in the frequency, intensity, and pointing of the laser beam entering the interferometer is reduced with dedicated multistage stabilization systems to a level such that it does not impact the sensitivity of the detectors; however, suboptimal tuning of these stabilization systems can lead to laser noise affecting sensitivity (C. Cahillane et al.
2021
). Environmental noise is caused when environmental effects in the vicinity of the interferometer (e.g., seismic activity) couple into the measurement of the interferometer strain signal (F. Acernese et al.
2006
; A. Effler et al.
2015
; I. Fiori et al.
2020
; P. Nguyen et al.
2021
; A. Helmling-Cornell et al.
2024
). Detector commissioning seeks to mitigate such nonfundamental noise sources.
The key parameters of the LIGO, Virgo, KAGRA, and GEO detectors across the advanced era observing runs are given in Table
. The specific evolution of each detector in terms of detector upgrades and improvements is detailed in the remainder of this section.
Table 1.
Selected Optical and Physical Parameters of the LIGO Hanford (LHO), LIGO Livingston (LLO), Virgo, KAGRA, and GEO600 (GEO) Interferometers throughout the Advanced-detector Era
Observing Period
Interferometer
Input Laser Power
Power-recycling Gain
Signal Recycling
Squeezing
Suspension Type
O1
LHO
21 W
38
Silica
LLO
22 W
38
Silica
O2
LHO
26 W
40
Silica
LLO
25 W
36
Silica
Virgo
10 W
38
Steel
O3a
LHO
34 W
44
Silica
LLO
44 W
47
Silica
Virgo
18 W
36
Silica
O3b
LHO
34 W
44
Silica
LLO
40 W
42
Silica
Virgo
26 W
34
Silica
O3GK
GEO
3 W
1000
Silica
KAGRA
5 W
12
Sapphire
O4a
LHO
57 W
50
Silica
LLO
64 W
35
Silica
Note.
The input laser power is the power that would be measured at the power-recycling mirror (after the input mode cleaner) and is an estimate of the maximum level typically achieved during an observing period. Suspension types are monolithic fused silica fibers, sapphire fibers, or steel wires.
Download table as:
ASCII
Typeset image
4.1. LIGO Hanford and Livingston Observatories
LIGO is a US national facility comprising two US-based interferometric detectors in Hanford, Washington (LHO), and Livingston, Louisiana (LLO), each with 4 km arms. LIGO construction began in 1994. From 2002 to 2010, initial power-recycled Fabry–Perot Michelson interferometers were operated at these sites in a series of science runs S1−S6 (B. P. Abbott et al.
2009
; J. Aasi et al.
2015b
). During this period, LIGO also operated a second interferometer with 2 km arms at the Hanford site. Subsequently the aLIGO project resulted in a major overhaul of the interferometers to improve the capabilities of the detectors (J. Aasi et al.
2015a
), leading up to O1 and the first observation of GWs.
Across the observing runs certain areas have been the main focus of much of the detector improvement effort: (i) increasing the arm cavity power by increasing the injected laser power and the power-recycling gain while achieving stable operation, (ii) mitigation of scattered-light sources and coupling mechanisms, and (iii) reduction of quantum noise with addition of a squeezed-light system for O3 and the following improvements to the quantum-enhancement factor.
Both aLIGO detectors are operated with a lower injected laser power and lower power-recycling gain than the design goal (J. Aasi et al.
2015a
). The full amount of available laser power cannot be fully utilized, due to issues with maintaining long-duration stable locking of the interferometer owing to angular instabilities and point absorbers in the test-mass mirrors (A. F. Brooks et al.
2021
). This issue was the focus of commissioning efforts to continually improve the operating power in the cavity by optimizing the interferometer control loops (A. Buikema et al.
2020
) and reducing the presence of point absorbers in the mirrors. Stray-light control can be achieved by the addition of baffles to block unwanted beam paths and with active control of known scattered-light paths. The addition of a squeezed vacuum source at the interferometer’s output alters the quantum noise in the interferometer and, with the inclusion of a filter cavity, can produce frequency-dependent squeezing, which can be used to surpass the standard quantum limit on sensitivity of a laser interferometer (M. Tse et al.
2019
; D. Ganapathy et al.
2023
).
4.1.1. O1
The sensitivity and limiting noise sources of the LIGO detectors during O1 are described in B. P. Abbott et al. (
2016c
). Figure
shows a representative amplitude spectral density of the strain noise and the BNS range. In O1, the typical input power entering the power-recycling cavity was 21 W in LHO and 22 W in LLO, circulation of laser light in the power-recycling cavity increases the power on the beam splitter to be a factor of 38 times greater (the power-recycling gain), and a further increase in circulating power by a factor of 144 is achieved in the arms by the Fabry–Perot cavities. The laser input power and power-recycling gain during O1 and the later observing runs are given in Table
, alongside other detector parameters. An example of commissioning improvement is the investigation at LLO during O1 of recurring changes in the BNS range from 65 Mpc to 60 Mpc. By searching for correlation between the detector range and the hundreds of data channels recorded by aLIGO, it was found that the issue was caused by a malfunctioning temperature sensor. This sensor was replaced, resulting in a stabler increased range (M. Walker et al.
2018
).
4.1.2. O2
After O1, several improvements were made to both LIGO instruments (B. P. Abbott et al.
2017d
). Detector upgrades included installation of new mass dampers on the end-test-mass suspensions to dampen mechanical modes, improving the stabilization of laser intensity, and installing a new output Faraday isolator and higher quantum-efficiency photodiodes at the output port to improve signal detection efficiency in the readout system. Mitigation of scattered-light sources and other improvements to the detector sensitivity throughout O2 resulted in a BNS range improvement to 100 Mpc by the end of the run (D. Davis et al.
2021
). Commissioning tests during O2 on the LHO detector to increase the laser power to 50 W did not result in an overall improvement in performance of the 80 Mpc BNS range at the end of O1, due to point absorbers on one of the input test-mass optics, so the detector operated with 30 W input power. After O2, it was demonstrated that the use of witness channels to perform noise subtraction on the strain data was able to increase the BNS range by 20% (D. Davis et al.
2019
; J. C. Driggers et al.
2019
).
4.1.3. O3
Leading up to O3, several upgrades were made to the LIGO instruments (A. Buikema et al.
2020
). The most significant was the installation of an in-vacuum squeezed-light injection system at each site to inject squeezed vacuum into the interferometers to reduce shot noise at frequencies above 50 Hz (M. Tse et al.
2019
). The squeezer works by optically pumping a nonlinear crystal to modify the distribution of the quantum vacuum state that enters the interferometer (C. M. Caves
1981
; L. Barsotti et al.
2019
).
Between O3a and O3b, adjustments to the squeezing subsystem produced large sensitivity improvements. Among these were the installation of higher-power laser amplifiers with stable operation and output power over 70 W (N. Bode et al.
2020
). A program of installation of optical baffles was completed to improve stray-light control. The correlation of microseismic activity with scattered-light noise was determined to be primarily caused by a scattered-light path arising from large relative motion between the end test mass and the reaction mass that is immediately behind it (S. Soni et al.
2020
). A control loop that makes the reaction mass follow the end mass, implemented on 2024 January 7 at LLO and 2024 January 14 2024 at LHO, reduced the relative motion and mitigated the scattered-light noise (D. Davis et al.
2021
). At LHO, wind fences were installed to mitigate ground tilt induced by wind on the buildings (P. Nguyen et al.
2021
).
4.1.4. O4a
Several upgrades were implemented at LHO and LLO to improve the quantum-limited sensitivity of the detectors via improved quantum squeezing and higher intracavity power (A. G. Abac et al.
2024a
). Further upgrades to the laser amplification system were implemented with stable operation and output power over 140 W (N. Bode et al.
2020
). A new vacuum system to house a 300 m filter cavity was built at both detectors, along with an upgraded squeezing injection system to allow the injection of frequency-dependent squeezed vacuum to achieve quantum noise reduction across the detection frequency band (D. Ganapathy et al.
2023
; W. Jia et al.
2024
). Squeezing levels in O4a reached 5.8 dB at LLO and 4.6 dB at LHO, compared to the 2 dB to 3 dB achieved in O3 (E. Capote et al.
2025
). Test-mass mirrors were replaced at both observatories to remove point defects on the mirrors that contributed to control challenges and excess noise (A. Buikema et al.
2020
). This involved a replacement of both end test masses at LLO and the input
-arm test mass at LHO. Replacing these test masses allowed both observatories to approximately double the input power compared to O3, further improving the quantum-limited sensitivity of the detectors, due to higher circulating power in the Fabry–Perot arm cavities (A. Buikema et al.
2020
; E. Capote et al.
2025
).
Other upgrades to the LIGO detectors include improvements to the electronics in the GW signal readout chain, damping of baffles to mitigate scattered light, and improvements to electronics grounding (E. Capote et al.
2025
; S. Soni et al.
2025
). The photodetector transimpedance amplifiers were improved ahead of O4a using a design tested at GEO, resulting in a factor of 10 reduction in dark noise compared to O3 (H. Grote et al.
2016
). At both LIGO detectors, a septum window separating two vacuum volumes housing the output optics was removed, significantly reducing the coupling of acoustic noise. Baffles along the arm cavity and around vacuum pumps were previously identified to couple excess scattered light in O3 and were damped to reduce their motion and therefore shift the frequency of up-converted scattered light out of the sensitive band. Finally, injections into the building electronics ground demonstrated that many spectral features in the strain at LHO were the result of a fluctuating ground potential (E. Capote et al.
2025
; S. Soni et al.
2025
). The resistance to ground was reduced for several electronics chassis around the detector. Additionally, the voltage biases of the test-mass electrostatic drives were adjusted to minimize the electronics noise coupling further (E. Capote et al.
2025
).
Detector commissioning ahead of O4a also focused on optimization of the auxiliary controls to reduce technical noise that limited the detectors at low frequency in O3 (A. Buikema et al.
2020
). Alignment control noise was reduced by a factor of 10 and length control noise by a factor of two at both detectors near 20 Hz (A. Buikema et al.
2020
; E. Capote et al.
2025
). Significant improvements to the controls included the upgrade to a camera servo system that requires no line injection to sense the alignment of the main detector optics (E. Capote et al.
2025
). Suspension local control loops were reoptimized to focus on noise suppression above 5 Hz, reducing both noise directly coupled to the strain and noise that couples indirectly through the length and alignment controls (E. Capote et al.
2025
). Both detectors were also limited by unmitigated beam jitter noise that was well witnessed by auxiliary sensors (E. Capote et al.
2025
). As such, front-end infrastructure using the non-stationary estimation and noise subtraction (NonSENS) code (G. Vajente
2018
) was implemented to perform noise cleaning in low latency, increasing detector sensitivity by up to 5 Mpc in BNS range (G. Vajente et al.
2020
; G. Vajente
2022
; E. Capote et al.
2025
).
4.1.5. Beyond O4
Looking to the future, there is ongoing construction of LIGO-India (T. Souradeep et al.
2017
), a third LIGO interferometer to be built in the Hingoli district of Maharashtra, India. This facility will be based on aLIGO hardware and design, and its location will provide a significant improvement in the sky localization of GW sources (C. Pankow et al.
