GWTC-2.1: Deep extended catalog of compact binary coalescences observed by LIGO and Virgo during the first half of the third observing run

被引：117

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
]}

Albanesi, S. ^{[20
]}

Allocca, A. ^{[4
,21
]}

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

Amato, A. ^{[22
]}

Anand, C. ^{[5
]}

Anand, S. ^{[1
]}

Ananyeva, A. ^{[1
]}

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

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

Andrade, T. ^{[23
]}

Andres, N. ^{[24
]}

Andric, T. ^{[25
]}

Angelova, S., V ^{[26
]}

Ansoldi, S. ^{[27
,28
]}

Antelis, J. M. ^{[29
]}

Antier, S. ^{[30
]}

Appert, S. ^{[1
]}

Arai, K. ^{[1
]}

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

Areeda, J. S. ^{[31
]}

Arene, M. ^{[30
]}

Arnaud, N. ^{[32
,33
]}

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

Arun, K. G. ^{[34
]}

Asali, Y. ^{[35
]}

Ashton, G. ^{[5
]}

Assiduo, M. ^{[36
,37
]}

Aston, S. M. ^{[6
]}

Astone, P. ^{[38
]}

Aubin, F. ^{[24
]}

Austin, C. ^{[2
]}

Babak, S. ^{[30
]}

Badaracco, F. ^{[39
]}

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] Complesso Univ Monte S Angelo, Sez Napoli, Ist Nazl Fis Nucl, 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 Astrophys CI, 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] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy

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

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

[23] Univ Barcelona, Inst Ciencies Cosmos ICCUB, C Marti i Franques 1, Barcelona 08028, Spain

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

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

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

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

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

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

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

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

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

[33] European Gravitat Observ EGO, I-56021 Pisa, Italy

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

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

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

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

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

[39] Catholic Univ Louvain, B-1348 Louvain La Neuve, Belgium

[40] Nikhef, Sci Pk 105, NL-1098 XG Amsterdam, Netherlands

[41] Univ London, Kings Coll London, London WC2R 2LS, England

[42] Korea Inst Sci & Technol Informat KISTI, Daejeon 34141, South Korea

[43] Christopher Newport Univ, Newport News, VA 23606 USA

[44] Univ Oregon, Eugene, OR 97403 USA

[45] Syracuse Univ, Syracuse, NY 13244 USA

[46] Univ Liege, B-4000 Liege, Belgium

[47] Univ Minnesota, Minneapolis, MN 55455 USA

[48] Univ Milano Bicocca, I-20126 Milan, Italy

[49] Ist Nazl Fis Nucl, Sez Milano Bicocca, I-20126 Milan, Italy

[50] INAF, Osservatorio Astron Brera, Sede Merate, I-23807 Merate, Lecco, Italy

来源：

PHYSICAL REVIEW D | 2024年 / 109卷 / 02期

基金：

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

关键词：

BLACK-HOLE MERGERS; GRAVITATIONAL-WAVE OBSERVATIONS; NEUTRON-STAR; MASS-GAP; BAYESIAN-INFERENCE; HIERARCHICAL MERGERS; AGN DISCS; POPULATION; SPIN; EVOLUTION;

D O I：

10.1103/PhysRevD.109.022001

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The second Gravitational-Wave Transient Catalog, GWTC-2, reported on 39 compact binary coalescences observed by the Advanced LIGO and Advanced Virgo detectors between 1 April 2019 1500 UTC and 1 October 2019 1500 UTC. Here, we present GWTC-2.1, which reports on a deeper list of candidate events observed over the same period. We analyze the final version of the strain data over this period with improved calibration and better subtraction of excess noise, which has been publicly released. We employ three matched-filter search pipelines for candidate identification, and estimate the probability of astrophysical origin for each candidate event. While GWTC-2 used a false alarm rate threshold of 2 per year, we include in GWTC-2.1, 1201 candidates that pass a false alarm rate threshold of 2 per day. We calculate the source properties of a subset of 44 high-significance candidates that have a probability of astrophysical origin greater than 0.5. Of these candidates, 36 have been reported in GWTC-2. We also calculate updated source properties for all binary black hole events previously reported in GWTC-1. If the eight additional high-significance candidates presented here are astrophysical, the mass range of events that are unambiguously identified as binary black holes (both objects >= 3M(circle dot)) is increased compared to GWTC-2, with total masses from similar to 14M(circle dot) for GW190924_021846 to similar to 182M(circle dot) for GW190426_190642. Source properties calculated using our default prior suggest that the primary components of two new candidate events (GW190403_051519 and GW190426_190642) fall in the mass gap predicted by pair-instability supernova theory. We also expand the population of binaries with significantly asymmetric mass ratios reported in GWTC-2 by an additional two events (the mass ratio is less than 0.65 and 0.44 at 90% probability for GW190403_051519 and GW190917_114630 respectively), and find that two of the eight new events have effective inspiral spins chi(eff)>0 (at 90% credibility), while no binary is consistent with chi(eff)<0 at the same significance. We provide updated estimates for rates of binary black hole and binary neutron star coalescence in the local Universe.

引用

页数：45

共 308 条

[91] The chemically homogeneous evolutionary channel for binary black hole mergers: rates and properties of gravitational-wave events detectable by advanced LIGO [J].