GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs

被引：2776

作者：

Abbott, B. P. ^{[1
]}

Abbott, R. ^{[1
]}

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

Abraham, S. ^{[3
]}

Acernese, F. ^{[4
,5
]}

Ackley, K. ^{[6
]}

Adams, C. ^{[7
]}

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

Adya, V. B. ^{[8
,9
]}

Affeldt, C. ^{[8
,9
]}

Agathos, M. ^{[10
]}

Agatsuma, K. ^{[11
]}

Aggarwal, N. ^{[12
]}

Aguiar, O. D. ^{[13
]}

Aiello, L. ^{[14
,15
]}

Ain, A. ^{[3
]}

Ajith, P. ^{[16
]}

Allen, G. ^{[17
]}

Allocca, A. ^{[18
,19
]}

Aloy, M. A. ^{[20
]}

Altin, P. A. ^{[21
]}

Amato, A. ^{[22
]}

Ananyeva, A. ^{[1
]}

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

Anderson, W. G. ^{[23
]}

Angelova, S., V ^{[24
]}

Antier, S. ^{[25
]}

Appert, S. ^{[1
]}

Arai, K. ^{[1
]}

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

Areeda, J. S. ^{[26
]}

Arene, M. ^{[27
]}

Arnaud, N. ^{[25
,28
]}

Arun, K. G. ^{[29
]}

Ascenzi, S. ^{[30
,31
]}

Ashton, G. ^{[6
]}

Aston, S. M. ^{[7
]}

Astone, P. ^{[32
]}

Aubin, F. ^{[33
]}

Aufmuth, P. ^{[9
]}

AultONeal, K. ^{[34
]}

Austin, C. ^{[2
]}

Avendano, V ^{[35
]}

Avila-Alvarez, A. ^{[26
]}

Babak, S. ^{[27
,36
]}

Bacon, P. ^{[27
]}

Badaracco, F. ^{[14
,15
]}

Bader, M. K. M. ^{[37
]}

Bae, S. ^{[38
]}

Baker, P. T. ^{[39
]}

机构：

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

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

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

[4] Univ Salerno, I-84084 Salerno, Italy

[5] INFN, Sez Napoli, Complesso Univ Monte S Angelo, I-80126 Naples, Italy

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

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

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

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

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

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

[12] MIT, LIGO, 77 Massachusetts Ave, Cambridge, MA 02139 USA

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

[14] GSSI, I-67100 Laquila, Italy

[15] INFN, Lab Nazl Gran Sasso, I-67100 Assergi, Italy

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

[17] Univ Illinois, NCSA, Urbana, IL 61801 USA

[18] Univ Pisa, I-56127 Pisa, Italy

[19] INFN, Sez Pisa, I-56127 Pisa, Italy

[20] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain

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

[22] CNRS, LMA, IN2P3, F-69622 Villeurbanne, France

[23] Univ Wisconsin, Milwaukee, WI 53201 USA

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

[25] Univ Paris Saclay, Univ Paris Sud, CNRS IN2P3, LAL, F-91898 Orsay, France

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

[27] Univ Paris Diderot, Sorbonne Paris Cite, CEA Irfu, APC,AstroParticule & Cosmol,CNRS IN2P3,Observ Par, F-75205 Paris 13, France

[28] EGO, I-56021 Pisa, Italy

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

[30] Univ Roma Tor Vergata, I-00133 Rome, Italy

[31] INFN, Sez Roma Tor Vergata, I-00133 Rome, Italy

[32] INFN, Sez Roma, I-00185 Rome, Italy

[33] Univ Grenoble Alpes, Univ Savoie Mt Blanc, CNRS IN2P3, LAPP, F-74941 Annecy, France

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

[35] Montclair State Univ, Montclair, NJ 07043 USA

[36] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Potsdam, Germany

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

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

[39] West Virginia Univ, Morgantown, WV 26506 USA

[40] Univ Perugia, I-06123 Perugia, Italy

[41] INFN, Sez Perugia, I-06123 Perugia, Italy

[42] Syracuse Univ, Syracuse, NY 13244 USA

[43] Univ Minnesota, Minneapolis, MN 55455 USA

[44] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland

[45] LIGO Hanford Observ, Richland, WA 99352 USA

[46] Caltech CaRT, Pasadena, CA 91125 USA

[47] RMKI, Wigner RCP, Konkoly Thege Miklos Ut 29-33, H-1121 Budapest, Hungary

[48] Univ Florida, Gainesville, FL 32611 USA

[49] Stanford Univ, Stanford, CA 94305 USA

[50] Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy

来源：

PHYSICAL REVIEW X | 2019年 / 9卷 / 03期

基金：

俄罗斯基础研究基金会; 俄罗斯科学基金会; 英国科学技术设施理事会; 中国国家自然科学基金; 瑞士国家科学基金会; 美国国家科学基金会; 匈牙利科学研究基金会; 英国工程与自然科学研究理事会; 新加坡国家研究基金会;

关键词：

BLACK-HOLE; MASS; PROGENITORS; EVOLUTION; RADIATION; INFERENCE; METALLICITY; DYNAMICS; SIGNALS; OBJECTS;

D O I：

10.1103/PhysRevX.9.031040

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

We present the results from three gravitational-wave searches for coalescing compact binaries with component masses above 1 M-circle dot during the first and second observing runs of the advanced gravitational-wave detector network. During the first observing run (O1), from September 12, 2015 to January 19, 2016, gravitational waves from three binary black hole mergers were detected. The second observing run (O2), which ran from November 30, 2016 to August 25, 2017, saw the first detection of gravitational waves from a binary neutron star inspiral, in addition to the observation of gravitational waves from a total of seven binary black hole mergers, four of which we report here for the first time: GW170729, GW170809, GW170818, and GW170823. For all significant gravitational-wave events, we provide estimates of the source properties. The detected binary black holes have total masses between 18.6(-0.7)(+3.2) M-circle dot and 84.4(-11.1)(+15.8) M-circle dot and range in distance between 320(-110)(+120) and 2840(-1360)(+1400) Mpc. No neutron star-black hole mergers were detected. In addition to highly significant gravitational-wave events, we also provide a list of marginal event candidates with an estimated false-alarm rate less than 1 per 30 days. From these results over the first two observing runs, which include approximately one gravitational-wave detection per 15 days of data searched, we infer merger rates at the 90% confidence intervals of 110 - 3840 Gpc(-3) y(-1) for binary neutron stars and 9.7 - 101 Gpc(-3) y(-1) for binary black holes assuming fixed population distributions and determine a neutron star-black hole merger rate 90% upper limit of 610 Gpc(-3) y(-1).

引用

页数：49

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