2020
; M. Saleem et al.
2022
; S. Pandey et al.
2025
).
In parallel, there are plans underway to upgrade the existing LIGO detectors (and eventually LIGO-India) to Advanced+ LIGO (A+) sensitivity (B. P. Abbott et al.
2020a
; S. J. Cooper et al.
2023
). The A+ upgrade to the LIGO detectors is a series of detector upgrades utilizing improved technology that has been developed in parallel to the observing runs. The inclusion of frequency-dependent squeezing was originally planned as an A+ upgrade but was implemented ahead of O4a at both sites (E. Capote et al.
2025
). Other A+ upgrades, which will be implemented for future observing runs, include new optics with lower noise and loss, improved sensors for controlling the mirrors, a new pre-mode cleaner to reduce beam jitter noise, improved output mode cleaners with lower loss, and a balanced homodyne readout system that allows for better readout control of the interferometer signal.
A post-O5 upgrade, referred to as LIGO A
(A
), explores more transformative changes in detector design, with the goal of increasing the sensitivity to the limits of what is possible with the existing infrastructure of the LIGO detectors (P. Fritschel et al.
2024
). Detector improvements that facilitate the achievement of the A
sensitivity include the upgrade of the laser injection system to deliver more power into the interferometer and an improved system for the thermal compensation of the test-mass mirrors. The test-mass mirrors will be replaced with heavier masses with improved optical coatings, and A
targets an improved exploitation of the quantum noise reduction from the squeezed-light system. The A
configurations are natural outgrowths of A+ configurations and will serve as pathfinders for the next-generation Cosmic Explorer concept (M. Evans et al.
2021
). Additionally, it has much technological overlap with Advanced Virgo+ (AdV+) and Virgo_nEXT (Section
4.2
), which presents the possibility of collaborating on developing these technologies.
4.2. Virgo Observatory
The Virgo interferometer, located in Cascina (Italy), is the largest European GW detector, designed in its AdV Phase I as a 3 km dual-recycled Fabry–Perot Michelson interferometer (F. Acernese et al.
2015
). Construction of Virgo started in 1997 and was completed in 2003 (F. Acernese et al.
2005
). Four science runs of the initial Virgo interferometer, VSR1−VSR4, took place between 2007 and 2011. These were followed by upgrades leading to the AdV design operated during O2 and O3. Subsequently, further upgrades leading to AdV+ were planned to take place in two phases, the first for operation during O4 and the second for operation during O5. A proposed next-generation upgrade planned post-O5, Virgo_nEXT, would provide further sensitivity by pushing current facilities to their limit and would serve as a pathfinder for future ground-based GW detectors.
The first-generation Virgo detector (T. Accadia et al.
2012a
) observed jointly with the initial LIGO detector’s fourth and fifth science runs. After several years of commissioning, from 2007 May to 2007 October the first scientific data run VSR1 (along with LIGO) took place, for which a BNS range of 4 Mpc was achieved (F. Acernese et al.
2008
). At this stage, Virgo was a power-recycled Fabry–Perot Michelson interferometer with a 20 W laser source. The second Virgo science run, VSR2 (also along with LIGO), from 2009 July to 2010 January (T. Accadia & B. L. Swinkels
2010
), was preceded by a set of major improvements to mitigate scattered light and to improve the light injection system.
The replacement of the four payloads in the Fabry–Perot cavities was the major improvement in preparation for the third Virgo science run VSR3, from 2010 July to 2010 October (T. Accadia et al.
2012b
). Issues arising from thermal noise due to improperly aligned suspension wires and degraded contrast resulting from differing radii of mirror curvature were addressed leading up to VSR4, from 2011 June to 2011 October, during which Virgo achieved a BNS range of 12 Mpc. While the three previous VSRs were aligned with initial LIGO science runs, Virgo took data during this run together with GEO. The main upgrade consisted of the installation of the central heating radius of curvature correction (CHRoCC) on both end mirrors, which allowed the radius of curvature of the mirrors to be controlled in real time (T. Accadia et al.
2013
). This system was designed to correct the thermal lensing effect in the mirrors, which had been a significant source of noise in the interferometer. Virgo stopped observing in 2011 for the AdV upgrade.
4.2.1. O2
After these four science runs, major modifications were made to the optical layout to increase the broadband sensitivity by up to an order of magnitude (B. P. Abbott et al.
2017e
). These upgrades marked the transition from Virgo, a first-generation interferometer, to AdV, a second-generation GW detector (F. Acernese et al.
2015
). The installation of AdV started in 2011 and was completed in 2016. AdV was planned as a dual-recycled interferometer with 125 W entering the interferometer, though signal recycling was not implemented until O4. The main improvements included a ∼3-fold increase in the arm cavity finesse (a measure of how long light stays within the cavity), 42 kg fused silica test masses with ultralow absorption and high homogeneity, new stray-light control using diaphragm baffles and a vibration isolation system, an improved thermal compensation system with double axicon CO
laser projectors and ring heaters, an improved output mode cleaner with two cascaded monolithic bow-tie resonators, and a new design of payloads triggered by the need to suspend heavier mirrors, baffles, and compensation plates.
The several months of commissioning that started at the end of 2016 October achieved the target early-stage BNS range of 8 Mpc in 2017 April with 13 W input laser power. After an intense campaign of noise investigations, AdV sensitivity was considered sufficient to join aLIGO during the O2 observing run in 2017 August (F. Acernese et al.
2018
). During O2, the AdV BNS range reached 30 Mpc. As noted in Section
3.2
, the low-frequency Virgo sensitivity during O2 was limited by thermal noise from metallic suspension wires, which were implemented as a fallback option owing to the frequent failure of monolithic suspensions after the installation of the main AdV upgrades.
4.2.2. O3
The most important Virgo upgrades for O3 were the mitigation of suspension thermal noise by installation of monolithic suspensions and the mitigation of quantum noise by increase of input laser power and by injection of frequency-independent squeezing. An in-air optical parametric amplifier was implemented in the Virgo interferometer before the start of O3a, and squeezing injections were maintained during the whole of O3, with a 3 dB gain in sensitivity at high frequency (F. Acernese et al.
2019
2020
).
Throughout O3, work was continuously carried out to improve the Virgo sensitivity in parallel with the ongoing data taking. Dedicated tests were made during planned breaks in operation (commissioning, calibration, and maintenance), and in-depth data analysis of these tests was performed between breaks to ensure continual improvement. In particular, the 1-month commissioning break between the O3a and O3b observing periods was used to get a better understanding of the Virgo sensitivity and of some of its main limiting noises (R. Abbott et al.
2023
). This effort culminated during the last 3 months of O3b.
The most significant change to the Virgo configuration between O3a and O3b was the increase of the input power from 18 W to 26 W. As with the LIGO detectors, it was found that the optical losses of the arms increased following the increase of the input power.
New high quantum efficiency photodiodes that had been installed at the output (detection) port of the interferometer prior to the start of O3a were found to increase the electronics noise at low frequency. These were improved at the end of 2020 January during a maintenance period, by replacing pre-amplifiers. The electronic noise disappeared completely, leading to a BNS inspiral range gain of ∼2 Mpc.
Finally, in the period from the end of 2020 January to the beginning of 2020 February the alignment was improved for the injection of the squeezed light into the interferometer (F. Acernese et al.
2019
2020
), a critical parameter of the low-frequency sensitivity. By mitigating scattered-light noise, the BNS range increased by 1 Mpc to 2 Mpc.
4.2.3. O4
The AdV+ interferometer layout (F. Acernese et al.
2023b
) was designed as a two-step project, for O4 (Phase I) and O5 (Phase II), with the aim to reduce quantum and thermal noise, respectively. The main upgrades for O4 included a new high-power fiber laser amplifier replacing the former solid-state amplifier, to reach 125 W; the implementation of an additional recycling cavity at the output of the interferometer, the signal-recycling cavity, to broaden the sensitivity band; an output mode cleaner with increased finesse; a frequency-dependent squeezing system to reduce quantum noise at all frequencies; a network of seismic and acoustic sensors for Newtonian noise monitoring; and a Newtonian calibrator for improved calibration accuracy. These upgrades, while meant to improve the detector sensitivity, also increased the difficulties in controlling the interferometer in the presence of optical defects (from both thermal aberration and cold defects), due to the marginal stability of the Virgo recycling cavities (F. Acernese et al.
2023b
). Efforts were put forward to control the dual-recycled interferometer’s sensitivity to small defects. For instance, a CHRoCC (T. Accadia et al.
2013
) was installed in 2022 to create a thermal lens on the pick-off plate so as to match the power-recycling cavity to the arm cavities. These turned out not to be enough to have a stable interferometer working at the targeted laser power. High-order modes were resonant in the cavities, and these strongly complicated stable operations. The laser input power was decreased to 18 W to improve interferometer control and stability. The various changes on the configuration and attempts to reach stable operations prolonged the anticipated commissioning period between runs. Thus, AdV+ could not join for the O4a observing run. Instead, continued commissioning allowed AdV+ to reach a BNS range of 54 Mpc, with which it joined O4b.
4.3. KAGRA Observatory
The KAGRA interferometer, situated in Japan’s Kamioka mine, is the only large-scale GW detector in East Asia. It is designed as a cryogenic, 3 km, dual-recycled Fabry–Perot Michelson interferometer. The KAGRA project was funded in 2010, construction began in 2012, and tunnel excavation was completed in 2014 (T. Akutsu et al.
2021
). Following installation and assembly in the tunnel, two operations using temporary detector configurations served as key project milestones: the initial-phase KAGRA (iKAGRA) operation in 2016 April (T. Akutsu et al.
2018
), and the baseline-design KAGRA (bKAGRA) phase-1 operation in 2018 April. During the bKAGRA phase-1 operation, both cryogenic technology and the large-scale vibration isolation systems of KAGRA were successfully demonstrated (T. Akutsu et al.
2019
). By the summer of 2019, the primary installation of instruments was completed, allowing for the commissioning of the detector to begin immediately. In 2019 October, a memorandum of agreement forming the LVK was signed, and the LVK international observation network was launched (P. Brady et al.
2019
). After that, the commissioning phase continued until 2020 March, marking the commencement of the detector’s scientific operation.
4.3.1. O3GK
O3GK was a joint observation conducted with the GEO detector in 2020 April (H. Abe et al.
2023
), just after the early termination of O3b. The O3GK operation marked the first joint observation between KAGRA and GEO. This collaboration aimed to improve the detection capabilities by combining data from both detectors. The optical configuration used during O3GK was a power-recycled Fabry–Perot Michelson interferometer, with one room-temperature sapphire test mass and the others set around 250 K.
During the O3GK operation, KAGRA observed for approximately 7.3 days, with a strain sensitivity of 3.0 × 10
−22
Hz at 250 Hz. The BNS range was about 0.7 Mpc (R. Abbott et al.
2022
). The sensitivity of KAGRA during O3GK was influenced by various noise sources, including sensor noise from local controls of the vibration isolation systems, acoustic noise, shot noise, and laser frequency noise (H. Abe et al.
2023
). Understanding these noise contributions was crucial for planning future improvements to the detector’s sensitivity. To enhance its performance, KAGRA plans to implement hardware upgrades and refine its noise mitigation strategies. These improvements aim to extend the detection range and increase the precision of GW observations.
