GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo during the Second Part of the Third Observing Run

被引：691

作者：

Abbott, R. ^{[1
]}

Abbott, T. D. ^{[2
]}

Acernese, F. ^{[3
,4
]}

Ackley, K. ^{[5
]}

Adams, C. ^{[6
]}

Adhikari, N. ^{[7
]}

Adhikari, R. X. ^{[1
]}

Adya, V. B. ^{[8
]}

Affeldt, C. ^{[9
,10
]}

Agarwal, D. ^{[11
]}

Agathos, M. ^{[12
,13
]}

Agatsuma, K. ^{[14
]}

Aggarwal, N. ^{[15
]}

Aguiar, O. D. ^{[16
]}

Aiello, L. ^{[17
]}

Ain, A. ^{[18
]}

Ajith, P. ^{[19
]}

Akcay, S. ^{[13
,20
]}

Akutsu, T. ^{[21
,22
]}

Albanesi, S. ^{[23
]}

Allocca, A. ^{[4
,24
]}

Altin, P. A. ^{[8
]}

Amato, A. ^{[25
]}

Anand, C. ^{[5
]}

Anand, S. ^{[1
]}

Ananyeva, A. ^{[1
]}

Anderson, S. B. ^{[1
]}

Anderson, W. G. ^{[7
]}

Ando, M. ^{[26
,27
]}

Andrade, T. ^{[28
]}

Andres, N. ^{[29
]}

Andric, T. ^{[30
]}

Angelova, S., V ^{[31
]}

Ansoldi, S. ^{[32
,33
]}

Antelis, J. M. ^{[34
]}

Antier, S. ^{[35
]}

Appert, S. ^{[1
]}

Arai, Koji ^{[1
]}

Arai, Koya ^{[36
]}

Arai, Y. ^{[36
]}

Araki, S. ^{[37
]}

Araya, A. ^{[38
]}

Araya, M. C. ^{[1
]}

Areeda, J. S. ^{[39
]}

Arene, M. ^{[35
]}

Aritomi, N. ^{[26
]}

Arnaud, N. ^{[40
,41
]}

Arogeti, M. ^{[42
]}

Aronson, S. M. ^{[2
]}

Arun, K. G. ^{[43
]}

机构：

[1] CALTECH, LIGO Lab, Pasadena, CA 91125 USA

[2] Louisiana State Univ, Baton Rouge, LA 70803 USA

[3] Univ Salerno, Dipartimento Farm, I-84084 Salerno, Italy

[4] Ist Nazl Fis Nucl, Complesso Univ Monte S Angelo, Sez Napoli, I-80126 Naples, Italy

[5] Monash Univ, Sch Phys & Astron, OzGrav, Clayton, Vic 3800, Australia

[6] LIGO Livingston Observ, Livingston, LA 70754 USA

[7] Univ Wisconsin Milwaukee, Milwaukee, WI 53201 USA

[8] Australian Natl Univ, OzGrav, Canberra, ACT 0200, Australia

[9] Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-30167 Hannover, Germany

[10] Leibniz Univ Hannover, D-30167 Hannover, Germany

[11] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India

[12] Univ Cambridge, Cambridge CB2 1TN, England

[13] Friedrich Schiller Univ Jena, Theoret Phys Inst, D-07743 Jena, Germany

[14] Univ Birmingham, Birmingham B15 2TT, W Midlands, England

[15] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astron CIERA, Evanston, IL 60208 USA

[16] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, SP, Brazil

[17] Cardiff Univ, Grav Explorat Inst, Cardiff CF24 3AA, Wales

[18] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy

[19] Tata Inst Fundamental Res, Int Ctr Theoret Sci, Bengaluru 560089, India

[20] Univ Coll Dublin, Dublin 4, Ireland

[21] Natl Astron Observ Japan, Gravitat Wave Sci Project, Mitaka, Tokyo 1818588, Japan

[22] Natl Astron Observ Japan, Adv Technol Ctr, Mitaka, Tokyo 1818588, Japan

[23] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy

[24] Univ Napoli Federico II, Complesso Univ Monte S Angelo, I-80126 Naples, Italy

[25] Univ Claude Bernard Lyon 1, Univ Lyon, CNRS, Inst Lumiere Mat, F-69622 Villeurbanne, France

