A gravitational-wave standard siren measurement of the Hubble constant

被引：684

作者：

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

Abbott, R. ^{[1
]}

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

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

Ackley, K. ^{[5
,6
]}

Adams, C. ^{[7
]}

Adams, T. ^{[8
]}

Addesso, P. ^{[4
,9
]}

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

Adya, V. B. ^{[10
]}

Affeldt, C. ^{[10
]}

Afrough, M. ^{[11
]}

Agarwal, B. ^{[12
]}

Agathos, M. ^{[13
]}

Agatsuma, K. ^{[14
]}

Aggarwal, N. ^{[15
]}

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

Aiello, L. ^{[17
,18
]}

Ain, A. ^{[19
]}

Ajith, P. ^{[20
]}

Allen, B. ^{[10
,21
,22
]}

Allen, G. ^{[12
]}

Allocca, A. ^{[23
,24
]}

Altin, P. A. ^{[25
]}

Amato, A. ^{[26
]}

Ananyeva, A. ^{[1
]}

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

Anderson, W. G. ^{[21
]}

Angelova, S. V. ^{[27
]}

Antier, S. ^{[28
]}

Appert, S. ^{[1
]}

Arai, K. ^{[1
]}

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

Areeda, J. S. ^{[29
]}

Arnaud, N. ^{[28
,30
]}

Arun, K. G. ^{[31
]}

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

Ashton, G. ^{[10
]}

Ast, M. ^{[34
]}

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

Astone, P. ^{[35
]}

Atallah, D. V. ^{[36
]}

Aufmuth, P. ^{[22
]}

Aulbert, C. ^{[10
]}

AultO'Neal, K. ^{[37
]}

Austin, C. ^{[2
]}

Avila-Alvarez, A. ^{[29
]}

Babak, S. ^{[38
]}

Bacon, P. ^{[39
]}

Bader, M. K. M. ^{[14
]}

机构：

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

[2] Louisiana State Univ, Baton Rouge, LA 70303 USA

[3] Univ Salerno, I-34084 Salerno, Italy

[4] INFN, Sez Napoli, Complesso Univ Monte St Angelo, I-80126 Naples, Italy

[5] Univ Florida, Gainesville, FL 32611 USA

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

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

[8] Univ Savoie Mt Blanc, LAPP, CNRS IN2P3, F-74941 Annecy, France

[9] Univ Sannio Benevento, I-82100 Benevento, Italy

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

[11] Univ Mississippi, University, MS 38677 USA

[12] Univ Illinois, NCSA, Urbana, IL 61301 USA

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

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

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

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

[17] GSSI, I-67100 Laquila, Italy

[18] INFN, Lab Nazl Gran Sasso, I-67100 Laquila, Italy

[19] Interunivers Ctr Astron & Astrophys, Pune 411007, Maharashtra, India

[20] Tata Inst Fundamental Res, Int Ctr Theoret Sci, Bengaluru 560039, India

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

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

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

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

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

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

[27] Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland

[28] Univ Paris Sud, Univ Paris Saclay, CNRS IN2P3, LAL, F-91393 Orsay, France

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

[30] EGO, I-56021 Cascina, Italy

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

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

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

[34] Univ Hamburg, D-22761 Hamburg, Germany

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

[36] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales

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

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

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

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

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

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

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

[44] Syracuse Univ, Syracuse, NY 13244 USA

[45] Univ Minnesota, Minneapolis, MN 55455 USA

[46] Univ Glasgow, SUPA, Glasgow G12 3QQ, Lanark, Scotland

[47] CALTECH, CaRT, Pasadena, CA 91125 USA

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

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

[50] Stanford Univ, Stanford, CA 94305 USA

来源：

NATURE | 2017年 / 551卷 / 7678期

基金：

美国国家科学基金会; 澳大利亚研究理事会; 俄罗斯科学基金会; 瑞士国家科学基金会; 新加坡国家研究基金会; 英国科学技术设施理事会; 俄罗斯基础研究基金会; 匈牙利科学研究基金会; 中国国家自然科学基金; 以色列科学基金会;

关键词：

TELESCOPE KEY PROJECT; GAMMA-RAY BURSTS; GALAXIES; DENSITY;

D O I：

10.1038/nature24471

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

On 17 August 2017, the Advanced LIGO(1) and Virgo(2) detectors observed the gravitational-wave event GW170817-a strong signal from the merger of a binary neutron-star system(3). Less than two seconds after the merger, a gamma-ray burst (GRB 170817A) was detected within a region of the sky consistent with the LIGO-Virgo-derived location of the gravitational-wave source(4-6). This sky region was subsequently observed by optical astronomy facilities(7), resulting in the identification(8-13) of an optical transient signal within about ten arcseconds of the galaxy NGC 4993. This detection of GW170817 in both gravitational waves and electromagnetic waves represents the first 'multi-messenger' astronomical observation. Such observations enable GW170817 to be used as a 'standard siren'(14-18) (meaning that the absolute distance to the source can be determined directly from the gravitational-wave measurements) to measure the Hubble constant. This quantity represents the local expansion rate of the Universe, sets the overall scale of the Universe and is of fundamental importance to cosmology. Here we report a measurement of the Hubble constant that combines the distance to the source inferred purely from the gravitational-wave signal with the recession velocity inferred from measurements of the redshift using the electromagnetic data. In contrast to previous measurements, ours does not require the use of a cosmic 'distance ladder'(19): the gravitational-wave analysis can be used to estimate the luminosity distance out to cosmological scales directly, without the use of intermediate astronomical distance measurements. We determine the Hubble constant to be about 70 kilometres per second per megaparsec. This value is consistent with existing measurements(20,21), while being completely independent of them. Additional standard siren measurements from future gravitational-wave sources will enable the Hubble constant to be constrained to high precision.

引用

页码：85 / +

页数：14

共 50 条

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