4.3.2. O4
On 2024 January 1 a 7.5 mag earthquake struck near the KAGRA site, marking the most significant seismic event in the area in the past century. As a result, 10 seismic noise isolators sustained damage but have since been restored. While further investigation and improvements were still needed for some vacuum and facility-related components, partial commissioning began in 2024 July. By 2024 October, all earthquake-related repairs were completed, followed by noise reduction efforts across multiple domains. During the October commissioning, KAGRA achieved a significant improvement on the BNS range using a power-recycled Fabry–Perot Michelson interferometer configuration with DC readout. Further commissioning tasks have been performed, including reduction of suspension local control noise through updates to the control filters, reduction of photodiode dark noise below the shot noise level by mitigating electrical coupling from other electronic devices, reduction of quantum shot noise by increasing the laser power to above 10 W, reduction of thermal noise by cooling the mirrors and their suspensions to below 100 K, and reduction of frequency noise and acoustic noise through hardware improvements and control system updates. Following these improvements, KAGRA began operating in O4c on 2025 June 11.
4.4. GEO Observatory
The GEO detector is a Michelson interferometer with two nearly orthogonal 600 m arms (B. Willke et al.
2002
). Rather than Fabry–Perot cavities, GEO uses folding in the arms, in which the light traverses each arm twice, to give an optical length of 1200 m for each arm. GEO is sensitive to GWs in the 50 Hz to 1.5 kHz frequency range. GEO began operation in 2001. From 2009 to 2014, it underwent a series of upgrades, the GEO-HF program, that resulted in a factor of 4 improvement in sensitivity at high frequencies (H. Grote
2010
; K. L. Dooley et al.
2016
). In 2010, squeezed vacuum injection was first applied in GEO (J. Abadie et al.
2011
), and the first long-term application of squeezing was demonstrated in GEO in 2011 (H. Grote et al.
2013
). Subsequently, 6 dB of squeezing (equivalent to a factor of 4 increase in light power) has been achieved (J. Lough et al.
2021
).
GEO has served as an advanced development center and test bed for technologies that were subsequently incorporated in larger detectors (C. Affeldt et al.
2014
), such as dual-recycling (G. Heinzel et al.
2002
), monolithic suspension (S. Goßler
2004
), thermal compensation (H. Luck et al.
2004
), homodyne detection (DC readout; S. Hild et al.
2009
), and squeezed-light injection (J. Abadie et al.
2011
).
4.4.1. Astrowatch
Following the first-generation LIGO and Virgo science runs, GEO embarked on an astrowatch program of near-continual data collection (when the detector is not being used for instrument science research) as the sole observing detector (K. L. Dooley
2015
). This mode of operation has continued since 2007 and allows for searches for GWs associated with external events such as gamma-ray bursts, neutrino detections, or nearby supernovae, occurring outside of other detectors’ observing periods (e.g., A. G. Abac et al.
2024b
).
4.4.2. O3GK
As described in Section
3.3
, a 2-week-long joint observing run with the GEO and KAGRA detectors took place in 2020 April, during which GEO operated with an 80% duty cycle (10.9 days of operation) and a BNS range of 1.1 Mpc (R. Abbott et al.
2022
). The laser power injected was about 3 W, which led to about 3 kW of circulating power in the power-recycling cavity, or 1.5 kW of circulating power per arm (C. Affeldt et al.
2014
; K. L. Dooley et al.
2016
). Bilinear noise subtraction resulted in modest improvement in sensitivity and data quality (N. Mukund et al.
2020
). Since GEO and KAGRA had similar sensitivity during O3GK, this joint run enabled searches for GW transient signals occurring simultaneously in both detectors, though no significant events were observed (R. Abbott et al.
2022
).
5. Review of Observed Transient Sources
The GWTC includes all observed transient GW candidates reported by the LVK. It is most likely that the significant candidates in GWTC-4.0 have an astrophysical origin and were produced by CBC sources (the remaining less significant candidates are largely nonastrophysical). This section provides a foundational overview of transient GW signals, especially those from CBCs, for use in interpreting the catalog’s contents and for reference in companion articles. We first provide a short overview of the basic physics of GWs and then provide an introduction to the CBC sources to be used as a reference for companion articles. Additional detail can also be found in M. Maggiore (
2007
2018
) and J. D. E. Creighton & W. G. Anderson (
2011
).
5.1. Gravitational Waves
In metric theories of gravity, such as GR, the local gravitational field can be described in terms of six independent degrees of freedom that represent the relative accelerations of a collection of nearby freely falling observers (F. A. E. Pirani
1956
; C. W. Misner et al.
1973
). Plane wave solutions to the linearized gravitational field equations (A. Einstein
1916
) represent the weak GWs in the far-field region (where the observer is far from the source and the gravitational field is treated as a perturbation to Minkowski spacetime) that are observed by GW detectors. The vacuum Einstein field equations of GR then further restrict the degrees of freedom of the plane wave solutions to two transverse polarizations that propagate at the speed of light (A. S. Eddington
1922
). These are called the
plus
(+) polarization and the
cross
(×) polarization. In a suitably chosen set of coordinates, known as the
transverse-traceless gauge
(C. W. Misner et al.
1973
; K. S. Thorne
1987
), which is akin to the radiation gauge in classical electromagnetism, the perturbation to the Minkowski metric for these two polarizations is given by the two functions of spacetime
and
, respectively. These polarizations represent two spin-2 purely transverse tensor modes (S. Weinberg
1972
). The transverse-traceless gauge is a useful choice because world lines that are the histories of fixed points in these spatial coordinates are geodesics of the perturbed spacetime (J. B. Hartle
2021
). Thus, changes in time in the metrical distance between fixed spatial coordinate locations, which is described by the time derivatives of
and
, represent the deviation of the geodesics at these locations. Therefore,
and
are the physical (observable) degrees of freedom of a GW.
From an observational point of view, GW signals are broadly classified as
persistent
or
transient
. The main classes of persistent GWs include quasi-monochromatic signals, e.g., as produced by rotating NSs having a nonaxisymmetric mass distribution (M. Zimmermann & E. Szedenits
1979
), and continuous stochastic superpositions of GWs from numerous unresolved independent sources (J. D. Romano & N. J. Cornish
2017
). Here we focus on the transient signals that are cataloged in GWTC.
5.1.1. Transient GW Signals
transient
GW is one that registers a signal of short duration (much less than the duration of the observing run) within the sensitivity band of the GW detectors. Such GWs can be characterized by their
geocentric arrival time t
geo
, the time at which some fiducial point in the GW’s waveform (e.g., its peak amplitude) passes through Earth’s center. We expect that transient GWs will be observed as plane waves originating from a particular point in the sky, usually given in terms of the equatorial celestial coordinate system of R.A.
and decl.
, with a normal vector −
along this line of sight. A key task for multimessenger astronomy with GWs is the reconstruction of the source location, which facilitates follow-up with other astronomical facilities (B. P. Abbott et al.
2020a
).
A network of detectors spaced at different locations on Earth can observe the difference in the time of arrival of the fiducial point in the waveform arising from the propagation of the plane wave across Earth and thereby reconstruct the direction of propagation
(S. Fairhurst
2009
; J. D. E. Creighton & W. G. Anderson
2011
; S. Fairhurst
2011
; L. P. Singer & L. R. Price
2016
). Such triangulation is the main way in which the sources of transient GWs are localized. Hence, uncertainty in the sky location of the source, ΔΩ, partially results from the measurement uncertainty of the arrival time in each detector (S. Fairhurst
2011
). A single detector provides no ability to determine the sky location of a source for transient signals lasting much less than a day and having wavelengths much longer than the size of the detector (as is the case for all candidates reported in GWTC-4.0); however, with two detectors, the difference in times of arrival identifies a circle on the celestial sphere, centered on the axis separating the detectors, on which the wave’s origin may lie. The presence of a third detector whose location is not colinear with the other two then identifies the source position to one of two points on the sky mirrored across the plane containing these three detectors. A fourth detector, not coplanar with the other three, finally resolves the location of the source to a single point on the sky. Additional localization information can be provided by coherently combining the observed GW signals from an array of detectors as described below. For some types of transient sources having known GW emission, such as CBCs, it is also possible to estimate the distance to the source from measurements of the wave amplitude (C. Cutler & E. E. Flanagan
1994
). In such cases, there is a volume localization uncertainty Δ
as well (L. P. Singer et al.
2016
; W. Del Pozzo et al.
2018
).
GW detectors such as the LIGO, Virgo, and KAGRA detectors are designed to sense changes in the difference of the lengths of their orthogonal arms, Δ
= Δ(
), caused by GWs, via laser interferometry. These ⌞-shaped Michelson interferometers measure the difference in phase of coherent light, split at a beam splitter located at the vertex of the ⌞, after traversing the arms and recombining at the beam splitter Δ
= 2
, where
is the wavelength of the laser light (G. E. Moss et al.
1971
; R. L. Forward
1978
; R. Weiss
2022
). For GW transients having durations much less than a day and wavelengths much greater than the length
of the detector arms, the strain induced on the arms is a linear combination of plus- and cross-polarizations of the metric perturbation (R. L. Forward
1978
; V. N. Rudenko & M. V. Sazhin
1980
; B. F. Schutz & M. Tinto
1987
; K. S. Thorne
1987
Here
and
are the detector’s beam pattern functions, which depend on the position on the sky from which the GW source is located, a polarization angle that defines the axes of the plus- and cross-polarization in the wave frame, the Earth rotation angle at the time of the signal’s arrival, and the location, orientation, and geometry of the detector on Earth’s surface (W. Anderson et al.
2001
). Figure
shows the sky coordinate conventions used. For long-duration signals, effects of Earth’s rotation need to be included; for short-wavelength signals, the beam pattern functions also depend on the wavelength of the GWs (M. Rakhmanov et al.
2008
; M. Rakhmanov
2009
). Neither of these effects is significant in any of the transient signals detected to date. The amplitudes of the strains measured in a network of detectors provide additional information about the location of the source of the GW if the polarization of the GW is known owing to the dependence of the beam pattern functions on the position of the source on the sky (e.g., L. P. Singer & L. R. Price
2016
). This information helps to break degeneracies in sky localization; for instance, with only two detectors, the source is typically localized to an extended arc or ring on the sky, but the amplitude response can help reduce this uncertainty to specific regions along that ring.
Figure 4.
Relationship between the sky location in equatorial coordinates, the polarization angle, and the GW coordinate frame. The direction from the source to Earth is
, and the vector
defines a reference direction on the transverse plane called the wave plane. The location of the source on the sky in the equatorial coordinate system is given by its R.A.
and decl.
. The polarization angle
is the angle counterclockwise about
between the equatorial plane and
. Also shown is the Greenwich sidereal time (GST), the angle between the first point of Aries
and the prime meridian, and the Greenwich hour angle (GHA) of the source, GHA = GST −
. NCP is the north celestial pole.
Download figure:
Standard image
High-resolution image
Table
summarizes the parameters associated with a general transient plane GW, a detector’s response to such a GW, and the accuracy of localization of the wave’s source.