[26] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan

[27] Univ Tokyo, Res Ctr Early Universe RESCEU, Bunkyo Ku, Tokyo 1130033, Japan

[28] Univ Barcelona, Inst Ciencies Cosmos ICCUB, C Marti & Franques 1, E-08028 Barcelona, Spain

[29] Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules LAPP, CNRS,IN2P3, F-74941 Annecy, France

[30] Gran Sasso Sci Inst GSSI, I-67100 Laquila, Italy

[31] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland

[32] Univ Udine, Dipartimento Sci Matemat Informat & Fis, I-33100 Udine, Italy

[33] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy

[34] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA

[35] Univ Paris, CNRS, Astroparticule & Cosmol, F-75006 Paris, France

[36] Univ Tokyo, Inst Cosm Ray Res ICRR, KAGRA Observ, Kashiwa, Chiba 2778582, Japan

[37] High Energy Accelerator Res Org KEK, Accelerator Lab, Tsukuba, Ibaraki 3050801, Japan

[38] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130032, Japan

[39] Calif State Univ Fullerton, Fullerton, CA 92831 USA

[40] Univ Paris Saclay, IJCLab, CNRS, IN2P3, F-91405 Orsay, France

[41] European Gravitat Observ, I-56021 Pisa, Italy

[42] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA

[43] Chennai Math Inst, Chennai 603103, Tamil Nadu, India

[44] Hirosaki Univ, Dept Math & Phys, Gravitat Wave Sci Project, Hirosaki, Aomori 0368561, Japan

[45] Columbia Univ, New York, NY 10027 USA

[46] Natl Astron Observ Japan, Kamioka Branch, Kamioka Cho, Hida City, Gifu 5061205, Japan

[47] Grad Univ Adv Studies SOKENDAI, Mitaka, Tokyo 1818588, Japan

[48] Univ Urbino Carlo Bo, I-61029 Urbino, Italy

[49] Ist Nazl Fis Nucl, Sez Firenze, I-50019 Florence, Italy

[50] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy

来源：

PHYSICAL REVIEW X | 2023年 / 13卷 / 04期

基金：

新加坡国家研究基金会; 瑞士国家科学基金会; 美国国家科学基金会; 美国能源部; 匈牙利科学研究基金会; 中国国家自然科学基金; 俄罗斯科学基金会; 俄罗斯基础研究基金会;

关键词：

BLACK-HOLE MERGERS; GRAVITATIONAL-WAVE EVENTS; PAIR-INSTABILITY SUPERNOVAE; GAMMA-RAY BURSTS; CORE-COLLAPSE SUPERNOVAE; FOLLOW-UP OBSERVATION; EQUATION-OF-STATE; MAXIMUM MASS; ELECTROMAGNETIC COUNTERPARTS; MULTIMESSENGER SEARCHES;

D O I：

10.1103/PhysRevX.13.041039

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

The third Gravitational -Wave Transient Catalog (GWTC-3) describes signals detected with Advanced LIGO and Advanced Virgo up to the end of their third observing run. Updating the previous GWTC-2.1, we present candidate gravitational waves from compact binary coalescences during the second half of the third observing run (O3b) between 1 November 2019, 15:00 Coordinated Universal Time (UTC) and 27 March 2020, 17:00 UTC. There are 35 compact binary coalescence candidates identified by at least one of our search algorithms with a probability of astrophysical origin p(astro) > 0.5. Of these, 18 were previously reported as low -latency public alerts, and 17 are reported here for the first time. Based upon estimates for the component masses, our O3b candidates with p(astro) > 0.5 are consistent with gravitational -wave signals from binary black holes or neutron-star-black-hole binaries, and we identify none from binary neutron stars. However, from the gravitational -wave data alone, we are not able to measure matter effects that distinguish whether the binary components are neutron stars or black holes. The range of inferred component masses is similar to that found with previous catalogs, but the O3b candidates include the first confident observations of neutron-star-black-hole binaries. Including the 35 candidates from O3b in addition to those from GWTC-2.1, GWTC-3 contains 90 candidates found by our analysis with p(astro) > 0.5 across the first three observing runs. These observations of compact binary coalescences present an unprecedented view of the properties of black holes and neutron stars.

引用

页数：89

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