Search for Post-merger Gravitational Waves from the Remnant of the Binary Neutron Star Merger GW170817

被引：192

作者：

Abbott, B. P.

Abbott, R. ^{[1
]}

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

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

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

Adams, C. ^{[7
,8
]}

Adams, T.

Addesso, P. ^{[9
,10
]}

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

Adya, V. B. ^{[11
]}

Affeldt, C. ^{[11
]}

Afrough, M. ^{[12
]}

Agarwal, B. ^{[13
]}

Agathos, M. ^{[14
]}

Agatsuma, K. ^{[15
]}

Aggarwal, N. ^{[16
]}

Aguiar, O. D. ^{[17
]}

Aiello, L. ^{[18
,19
]}

Ain, A. ^{[11
,16
,20
]}

Ajith, P. ^{[21
]}

Allen, B. ^{[11
,22
,23
]}

Allen, G. ^{[13
]}

Allocca, A. ^{[24
,25
]}

Altin, P. A. ^{[26
]}

Amato, A. ^{[27
]}

Ananyeva, A. ^{[1
]}

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

Anderson, W. G. ^{[22
]}

Angelova, S. V. ^{[28
]}

Antier, S. ^{[29
]}

Appert, S. ^{[1
]}

Arai, K. ^{[1
]}

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

Areeda, J. S. ^{[30
]}

Arnaud, N. ^{[29
,31
]}

Arun, K. G. ^{[32
]}

Ascenzi, S. ^{[33
,34
]}

Ashton, G. ^{[11
]}

Ast, M. ^{[35
]}

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

Astone, P. ^{[36
]}

Atallah, D. V. ^{[37
]}

Aufmuth, P. ^{[23
]}

Aulbert, C. ^{[11
]}

AultONeal, K. ^{[38
]}

Austin, C. ^{[2
]}

Avila-Alvarez, A. ^{[30
]}

Babak, S. ^{[39
]}

Bacon, P. ^{[40
]}

Bader, M. K. M. ^{[15
]}

机构：

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

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

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

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

[5] Univ Florida, Gainesville, FL 32611 USA

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

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

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

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

[10] INFN, Sez Napoli, I-80100 Naples, Italy

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

[12] Univ Mississippi, University, MS 38677 USA

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

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

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

[16] MIT, LIGO, Cambridge, MA 02139 USA

[17] Inst Nacl Pesquisas Espaciais, Sao Jose Campos, BR-12227010 Sao Paulo, Brazil

[18] GSSI, I-67100 Laquila, Italy

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

[20] Inter Univ, Ctr Astron & Astrophys, Pune 411007, Maharashtra, India

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

[22] Univ Wisconsin, Milwaukee, WI 53201 USA

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

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

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

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

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

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

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

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

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

[32] Chennai Math Inst, Madras 603103, Tamil Nadu, India

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

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

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

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

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

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

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

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

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

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

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

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

[45] Syracuse Univ, Syracuse, NY 13244 USA

[46] Univ Minnesota, Minneapolis, MN 55455 USA

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

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

[49] Caltech CaRT, Pasadena, CA 91125 USA

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

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2017年 / 851卷 / 01期

基金：

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

关键词：

gravitational waves; methods: data analysis; stars: neutron; RADIATION INSTABILITY; BRAKING; HOT;

D O I：

10.3847/2041-8213/aa9a35

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The first observation of a binary neutron star (NS) coalescence by the Advanced LIGO and Advanced Virgo gravitational-wave (GW) detectors offers an unprecedented opportunity to study matter under the most extreme conditions. After such a merger, a compact remnant is left over whose nature depends primarily on the masses of the inspiraling objects and on the equation of state of nuclear matter. This could be either a black hole (BH) or an NS, with the latter being either long-lived or too massive for stability implying delayed collapse to a BH. Here, we present a search for GWs from the remnant of the binary NS merger GW170817 using data from Advanced LIGO and Advanced Virgo. We search for short-(less than or similar to 1 s) and intermediate-duration (less than or similar to 500 s) signals, which include GW emission from a hypermassive NS or supramassive NS, respectively. We find no signal from the post-merger remnant. Our derived strain upper limits are more than an order of magnitude larger than those predicted by most models. For short signals, our best upper limit on the root sum square of the GW strain emitted from 1-4 kHz is h(rss)(50%) = 2.1 x 10(-22) Hz(-1/2) detection efficiency. For intermediate-duration signals, our best upper limit at 50% detection efficiency is h(rss) (50%) = 8.4 x 10(-22) Hz(-1/2) for a millisecond magnetar model, and h(rss)(50%) = 5.9 x 10(-22) Hz(-1/2) for a bar-mode model. These results indicate that post-merger emission from a similar event may be detectable when advanced detectors reach design sensitivity or with next-generation detectors.

引用

页数：13

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