Table 2.
Parameters Describing a Transient Plane GW, a Detector’s Instantaneous Antenna Response in the Long-wavelength Limit, and Measures of Inferred Localization of the Signal on the Sky
Parameter Name
Symbol
Notes [Dimensions]
Plus- and cross-polarizations
Functions describing the plus-polarization (
) and cross-polarization (
) of the metric perturbation [dimensionless]
Geocentric arrival time
geo
Time of arrival at the center of Earth of some fiducial point in the GW’s waveform, normally close to the peak amplitude of the waveform [time]
Propagation direction
Direction of propagation of the GW, the unit vector normal to the planar wavefronts; the direction to the source of the wave is −
[dimensionless]
Right ascension (R.A.)
Azimuth of the sky location of the source of the GW in the equatorial coordinate system (see Figure
) [angle]
Declination (decl.)
Latitude of the sky location of the source of the GW in the equatorial coordinate system (see Figure
) [angle]
Polarization angle
Orientation of the axes defining the plus- and cross-polarization on the transverse plane of the GW relative to the line of nodes of this plane and Earth’s equatorial plane (see Figure
) [angle]
Plus and cross beam patterns
Antenna response of a detector to the plus-polarization (
) and the cross-polarization (
), functions of the sky location of the source, the polarization angle, the geocentric arrival time of the signal, and the location, orientation, and geometry of the detector on Earth (W. Anderson et al.
2001
) [dimensionless]
Detector strain
GW-induced strain on a detector, Equation (
); the GW readout of the detector is proportional to this quantity [length/length]
Sky area
ΔΩ
Localization area, typically taken as the 90% credible area; if results at different CLs are quoted, these are indicated with a subscript, e.g., ΔΩ
50
is the 50% credible area [solid angle]
Volume localization
Localization volume (for signals where the distance to the source can be estimated), typically taken as the 90% credible volume; if results at different CLs are quoted, these are indicated with a subscript, e.g., Δ
50
is the 50% credible volume [volume]
Download table as:
ASCII
Typeset image
LVK Catalog of Observed Transient GW Signals
. In the companion article A. G. Abac et al. (
2025b
), we describe the significant transient GW candidates in GWTC-4.0, highlighting those observed in O4a. GWTC-4.0 also provides the inferred properties of the GWs, as well as their sources, e.g., the masses and spins of the binary components under the assumption than the GWs were produced by CBCs. The GWTC dataset, along with other open data products, is detailed in the companion article A. G. Abac et al. (
2025i
).
5.1.2. Gravitational Lensing of GWs
Like electromagnetic waves, GWs can be gravitationally lensed by massive objects, e.g., galaxies, interposed between the GW source and the observer. The GW polarization tensor is parallel propagated along geodesics (C. W. Misner et al.
1973
) and is little affected by the gravitational potential of the lensing mass, so it is sufficient to consider scalar diffraction theory (R. Takahashi & T. Nakamura
2003
). In a thin-lens approximation, the bending of the trajectory of the GW propagation occurs on a lens plane orthogonal to the line of sight and at the distance of the lensing body. With
and
as the coordinates of the lens plane, at each point on this plane there is an observed time delay
) relative to straight-line motion with no lens, corresponding to the path from the source to that point on the lens plane to the observer. This delay accounts for the gravitational field of the lens. GWs are deflected by a gravitational lens with the time delay field on the lens plane determining the complex phases of the interfering partial waves used to compute a frequency-dependent complex-valued magnification factor. This factor is given by the Fresnel–Kirchhoff diffraction formula
where the integral is over the lens plane,
is the observed GW frequency, (1 +
is the blueshifted frequency of the GW on the lens plane (
is the redshift of the lens), and the distances
OS
OL
, and
LS
are the distances between the observer (us) and the GW source, between the observer and the gravitational lensing object, and between the lensing object and the source, respectively (P. Schneider et al.
1992
). In a cosmological setting, these are
angular diameter
distances (D. W. Hogg
1999
). The geometric optics limit corresponds to Fermat’s principle, in which the geodesic paths taken by GWs are those passing through the lens plane at extrema of this two-dimensional time delay field
), which may be local minima, which produce
Type I images
, local maxima, which produce
Type III images
, or saddle points, which produce
Type II images
(P. Schneider et al.
1992
). Equation (
) is evaluated in this high-frequency limit by use of the stationary phase approximation to obtain
where
and
are the magnification amplitude and observed time delay of image
, and
is 0, 1/2, or 1 for Type I, Type II, and Type III images, respectively. Therefore, such images are magnified or demagnified by a factor that is positive for Type I images and negative for Type III images, while the gravitational waveform of Type II images is additionally distorted, appearing as the Hilbert transform of the original waveform (L. Dai & T. Venumadhav
2017
; J. M. Ezquiaga et al.
2021
). For GW transients, the images are a set of repeated signals from the same event observed at different times, with the delays determined by the differences in the time delay field on the lens plane of the different images. These delays are typically minutes to months for galaxy lenses (S.-S. Li et al.
2018
; K. K. Y. Ng et al.
2018
; M. Oguri
2018
) and up to years for galaxy cluster lenses (G. P. Smith et al.
2017
2018
; A. Robertson et al.
2020
; D. Ryczanowski et al.
2020
). The images also appear at different points on the sky, with arcminute-scale separation, but GW detectors have insufficient sky localization capabilities to distinguish them in this way. When gravitational lensing can be described in this geometric optics limit, it is referred to as strong lensing.
However, when the wavelength of the GW is comparable to the Schwarzschild radius of the gravitational lens, the geometric optics limit of Fermat’s principle is no longer valid, and the Fresnel–Kirchhoff diffraction formula of Equation (
) must be used to determine the complex-valued and frequency-dependent magnification factor. Such lensing effects can result from objects having masses up to 10
, and searches can be done in a modeled (e.g., M. Wright & M. Hendry
2021
) or phenomenological (A. Liu et al.
2023
) way.
Searches for Gravitational Lensing Signatures in GW Signals
. In the companion article A. G. Abac et al. (
2025h
), we present searches for gravitational lensing signatures in GWTC-4.0. Such signatures sought include multiple images from strong lensing, individual Type II strongly lensed images, and waveform distortions induced by point-mass lensing.
5.1.3. GW Polarization and Propagation in Alternative Theories of Gravity
In GR, plane GW perturbations to flat spacetime propagate at the speed of light and contain two transverse polarizations. However, in modified theories of gravity extending beyond GR, additional polarizations may be present, including two transverse-longitudinal spin-1 vector modes, a transverse spin-0 scalar mode, and a longitudinal spin-0 scalar mode (D. M. Eardley et al.
1973a
1973b
; C. M. Will
2018
). With multiple detectors, it is possible to test for such additional polarizations (B. F. Schutz
1986
). A linear combination of strain data from three detectors can be formed in which any GW signal from a known sky location and containing only plus- and cross-polarizations is canceled (Y. Guersel & M. Tinto
1989
; S. Klimenko et al.
2008
; P. J. Sutton et al.
2010
; J. D. E. Creighton & W. G. Anderson
2011
; I. C. F. Wong et al.
2021
). Any residual GW signal found in such a null space would provide evidence for the presence of vector or scalar non-GR polarizations.
In addition, in alternative Lorentz invariance violating theories of gravity or in which the graviton is massive, GWs are dispersive. Certain theories of dark energy also result in dispersive GW propagation (C. de Rham & S. Melville
2018
; T. Baker et al.
2022
; I. Harry & J. Noller
2022
). The GW dispersion relation between the frequency
and the wavelength
(one where they are not inversely proportional) leads to phase speeds and/or group speeds that differ from the speed of light. Such propagation effects can be measured for a known waveform by the anomalous arrival times of different frequency components. A common parameterized dispersion relationship is motivated by a modified energy–momentum relationship for the graviton of the form (S. Mirshekari et al.
2012
where
is a GR-violating parameter having dimensions of (energy)
2−
. For de Broglie waves,
= 2
πℏf
and
= 2
πℏ
, where 2
πℏ
is the Planck constant. Such a modified energy–momentum relation leads to a dispersion relation in which the phase velocity
is given by
where the phase velocity is related to the frequency and the wavelength of the GW,
λf
. The group velocity,
, determines the difference in arrival times of different frequency components of the GW after propagation from its source to the observer. For small deviations from GR (
), the group velocity is frequency dependent with
Special cases include (i) a graviton of mass
≠ 0 for which
= 0,
, and
where
= 2
πℏ
/(
) is the Compton wavelength of the graviton, and (ii) the case in which GWs are nondispersive but propagate at a speed different from the speed of light for which
= 2 and
Stringent bounds on the latter are provided by the close temporal association of the BNS signal GW170817 and the gamma-ray burst GRB 170817A (the gamma rays arriving less than 2 s after the BNS GW merger signal), resulting in ∣
∣ ≲ 10
−14
(B. P. Abbott et al.
2017f
).
The Einstein–Hilbert action of GR contains second derivatives of the spacetime metric (S. Weinberg
1972
; C. W. Misner et al.
1973
; R. M. Wald
1984
; S. M. Carroll
2019
). Standard model extensions having modified actions containing third derivatives of the metric can produce CPT-violating terms in the gravitational field equations, which can produce birefringence effects in which different GW helicities propagate with different phase velocities (V. A. Kostelecky
2004
; V. A. Kostelecký & M. Mewes
2016
; M. Mewes
2019
; L. Haegel et al.
2023
). Other theories of gravitation also have GWs with birefringent propagation (T. Zhu et al.
2024
). Such birefringence leads to a frequency-dependent rotation of the GW polarization angle.
Both GW birefringence and the modified GW dispersion relation can potentially be anisotropic, where the magnitude of the observed effect depends on the direction to the source.
Tests of GR: GW Polarization and Propagation
. In the companion article A. G. Abac et al. (
2025d
), we test the GR prediction of the polarizations of GWs by searching for evidence of vector- or scalar-polarization modes in observed GW signals. Meanwhile, A. G. Abac et al. (
2025e
) present tests of a modified dispersion relation and of anisotropic birefringence using GW signals from CBCs, for which it is assumed that the GW near the source is described by GR to a good approximation, but the waveform is affected during propagation.
5.2. Compact Binary Coalescence
Binaries consisting of two BHs (BBH systems), consisting of two NSs (BNS systems), or in which one component is an NS and the other a BH (NSBH systems), have all been observed by the LVK (B. P. Abbott et al.
2016a
2017a
; R. Abbott et al.
2021c
). The detectable signal produced by such systems arises from the late stage of orbital decay, driven by GW emission, and by the ensuing merger of the binary components and the settling of the resulting object (an NS or BH) to a final, stationary configuration (K. Chatziioannou et al.
2024
).
Table
provides a list of parameters used to describe CBCs.
Table 3.
Parameters Describing a CBC System with Quasi-circular Orbits
Parameter Name
Symbol
Notes [Dimensions]
Primary and secondary masses
Mass of the more massive (
) and less massive (
) body in the system,
[mass]
Chirp mass
See Equation (
13
) [mass]
Total mass
[mass]
Final mass
Mass of the remnant [mass]
Mass ratio
≤ 1 [dimensionless]
Symmetric mass ratio
[dimensionless]
Energy radiated
rad
rad
= (
[energy]
Peak luminosity
peak
Peak GW luminosity, typically 0.1% of the Planck luminosity (
Planck
) for BBH coalescences [power]
Primary and secondary spin vectors
Spin angular momentum of the primary (
) and secondary (
) [angular momentum]
Primary and secondary dimensionless spin magnitudes
1,2
≤ 1 for Kerr BHs primary/secondary [dimensionless]
Remnant dimensionless spin magnitude
where
is the magnitude of the remnant’s spin angular momentum;
≤ 1 for a Kerr BH remnant [dimensionless]
Newtonian orbital angular momentum
Instantaneous orbital angular momentum about the center of mass; defines
-direction for spin coordinates [angular momentum]
Total angular momentum
[angular momentum]
Primary and secondary tilt angle
Angle between
1,2
and
[angle]
Spin azimuthal angle difference
12
Angle measured clockwise about
from
× (
) to
× (
) [angle]
Effective inspiral spin parameter
eff
See Equation (
15
) [dimensionless]
Effective precession spin parameter
See Equation (
16
) [dimensionless]
Orbital inclination angle
Angle between
and the direction to Earth
(see Figure
) [angle]
Source inclination angle
JN
Angle between
and the direction to Earth
[angle]
Viewing angle
[angle]
Orbital phase
Phase of a binary’s orbit, the angle on the orbital plane between the separation vector (the position vector of the primary minus the position vector of the secondary) and the line of nodes,
(see Figure
) [angle]
Coalescence phase
Orbital phase, the angle on the orbital plane between the separation vector (the position vector of the primary minus the position vector of the secondary) and the line of nodes,
, at a point in the evolution corresponding to the point in the waveform used to define
geo
(see Table
) [angle]
Angular diameter distance
An object of transverse length
is observed to subtend an angle in radians of
when both the object and observer are at rest relative to a homogeneous cosmology (D. W. Hogg
1999
) [length]
Transverse comoving distance
Areal radius of a sphere centered on a point in an isotropic cosmology, defined so the sphere has area
(D. W. Hogg
1999
) [length]
Luminosity distance
A source of isotropic radiation having luminosity
iso
is observed to have flux
when both the source and observer are at rest relative to a homogeneous cosmology (D. W. Hogg
1999
) [length]
Redshift
The fractional difference between the frequency of a wave at emission at its source
src
and its observed frequency at a detector
; the reference cosmology for the relationship between distance and the
cosmological
redshift is given in the text [dimensionless]
Primary and secondary dimensionless tidal deformabilities
, Λ
See Equation (
18
); Λ
1,2
= 0 for a BH primary/secondary [dimensionless]
Effective tidal deformability
See Equation (
19
);
for a BBH [dimensionless]
Primary and secondary dimensionless spin-induced quadrupole moments
See Equation (
21
);
1,2
= 1 for a BH primary/secondary [dimensionless]
Primary and secondary radii
Areal radii of primary and secondary objects, defined so their surface areas are
; used in defining NS compactness [length]
Primary and secondary compactness
Dimensionless mass-to-radius ratios
1,2
Gm
/(
1,2
) of primary/secondary;
for Kerr BH primary/secondary [dimensionless]
Merger rate density
Rate of binary mergers per unit volume in the local Universe; may be expressed as a function of cosmological redshift,
; the rate in the local Universe
can be notated
; subscripts can be used if considering different populations, e.g.,
, and
[time
−1
volume
−1
Download table as:
ASCII
Typeset image
5.2.1. Newtonian Inspiral
At early stages of the inspiral, when the magnitude of the difference in velocity vectors of the two components of the binary,
, is much smaller than the speed of light, the orbit is determined approximately by Newtonian mechanics, while the gravitational radiation is described by the quadrupole formula (A. Einstein
1916
, corrected by A. S. Eddington
1922
, page 279). For a quasi-circular orbit that is inclined an angle ι relative to the direction to an observer,
and
are sinusoidal and are 90° out of phase,
and
where
is the distance between the source and the observer,
is the total mass of the system,
is the symmetric mass ratio,
Mη
is the reduced mass of the system, and
is the orbital phase relative to the ascending node (P. C. Peters & J. Mathews
1963
; K. S. Thorne
1987
; L. S. Finn & D. F. Chernoff
1993
; C. M. Will & A. G. Wiseman
1996).
See Figure
. When ι = 0 or ι =
(face-on and face-off, respectively), the amplitudes of the sinusoidal functions
and
are equal and the GW is circularly polarized; when ι =
/2 (edge-on),
= 0 and the GW is linearly polarized.
Figure 5.
Relationship between the orbital elements and the GW coordinate frame. The direction from the source to Earth is
, and the vector
defines a reference direction on the transverse plane (the plane of the sky). The inclination ι is the angle between
and the orbital angular momentum vector
. The longitude of the ascending node of the orbit Ω is the angle on the plane of the sky between
and the ascending node ♌,
. The angle Ω is degenerate with the polarization angle
. The orbit of the primary about the center of mass of the system is shown. The orbital phase
is the angle on the orbital plane between the ascending node and position vector of the primary relative to the center of mass. For an eccentric orbit, the distance of the primary from the center of mass at periapsis is
, and the argument of the periapsis
for the primary is the angle on the orbital plane between the ascending node and the position vector of the primary at periapsis.
Download figure:
Standard image
High-resolution image
The GW luminosity of such a system, i.e., the power in gravitational radiation, is
This radiation gives rise to a secular orbital decay. Since the (Newtonian) energy of the bound system is
orb
= − (1/2)
ηMv
, and equating
, we deduce that the period of the orbit,
= 2
πGM
by Kepler’s third law, evolves according to
At fixed orbital period (or orbital frequency), the orbital velocity is proportional to the cube root of the total mass,
1/3
. It can be seen, then, that
ηM
5/3
orb
ηM
5/3
, and
. At the Newtonian level of approximation, a single combination of the component masses,
known as the
chirp mass
, solely determines both the amplitude of a GW at fixed orbital frequency and its frequency evolution (P. Kafka
1988
; C. Cutler et al.
1993
; L. S. Finn & D. F. Chernoff
1993
). This chirp mass is normally the most accurately measured mass parameter for low-mass systems in which most of the signal observed arises from the pre-merger phase.
5.2.2. Post-Newtonian Inspiral and Other Effects
Additional terms in the GW amplitude and frequency evolution appear at higher orders in
in a post-Newtonian (PN) expansion in the equations of motion and in the gravitational emission (L. Blanchet
2014
). At the Newtonian order, the frequency of the GW is twice the frequency of the orbital motion,
= 2
orb
= 2/
, and
At
) beyond this, additional components to the GW at frequencies at one and three times the orbital frequency arise from current quadrupole and mass octupole radiation, and other components occur at
) beyond Newtonian order from current octupole and mass hexadecapole radiation (K. S. Thorne
1980
); the amplitudes of these
higher-order multipole moments
of radiation are proportional to a different combination of component masses (L. E. Kidder
2008
). The frequency evolution also gains additional terms at
) beyond the leading-order Newtonian term, again having a different dependence on the component masses from the leading Newtonian order (R. V. Wagoner & C. M. Will
1976
). Spin effects from rotating binary components also appear in PN corrections to the quadrupole waveform due to
) spin–orbit and
) spin–spin effects (L. E. Kidder et al.
1993
) and to precession of the orbital plane if the spin angular momentum vectors of the bodies are not aligned (or antialigned) with the orbital angular momentum vector (T. A. Apostolatos et al.
1994
). The dimensionless parameter
eff
, defined as
where
and
are the spins of the two binary components and
is the orbital angular momentum about the center of mass, is an effective inspiral spin parameter that is conserved under the orbit-averaged precession equations of motion at
) (T. Damour
2001
; E. Racine
2008
; M. Kesden et al.
2010
; L. Santamaria et al.
2010
; P. Ajith et al.
2011
). Whereas
eff
depends on the spin components aligned with the orbital angular momentum, a dimensionless effective precession spin parameter that depends on in-orbital-plane components of the spins,
captures the dominant precession effects (P. Schmidt et al.
2015
).
Deformable binary components (NSs but not BHs) suffer an induced quadrupole deformation
ij
under an external tidal field
, where these quadrupole tensors are those appearing in a multipole expansion of the Newtonian potential centered on the body of mass
as (K. S. Thorne
1998
The
dimensionless tidal deformability
, Λ, of a body of mass
is defined in terms of the ratio of the induced deformation to the external tidal field as
where BHs have Λ = 0. Newtonian tidal interactions of deformable components appear as effective
10
10
) corrections to the binding energy and GW luminosity (E. E. Flanagan & T. Hinderer
2008
). At this order, the dimensionless combination of tidal parameters given by (M. Favata
2014
appears, where Λ
and Λ
are the dimensionless tidal deformabilities of the two bodies, and it is this parameter that is most measurable in the waveforms produced by binaries with deformable companions (E. Poisson
2021
). Spinning bodies experience quadrupole deformation of the form
where
is the spin-induced mass quadrupole moment scalar. The quadrupole deformations induced by an object’s spin result in Newtonian quadrupole–monopole effects as an effective
) correction, the same order as the spin–spin coupling relativistic effects (E. Poisson
1998
). The size of the spin-induced deformation depends on the nature of the body, where the ratio of the quadrupole scalar to the square of the body’s spin magnitude is given by the dimensionless parameter
as
where
is the mass of the body. For a BH,
= 1 (K. S. Thorne
1980
).
Binaries detected by ground-based observatories are commonly assumed to have negligibly small orbital eccentricity remaining by the time the orbital period has decayed to the point that the GW frequencies have entered the high-frequency sensitivity band of the detectors. This decay in eccentricity happens because orbital eccentricity is efficiently reduced by GW emission during the orbital decay (P. C. Peters
1964
). However, there are channels of compact binary formation that could result in nonnegligible orbital eccentricity being present even at the last stages of inspiral observed by ground-based detectors (e.g., M. Mapelli
2020
). The leading-order effects of orbital eccentricity would appear at the Newtonian level (P. C. Peters & J. Mathews
1963
). Two additional parameters are needed to describe an eccentric binary system, the eccentricity
and the argument of the periapsis
. Although these are well-defined for Newtonian two-body systems, there are different ways to generalize their definitions for relativistic systems, and there is not yet a settled convention for these parameters (M. A. Shaikh et al.
2023
).
Tests of GR from CBC Inspiral
. PN theory in GR predicts the relative amplitudes of subdominant modes of GW radiation (L. Blanchet
2014
), which depend on the binary’s masses and spins (e.g., K. G. Arun et al.
2009
). Thus, allowing for freedom in these amplitudes and checking whether they are consistent with those predicted by GR provides a consistency test of the agreement of the signal with the waveform model used to analyze it (A. Puecher et al.
2022
). In the companion article A. G. Abac et al. (
2025d
), this test is carried out for BBH signals, considering deviations,
δA
ℓm
, in the amplitude of the (
= 2,
= ± 1) or (
= 3,
= ± 3) subdominant multipole moments relative to the dominant (
= 2,
= ± 2) and other multipole moments.
The PN expansion of the orbital energy and GW energy loss makes a prediction of how the GW phase evolves with time as the orbit decays (L. Blanchet
2014
). The PN formalism expresses this phase evolution with a set of coefficients in a series expansion of the GW phase in terms of powers (
−5
and
for integer
(with
= 0 for the leading-order Newtonian inspiral) that depend on the binary components’ masses and spins for point particles. Violations of GR can lead to differences in the values of the PN coefficients from those predicted by GR (e.g., N. Yunes & F. Pretorius
2009
; S. Tahura & K. Yagi
2018
), which could be observed in a GW signal (L. Blanchet & B. S. Sathyaprakash
1994
1995
; K. G. Arun et al.
2006
; C. K. Mishra et al.
2010
; T. G. F. Li et al.
2012
). In the companion article A. G. Abac et al. (
2025e
), we present parameterized tests for such violations.
Effects arising from the finite size of the component masses of a binary include spin-induced multipole moments, most importantly their spin-induced quadrupole moments
, which also affect the orbital evolution. For a BH, there is a fixed relation between its spin-induced quadrupole moment and its mass and spin (E. Poisson
1998
). Deviations from this predicted value, as observed in the phase evolution of a GW signal, can be used to distinguish a BBH from a compact binary containing exotic, non-BH components. Some examples of exotic alternatives to BHs, being compact objects capable of having masses greater than the maximum mass of an NS, include boson stars (D. J. Kaup
1968
; R. Ruffini & S. Bonazzola
1969
), gravastars (P. O. Mazur & E. Mottola
2004
), fuzzballs (S. D. Mathur
2005
), and firewalls (A. Almheiri et al.
2013
). The companion article A. G. Abac et al. (
2025e
) presents such parameterized tests of the nature of the components of CBCs.
5.2.3. Compact Binary Merger and Ringdown
The final stages of GW emission from CBCs that result in a BH remnant can be modeled as a linear gravitational perturbation to a Kerr BH spacetime (W. H. Press & S. A. Teukolsky
1973
). Remarkably, the partial differential equations for the outgoing GW content of such a perturbation decouple from the other gravitational modes, and those decoupled equations are
separable
into a radial equation, an angular equation, and an exponential function of time with a complex frequency (S. A. Teukolsky
1972
1973
). The separation results in a spectrum of complex eigenfrequencies of the GW perturbations to the BH spacetime indexed by integer degree
and order
numbers,
≥ 2 and ∣
∣ ≤
, and integer overtone
with
≥ 1 (E. W. Leaver
1985
; E. Berti et al.
2006
). The angular eigenfunctions, which depend on
and
, also depend on the dimensionless complex frequency and the dimensionless spin parameter of the remnant BH. The complex eigenfrequencies describe the spectrum of exponentially decaying sinusoidal GW
quasi-normal modes
that make up what is called the
BH ringdown
. GR therefore provides a prediction for the relationship between the frequency and the decay constant for the spectrum of such quasi-normal modes that depend solely on the mass and spin of the final BH, and thus the BH ringdown radiation can be used to test these predictions of GR.
Spanning the region between the portion of the waveform that can be computed by PN calculations at early time and the portion that can be computed by a superposition of quasi-normal modes at late time is what is known as the
merger phase
of the compact binary. Due to the nonperturbative nature of this phase, numerical relativity (NR) solutions to Einstein’s field equations are sought (L. Lehner & F. Pretorius
2014
; M. D. Duez & Y. Zlochower
2019
). Such solutions both interpolate these early and late phases and also provide the information about the quasi-normal mode amplitudes and phases excited, as well as the mass and spin of the remnant BH (F. Hofmann et al.
2016
; J. Healy & C. O. Lousto
2017
; X. Jiménez-Forteza et al.
2017
).
When at least one component of the binary in the CBC is not a BH (i.e., an NS), the merger and ringdown phases might be considerably more complex owing to the presence of matter in the system. NR is typically required to compute the entire post-inspiral phase of the GWs emitted from such systems (J. A. Faber & F. A. Rasio
2012
; K. Kyutoku et al.
2021
). One important piece of such simulations is to determine whether disruption of an NS component occurs, particularly in the case of NSBH systems in which the NS might be swallowed whole by the BH (typical for high-mass and low-spin BHs) or might be tidally disrupted by the BH (typical for low-mass or high-spin BHs). Such NS disruption would be expected to produce electromagnetic emission that could be observed by electromagnetic astronomical observatories. Guided by numerical simulations, one can estimate whether a system having particular parameters inferred from the inspiral phase will be electromagnetically bright and so a candidate for electromagnetic follow-up observations (F. Foucart et al.
2018
; D. Chatterjee et al.
2020
; M. Berbel et al.
2024
).
Depending on the masses of the initial components, the product of the merger of two NSs might be another NS, a supramassive NS (a uniformly spinning NS that is more massive than the highest allowed mass for a nonspinning NS, which remains an NS until its angular momentum is dissipated, resulting in its collapse to a BH), a hypermassive NS (an NS more massive than would be allowed for any stationary, spinning configuration, but which is temporarily supported by differential rotation, and which will ultimately collapse to a BH), or there might be a direct collapse on a dynamical timescale to form a BH after the merger (T. W. Baumgarte et al.
2000
; A. L. Piro et al.
2017
). Both the electromagnetic emission and GW emission from these different scenarios are expected to vary considerably (B. P. Abbott et al.
2017c
).
Tests of GR from CBC Merger.
NR simulations of BBHs in GR provide predictions for the GW waveform spanning the inspiral, merger, and final ringdown phases of evolution. Tests for violations of GR can be performed by subtracting the best-fit GR waveform from the observed data and testing whether the remaining residual is consistent with detector noise or whether there is remaining signal present. Alternatively, since NR predicts how a final BH mass and spin are related to the initial BH masses and spins for a BBH CBC (F. Hofmann et al.
2016
; J. Healy & C. O. Lousto
2017
; X. Jiménez-Forteza et al.
2017
), a test of consistency between the initial orbital parameters and the final BH mass and spin can be performed. Here the initial component BH masses and spins can be determined from the early inspiral phase of the GW signal, while the mass and spin of the final BH are found from the late-time ringdown radiation. In practice, such a consistency test divides the GW signal into low- and high-frequency portions (below and above a given cutoff frequency) that are independently modeled with full inspiral–merger–ringdown waveforms (A. Ghosh et al.
2016
2018
). Companion article A. G. Abac et al. (
2025d
) presents results from such residual and inspiral–merger–ringdown consistency tests.
In GR, a BH remnant produced by a CBC will rapidly settle to a stationary Kerr BH (R. P. Kerr
1963
), uniquely characterized by its mass and spin (W. Israel
1967
; B. Carter
1971
), through emission of ringdown radiation in a spectrum of quasi-normal modes, as described earlier. These quasi-normal modes have a discrete spectrum of complex-valued eigenfrequencies (the imaginary part of which determines the decay timescale), so a possible non-BH remnant (e.g., C. F. B. Macedo et al.
2013
), or modifications of the spectrum in alternative theories of GR (e.g., P. A. Cano et al.
2024
), can be tested by looking for deviations in the observed ringdown radiation from the anticipated spectrum of quasi-normal modes (E. Berti et al.
2025
).
Furthermore, if the remnant object does not possess an event horizon, ingoing GW radiation can be reflected off of a surface or scattered off of an inner potential and reemerge as an echo signal observed within ∼seconds after the merger (V. Cardoso et al.
2016
; V. Cardoso & P. Pani
2019
; N. Siemonsen
2024
). The companion article A. G. Abac et al. (
2025f
) presents tests of the nature of the remnant resulting from CBC through observed quasi-normal mode spectra and searches for GW echoes.
The post-inspiral portion of a BBH signal can be phenomenologically modeled with various parameters that are fitted to NR simulations (G. Pratten et al.
2020
). The companion article A. G. Abac et al. (
2025e
) explores possible deviations of these parameters from their nominal values (J. Meidam et al.
2018
; S. Roy et al.
2025
).
5.2.4. Redshift and Cosmological Effects
GWs can be redshifted, just as electromagnetic waves are. These changes are caused by the Doppler effect due to relative motion of the emitter and the observer (often described in terms of
peculiar velocities
relative to the rest frame of the cosmological microwave background radiation), due to the expansion of space between the emitter and the observer, or due to gravitational redshift if the emitter and observer have different gravitational potentials. For sources beyond the nearby Universe (having redshifts ≳0.1), cosmological expansion is the dominant source of redshift (E. R. Peterson et al.
2022
).
The redshift is the fractional difference between the frequency of a wave at emission at its source
src
, and its observed frequency at a detector
det
= (
src
det
)/
det
(D. W. Hogg
1999
). Thus, the observed frequency of a wave is related to its emitted frequency by
det
src
/(1 +
). Similarly, an interval in time in the source-frame
dt
src
is related to an observed interval in time by a detector
dt
det
by
dt
det
= (1 +
dt
src
. Equations (
10
) and (
12
) are both parameterized in terms of the orbital velocity
, which is related to the GW frequency
in the dominant mode by Equation (
14
). At a fixed moment in a GW waveform, where the binary has some instantaneous value of
, we have
That is, a redshifted signal, observed at frequency
det
, produced by a system with intrinsic mass
has identical morphology to an unredshifted signal produced by a system with intrinsic mass (1 +
(A. Krolak & B. F. Schutz
1987
). If the redshift is unknown, then the observable mass parameters are the various combinations of (1 +
and (1 +
, e.g.,
and (1 +
. These mass parameters with the 1 +
scale factor are referred to as
detector-frame masses
det
= (1 +
, and
. PN corrections to the waveform preserve this degeneracy for point particles (and BHs). However, for NSs, a functional relationship between the mass of an NS and its tidal deformability means that a measurement of
can break the degeneracy between mass and redshift, allowing the two to be independently measured (C. Messenger & J. Read
2012
).
The amplitudes of
and
given in Equation (
10
) also depend on the total mass through the factor
. If the factor (1 +
is determinable from the rate of decay of the orbital period, Equation (
12
), then the amplitude factor can be written as [(1 +
]/[(1 +
], suggesting that the measurable amplitude distance parameter is (1 +
The parameter
that appears in inverse proportion to the GW amplitude in Equation (
10
) represents the areal radius, i.e., spheres centered on the GW source have area 4
πr
. Within a cosmological setting, this parameter is the
transverse comoving distance D
(D. W. Hogg
1999
). Then, if the redshift is entirely due to the cosmological expansion of spacetime, the combination (1 +
is equal to the
luminosity distance
of the source, and this becomes the observable distance parameter from the GW amplitude. In this sense, then, given a known cosmology (i.e., the values of the Hubble constant, matter density, and the spatial curvature), the functional relationship between luminosity distance and redshift allows the determination of the latter from the former, and the intrinsic masses, e.g.,
, can then be deduced from the observed mass–redshift combined parameters, e.g.,
det
= (1 +
. However, if other redshift effects are present, e.g., due to peculiar motion of the source or the observer relative to the Hubble flow, the combination (1 +
is no longer equal to the luminosity distance.
Nevertheless, when reporting the parameters of a CBC, we normally assume that cosmological expansion is the only significant source of redshift, and so the observed amplitude parameter (1 +
is referred to as luminosity distance
, while a dimensionful intrinsic mass parameter such as the primary mass
is derived from observed detector-frame mass parameters as
, where the relationship between the redshift and the luminosity distance,
), is obtained by some standard cosmological model. The only case where this was not done was for GW170817, where the measured geocentric redshift to its host galaxy NGC 4993 was used (B. P. Abbott et al.
2019b
). The main uncertainty in the chirp mass of the system comes from the unknown peculiar velocity of the system relative to its host galaxy. Unless otherwise specified, the reference cosmology used to relate luminosity distance to redshift throughout the works is a ΛCDM model (P. J. E. Peebles & B. Ratra
2003
) corresponding to a spatially flat Friedman–Lemaître–Robertson–Walker spacetime (G. Lemaitre
1931
; H. P. Robertson
1935a
1935b
1936
; A. G. Walker
1937
; S. Weinberg
1972
; C. W. Misner et al.
1973
; A. Friedmann
1999b
1999a
) with Hubble constant
= 67.9 km s
−1
Mpc
−1
, matter density parameter Ω
= 0.3065, and cosmological constant density parameter Ω
= 1 − Ω
= 0.6935 (P. A. R. Ade et al.
2016
, column TT+lowP+lensing+ext of Table 4).
Constraints on Cosmic Expansion from GW Observations.
If the redshift of a GW source can be determined independently of its distance, then a distance–redshift relationship can be obtained and used to infer cosmological parameters (B. F. Schutz
1986
; A. Krolak & B. F. Schutz
1987
). Here the CBC is called a
standard siren
(akin to the
standard candles
such as Cepheid variables and Type Ia supernovae used to measure distances to their galaxy hosts), where the luminosity distance of the CBC is inferred from the amplitude of the GWs (D. E. Holz & S. A. Hughes
2005
). The most direct method of determining the redshift of a GW source is if there is an electromagnetic counterpart in which spectroscopic measurements of the redshift of its host galaxy can be made (A. Krolak & B. F. Schutz
1987
; D. E. Holz & S. A. Hughes
2005
; N. Dalal et al.
2006
; H.-Y. Chen et al.
2018
). This method is known as the
bright siren
method. For example, the BNS coalescence GW170817 (B. P. Abbott et al.
2017a
) was associated with the optical kilonova AT 2017gfo in the galaxy NGC 4993 (B. P. Abbott et al.
2017b
), which allowed for a measurement of the maximum a posteriori value of the Hubble constant with 68.3% credible level (CL) highest-density interval
(B. P. Abbott et al.
2021a
).
If no electromagnetic counterpart to a GW is observed, various methods are available to deduce the associated redshift (BBHs are not normally expected to produce any electromagnetic radiation, unless there is matter present in their environment). One such method, the
galaxy catalog
method, also called the
dark siren
method, is to obtain statistical association of GW sources with potential host galaxies observed in surveys (B. F. Schutz
1986
; C. L. MacLeod & C. J. Hogan
2008
). This is usually done simultaneously with information obtained from another method, the
spectral siren
method. In the spectral siren method, a known feature in the mass distribution of the population of CBCs is used to statistically infer the redshift of a number of sources at a given distance by how the observed detector-frame mass distribution is shifted with respect to the local (zero-redshift) distribution (D. F. Chernoff & L. S. Finn
1993
; S. R. Taylor et al.
2012
; W. M. Farr et al.
2019
; S. Mastrogiovanni et al.
2021
). Finally, future observations of BNS mergers may be capable of directly inferring the redshift of the source from the GW signal alone through measurements of the NS tidal deformations (C. Messenger & J. Read
2012
; D. Chatterjee et al.
2021
).
The companion article A. G. Abac et al. (
2025g
) reports on constraints on the cosmic expansion history based on combined CBC bright and dark sirens, including both the galaxy catalog method and the spectral siren approach. If GWs propagate through cosmological backgrounds differently from electromagnetic waves in a manner that produces a different distance–amplitude relation, the modified propagation effects can be observed using standard siren methods (E. Belgacem et al.
2018
). The companion article A. G. Abac et al. (
2025g
) also reports on constraints on such effects of modified GW propagation.
5.2.5. Populations of Compact Binaries
With a multitude of observed CBCs, one can infer the underlying population of these sources. In doing so, one needs to account for the detector selection effects, e.g., the fact that events that are farther away are less likely to be detected as compared to events that are nearby. One key element of the population that can be measured is the local merger rate density,
, representing the number of CBCs occurring per unit time per unit volume in the local Universe (E. S. Phinney
1991
; C. Kim et al.
2003
; P. R. Brady et al.
2004
; R. Biswas et al.
2009
; W. M. Farr et al.
2015
; B. P. Abbott et al.
2016e
), or its evolution with cosmic redshift
, which is the number of coalescences per unit source-frame time per unit comoving volume at a cosmological redshift of
(M. Fishbach et al.
2018
). Another is the population distribution of masses and spins of merging compact binaries,
), which might also evolve over cosmic history,
). The measurement uncertainty in single-event parameters and the total number of detected events dictate the measurability of features in the population. These inferences are important in understanding the underlying astrophysical formation channels of compact binaries (e.g., S. Stevenson et al.
2017
; W. M. Farr et al.
2017
; M. Zevin et al.
2021
; I. Mandel & F. S. Broekgaarden
2022
).
Inference of the Population of CBCs.
In the companion article A. G. Abac et al. (
2025c
), we present measurements of the local rate of BNS, NSBH, and BBH mergers; inference of the evolution of the CBC rate over cosmological time; and inference of the distribution of masses and spins of CBCs.
6. Synopsis
This Letter serves as an introduction to the collection of articles accompanying the LVK’s GWTC-4.0. We have provided an overview of the GW detectors and observing runs of the LVK network and of the observed GWs from CBCs. The primary sequels to this introduction are a description of the methods used to perform searches for GWs in LVK data and to characterize source properties of identified signals (A. G. Abac et al.
2025a
) and a summary of the main observations of GWTC-4.0, highlighting new CBC candidates and their estimated estimated masses and spins (A. G. Abac et al.
2025b
). Other companion articles presenting science results from the analysis of the GWTC-4.0 candidates were described in Section
. GWTC provides a prodigious census of over 200 merging BHs and NSs spanning two orders of magnitude in mass from ∼1
NSs to remnant BHs exceeding 100
. Study of these observations will provide new insight into the nature of these objects, their population distribution, and their formation channels. These GW observations allow for sensitive tests of GR and provide information about the cosmological expansion history.
Acknowledgments
This material is based on 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 ICSC—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 US–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 acknowledgments for support of individual authors may be found in the following document:
. For the purpose of open access, the authors have applied a Creative Commons Attribution (CC BY) license to any Author Accepted Manuscript version arising. We request that citations to this article use “A. G. Abac et al. (LIGO–Virgo–KAGRA Collaboration), ...” or similar phrasing, depending on journal convention.
Facilities:
EGO:Virgo - Virgo Interferometer at the European Gravitational Observatory, GEO600 - The German-British 600m Armlength Gravitational Wave Detector, Kamioka:KAGRA - , LIGO - Laser Interferometer Gravitational-Wave Observatory.
Software
: Plots were prepared with
Matplotlib
(J. D. Hunter
2007
) and
seaborn
(M. Waskom
2021
).
Astropy
(A. M. Price-Whelan et al.
2022
),
GWpy
(D. M. Macleod et al.
2021
),
LALSuite
(LIGO–Virgo–KAGRA Collaboration
2018
; K. Wette
2020
),
NumPy
(C. R. Harris et al.
2020
), and
SciPy
(P. Virtanen et al.
2020
) were used for data processing in generating the figures and quantities in the manuscript.
Data availability
Event data used within this work are openly available in the GWTC-4.0 online catalog, which is hosted at
and documented further in A. G. Abac et al. (
2025i
). Data behind Figures
, and
can be found in LIGO–Virgo–KAGRA Collaboration (
2025
).
Appendix A: Acronyms and Glossary
This is a reference of frequently used terms and acronyms.
A+:
Advanced+ LIGO refers to a configuration of LIGO following a series of upgrades, some in advance of O4 (such as the addition of a new 300 m filter cavity for frequency-dependent vacuum squeezing), and some planned in advance of O5, such as installation of new optics with lower noise and loss (B. P. Abbott et al.
2020a
; S. J. Cooper et al.
2023
).
A♯:
LIGO A
(A-sharp) is a proposed upgrade of the Advanced+ LIGO interferometers anticipated on a post-O5 timeline. The baseline A
design is a room-temperature 1
m laser wavelength interferometer upgrade with larger test masses having coatings with lower thermal noise, higher laser power, and increased levels of vacuum squeezing (P. Fritschel et al.
2024
).
AdV:
Advanced Virgo refers to an upgraded Virgo detector (F. Acernese et al.
2015
) with an advanced interferometer. Virgo operated with the AdV configuration during O2 and O3.
AdV+:
Advanced Virgo+ is an upgrade to the AdV detector to take place in two phases: the first phase for operation during O4, and the second phase for operation during O5.
aLIGO:
Advanced LIGO refers to an upgraded LIGO configuration with advanced interferometers installed at both LHO and LLO. LIGO operated with the aLIGO configuration during O1, O2, O3, and O4 (J. Aasi et al.
2015a
).
BBH:
Binary black hole. A binary system where both components are BHs.
BH:
Black hole.
BHNS:
Black hole–neutron star specifically refers to systems in which the BH formed before the NS. See also NSBH.
bKAGRA:
Baseline-design KAGRA is a configuration of the KAGRA detector as a cryogenic dual-recycled Fabry–Perot Michelson interferometer. bKAGRA phase-1 operation without power- or signal recycling took place from 2018 April 28 to 2018 May 6 2018 (T. Akutsu et al.
2019
).
BNS:
Binary neutron star. A binary system where both components are NSs.
CBC:
Compact binary coalescence. The gravitational-radiation-driven orbital decay resulting in merger of a binary system made of two compact objects (NSs or BHs).
CI:
Credible interval. See CL.
CL:
Credible level. Given an
= 1 univariate or
-dimensional multivariate random variable
having probability density function (pdf)
) and an
-dimensional region
, then the CL
of the region
is the probability of
lying in
. The region
is then known as a 100
% CL
credible region
, with special cases:
credible interval
(CI) if
= 1,
credible area
if
= 2, or
credible volume
if
= 3. When
> 1, we normally take
to be the region having the smallest volume that has CL
(the
highest-density region
). When
= 1 (CI),
is normally chosen to be an
equal-tailed interval
(also known as a symmetric interval), from the
/2 quantile to the 1 −
/2 quantile, but sometimes the smallest
highest-density interval
is used instead.
EOS:
Equation of state of an NS. For cold NSs (having temperature below the Fermi temperature), the EOS is of a barotropic fluid, a relationship between the energy density of the fluid and its pressure.
FAR:
False-alarm rate. Often used as a detection threshold, the probability of any one or more of a sequence of statistical tests performed over a duration
erroneously rejecting a null hypothesis is
. FAR therefore has dimensions of time
−1
. When interpreted as a measure of a detection significance of a candidate detection, this is the rate at which noise alone would produce more significant candidates.
GEO:
The GEO600 GW detector is a British–German ⌞-shaped interferometric GW detector with 600 m arms located near Hannover, Germany (B. Willke et al.
2002
).
GR:
General relativity. Einstein’s theory of gravitation.
GW:
Gravitational wave. See Sections
and
5.1
GWOSC:
The Gravitational Wave Open Science Center (formerly known as the LIGO open science center) was created to provide public access to GW data products (R. Abbott et al.
2021d
). The GWOSC online data and resources can be found at
GWTC:
The Gravitational-Wave Transient Catalog is the electronic catalog of GW transients observed by LIGO, Virgo, and KAGRA detectors produced by the LVK.
IFAR:
Inverse false-alarm rate. The reciprocal of FAR, IFAR = (FAR)
−1
, having dimensions of time. A larger IFAR implies a more significant candidate, while a larger FAR implies a less significant candidate.
IFO:
Interferometer, a type of detector that uses laser interferometry to measure changes in the lengths of optical paths induced by GWs.
IGWN:
The International GW Observatory Network is a self-governing consortium using ground-based GW interferometers to explore the fundamental physics of gravity and to observe the Universe. The observatory network includes the KAGRA, LHO, LLO, and Virgo detectors. In addition, the GEO detector serves as a technology test bed and operates in an
astrowatch
mode outside of other detectors’ observing periods.
iKAGRA:
Initial-phase KAGRA is a configuration of the KAGRA detector as a simple Michelson interferometer that consists of two end test masses and a beam splitter. iKAGRA was operated from 2016 March 25 to 2016 March 31 and from 2016 April 11 to 2016 April 25 (T. Akutsu et al.
2018
).
IMBH:
Intermediate-mass black hole. A BH in the mass range ∼10
to ∼10
KAGRA:
KAGRA is a Japanese ⌞-shaped interferometric GW detector with 3 km arms located underground at the Kamioka Observatory in Japan (T. Akutsu et al.
2021
).
KAGRA Collaboration:
The KAGRA Collaboration manages the building, operation, and development of the KAGRA detector.
LHO:
The LIGO Hanford Observatory, one of the two LIGO observatories, located in Hanford, Washington, is an ⌞-shaped interferometric GW detector with 4 km arms.
LIGO:
The Laser Interferometer Gravitational-Wave Observatory consists of two widely spaced installations within the United States: one in Hanford, Washington (LHO), and the other in Livingston, Louisiana (LLO). LIGO is operated by the LIGO Laboratory, a consortium of the California Institute of Technology and the Massachusetts Institute of Technology funded by the US National Science Foundation.
LLO:
The LIGO Livingston Observatory, one of the two LIGO observatories, located in Livingston, Louisiana, is an ⌞-shaped interferometric GW detector with 4 km arms.
LSC:
The LIGO Scientific Collaboration, founded in 1997, is a group of more than 1000 scientists that carries out science related to the LIGO detectors and their observations.
LV:
The LIGO–Virgo Collaboration. Prior to O3b, all observational results were published by the LV.
LVC:
The LIGO–Virgo Collaboration. The acronym LV is now preferred.
LVK:
The LIGO–Virgo–KAGRA Collaboration.
NS:
Neutron star.
NSBH:
The general term for a neutron star–black hole binary: a binary system in which one component is an NS and the other is a BH. If used in distinction with BHNS, it refers to such systems in which the NS formed before the BH.
NR:
Numerical relativity, the use of numerical methods to solve relativistic field equations.
O1:
The first observing run began on 2015 September 12 and ended on 2016 January 19. The LHO and LLO detectors participated in this observing run.
O2:
The second observing run began on 2016 November 30 and ended on 2016 August 25, during which the LHO and the LLO detectors were operating. On 2017 August 1, the AdV detector joined the observing run, forming a three-detector network.
O3:
The third observing run began on 2019 April 1 and ended on 2020 March 27, during which the LHO, LLO, and Virgo detectors were operating. A commissioning break from 2019 October 1 to 2019 November 1 divided O3 into two parts, O3a and O3b. A subsequent short run, O3GK, from 2020 April 7 to 2020 April 21 with GEO and KAGRA observing, followed O3b.
O3a:
The first, pre–commissioning break part of O3, from 2019 April 1 to October 1, during which the LHO, LLO, and Virgo detectors were operating.
O3b:
The second, post–commissioning break part of O3, from 2019 November 1 to 2020 March 27, during which the LHO, LLO, and Virgo detectors were operating. O3b was planned to continue until 2020 April 30 but ended early owing to the COVID-19 pandemic.
O3GK:
A short observing run after O3b from 2020 April 7 to 2020 April 21, during which the KAGRA and GEO detectors were observing. KAGRA had intended to join LIGO and Virgo at the end of O3, but the early end of O3b made this impossible.
O4:
The fourth observing run began on 2023 May 24 and is planned to continue into late 2025. It is divided into parts, the first of which, O4a, covered the period from 2023 May 24 until a commissioning break from 2024 January 16 to 2024 April 10. During O4a, LHO and LLO were observing. Following the break, observing continued in O4b from 2024 April 10 until an original intended end date of 2025 January 23, with LHO, LLO, and Virgo observing. It was decided to continue O4 observing in a third period O4c, beginning 2025 January 23 and lasting until 2025 November 18.
O4a:
The first part of the fourth observing run including data from 2023 May 24 until a commissioning break that began on 2024 January 16. During O4a, LHO and LLO were observing.
O4b:
The second part of the fourth observing run starting at the end of a commissioning break on 2024 April 10 and ending on the originally planned O4 end date of 2025 January 23. During O4b, LHO, LLO, and Virgo were observing. It was decided to continue O4 observations with a third part, O4c, immediately following the end of O4b on 2025 January 23.
O4c:
The third part of the fourth observing run, extending the run beyond its intended end date of 2025 January 23 through 2025 November 18. A commissioning break in O4c took place between 2025 April 1 and 2025 June 11.
O5:
The fifth observing run is the planned future observing run to follow O4.
pdf:
Probability density function. Given an
= 1 univariate or
-dimensional multivariate random variable
, the probability of
lying in an
-dimensional region
is
, where
) is the pdf.
PE:
Parameter estimation, the process of measuring the parameters that describe the source of a signal, e.g., the masses and spins of the binary components of a CBC, from the observational data.
PN:
Post-Newtonian, a perturbative method of obtaining solutions to relativistic field equations based on slow-motion and weak-field expansion of the spacetime metric and the stress–energy source.
PSD:
Power spectral density. See Appendix
SNR:
Signal-to-noise ratio. See Appendix
Virgo:
The Virgo detector is a European ⌞-shaped interferometric GW detector with 3 km arms located near Cascina, Italy (near Pisa).
VirgoNEXT:
Virgo_nEXT is a planned, post-O5, major upgrade of Virgo to fill the gap between the current phase, AdV+, and next-generation detectors.
Virgo Collaboration:
The Virgo Collaboration manages the building, operation, and development of the Virgo detector.
Appendix B: Conventions for Data Analysis
This appendix serves to define the data analysis conventions that will be used throughout the GWTC-4.0 companion articles. For a general introduction to data analysis we refer the reader to B. P. Abbott et al. (
2020c
) and references therein.
Time series
) and frequency series
are related to each other by our conventions for the
Fourier transform
and its inverse transform
With these conventions, the dimensions of
are
Detector noise is often taken to be a stochastic Gaussian process. If
) is a real-valued stochastic Gaussian process, then the
one-sided PSD
) is formally defined by
where 〈 · 〉 is a statistical ensemble average of realizations of
) and
is the complex conjugate of
. The one-sided PSD is defined only for
≥ 0. With these conventions, the dimensions of
are [
] = [
× time. Real detector noise is neither entirely stationary nor Gaussian (B. P. Abbott et al.
2020c
). However, it is often sufficient to assume that
) is ergodic such that
The factor of two in the one-sided PSD ensures that the integrated power is
The
amplitude spectral density
is defined to be the square root of the PSD,
We often use a detector-noise-weighted inner product between two real-valued time series,
) and
), which is defined as
where
) is the detector’s one-sided PSD for the readout noise from that detector. The second form, Equation (
28b
), is an appropriate generalization of the inner product for complex-valued time series.
Since GW detectors are insensitive at very low frequencies, the mean of the detector readout is arbitrary, and so we take the detector noise to have zero mean, 〈
)〉 = 0. Gaussian noise is then entirely characterized by its PSD, and its distribution is given by the probability density
where
is a usually neglected normalizing constant, the path integral
Consider a template waveform
) that is unit normalized, 〈
〉 = 1, which is expected to match a hypothetical signal in detector data
). The
matched filter
SNR
is
If data
) =
) +
) contain Gaussian noise
) plus a signal
) that is perfectly matched by the template waveform,
) ∝
), then
mf
is a random variable having a normal distribution with unit variance and mean equal to the
optimal
SNR
The
likelihood
that detector data
) contains a signal
) is given by Equation (
29
) with
) =
) −
),
where
mf
is the matched filter SNR with unit-normalized template
) ∝
) and
is the likelihood under the no-signal hypothesis,
) =
). The likelihood is viewed as a functional of
) for a given realization of detector data
). The second factor in Equation (
32c
) is the signal-to-noise
likelihood ratio
. Note that the likelihood ratio is a monotonically increasing function of the matched filter SNR, and so
mf
is the uniformly most powerful test for a known signal in Gaussian detector noise (J. Neyman & E. S. Pearson
1933
). If the amplitude of the signal is unknown,
) =
opt
) with unknown
opt
, then the likelihood is maximized for
opt
mf
and
For the Newtonian inspiral of Section
5.2.1
, the signal observed in a detector can be obtained in the frequency domain under the stationary phase approximation as (B. S. Sathyaprakash & S. V. Dhurandhar
1991
; C. Cutler et al.
1993
where Ψ(
) is the stationary phase function and
is the
effective distance
(B. Allen et al.
2012
), which is related to the distance to the binary
by a factor that accounts for the orientation angles that describe the position of the source on the sky (
), its inclination ι, and polarization angle
. Since
(with equality for a source on the zenith or nadir of an ⌞-shaped interferometric detector),
eff
(with equality only if ι = 0 or ι =
). The optimal SNR for such a signal is
The
horizon distance D
hor
(B. Allen et al.
2012
) of a source is the effective distance of a signal from such a source that has SNR
opt
equal to some detection threshold
th
. Such sources would not be expected to be detected beyond the horizon distance, but not all nearer sources will be detected either. The
sensitive volume
(L. S. Finn & D. F. Chernoff
1993
; H.-Y. Chen et al.
2021
) is a measure of the effective volume of space in which randomly isotropically oriented and homogeneously distributed identical sources will produce signals in the detector with SNR
opt
greater than the threshold
th
If the merger rate density is
, then the expected number of detections in time
is
. For a standard measure of detector sensitivity, a binary source of two 1.4
objects (
) is considered and a threshold SNR of
th
= 8 is adopted (H.-Y. Chen et al.
2021
). The sensitive volume is converted into an equivalent spherical radius as
= (4
/3)
to obtain the BNS range
hor
/2.26478, Equation (
).
Footnotes
327
GWOSC event portal
328
LVK observing run plans
Please wait… references are loading.
10.3847/2041-8213/ae0c06