Methods and results of a search for gravitational waves associated with gamma-ray bursts using the GEO 600, LIGO, and Virgo detectors

被引：27

作者：

Aasi, J. ^{[1
]}

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

Abbott, R. ^{[1
]}

Abbott, T. ^{[2
]}

Abernathy, M. R. ^{[1
]}

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

Ackley, K. ^{[5
]}

Adams, C. ^{[6
]}

Adams, T. ^{[7
]}

Addesso, P. ^{[8
,9
]}

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

Affeldt, C. ^{[10
]}

Agathos, M. ^{[11
]}

Aggarwal, N. ^{[12
]}

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

Ajith, P. ^{[14
]}

Alemic, A. ^{[15
]}

Allen, B. ^{[10
,16
,17
]}

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

Amariutei, D. ^{[5
]}

Andersen, M. ^{[20
]}

Anderson, R. A. ^{[1
]}

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

Anderson, W. G. ^{[16
]}

Arai, K. ^{[1
]}

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

Arceneaux, C. ^{[21
]}

Areeda, J. S. ^{[22
]}

Ast, S. ^{[17
]}

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

Astone, P. ^{[23
]}

Aufmuth, P. ^{[17
]}

Augustus, H. ^{[24
]}

Aulbert, C. ^{[10
]}

Aylott, B. E. ^{[24
]}

Babak, S. ^{[25
]}

Baker, P. T. ^{[26
]}

Ballardin, G. ^{[27
]}

Ballmer, S. W. ^{[15
]}

Barayoga, J. C. ^{[1
]}

Barbet, M. ^{[5
]}

Barish, B. C. ^{[1
]}

Barker, D. ^{[28
]}

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

Barr, B. ^{[29
]}

Barsotti, L. ^{[12
]}

Barsuglia, M. ^{[30
]}

Barton, M. A. ^{[28
]}

Bartos, I. ^{[31
]}

Bassiri, R. ^{[20
]}

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] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy

[5] Univ Florida, Gainesville, FL 32611 USA

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

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

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

[9] Ist Nazl Fis Nucl, Sez Napoli, I-80100 Naples, Italy

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

[11] Nikhef, NL-1098 XG Amsterdam, Netherlands

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

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

[14] Tata Inst Fundamental Res, Int Ctr Theoret Phys, Bangalore 560012, Karnataka, India

[15] Syracuse Univ, Syracuse, NY 13244 USA

[16] Univ Wisconsin, Milwaukee, WI 53201 USA

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

[18] Univ Siena, I-53100 Siena, Italy

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

[20] Stanford Univ, Stanford, CA 94305 USA

[21] Univ Mississippi, University, MS 38677 USA

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

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

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

[25] Max Planck Inst f r Gravitationsphys, Albert Einstein Inst, D-14476 Golm, Germany

[26] Montana State Univ, Bozeman, MT 59717 USA

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

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

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

[30] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, APC,CNRS IN2P3,CEA Irfu, F-75205 Paris 13, France

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

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

[33] CAMK PAN, PL-00716 Warsaw, Poland

[34] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland

[35] Univ Genoa, I-16146 Genoa, Italy

[36] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy

[37] Moscow MV Lomonosov State Univ, Fac Phys, Moscow 119991, Russia

[38] Univ Paris 11, CNRS, IN2P3, LAL, F-91898 Orsay, France

[39] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[40] Univ Western Australia, Crawley, WA 6009, Australia

[41] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands

[42] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice, France

[43] Univ Rennes 1, CNRS, Inst Phys Rennes, F-35042 Rennes, France

[44] Univ Savoie, CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules LAPP, F-74941 Annecy Le Vieux, France

[45] Washington State Univ, Pullman, WA 99164 USA

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

[47] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy

[48] Kyoto Univ, Yukawa Inst Theoret Phys, Kyoto 6068502, Japan

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

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

来源：

PHYSICAL REVIEW D | 2014年 / 89卷 / 12期

基金：

美国国家科学基金会; 澳大利亚研究理事会; 美国国家航空航天局; 新加坡国家研究基金会;

关键词：

SHORT-DURATION; NEUTRON-STARS; BLACK-HOLE; GRB; 051103; REDSHIFT; SUPERNOVA; AFTERGLOW; SCIENCE; ORIGIN; POPULATION;

D O I：

10.1103/PhysRevD.89.122004

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In this paper we report on a search for short-duration gravitational wave bursts in the frequency range 64 Hz-1792 Hz associated with gamma-ray bursts (GRBs), using data from GEO 600 and one of the LIGO or Virgo detectors. We introduce the method of a linear search grid to analyze GRB events with large sky localization uncertainties, for example the localizations provided by the Fermi Gamma-ray Burst Monitor (GBM). Coherent searches for gravitational waves (GWs) can be computationally intensive when the GRB sky position is not well localized, due to the corrections required for the difference in arrival time between detectors. Using a linear search grid we are able to reduce the computational cost of the analysis by a factor of O(10) for GBM events. Furthermore, we demonstrate that our analysis pipeline can improve upon the sky localization of GRBs detected by the GBM, if a high-frequency GW signal is observed in coincidence. We use the method of the linear grid in a search for GWs associated with 129 GRBs observed satellite-based gamma-ray experiments between 2006 and 2011. The GRBs in our sample had not been previously analyzed for GW counterparts. A fraction of our GRB events are analyzed using data from GEO 600 while the detector was using squeezed-light states to improve its sensitivity; this is the first search for GWs using data from a squeezed-light interferometric observatory. We find no evidence for GW signals, either with any individual GRB in this sample or with the population as a whole. For each GRB we place lower bounds on the distance to the progenitor, under an assumption of a fixed GW emission energy of 10(-2)M circle dot c(2), with a median exclusion distance of 0.8 Mpc for emission at 500 Hz and 0.3 Mpc at 1 kHz. The reduced computational cost associated with a linear search grid will enable rapid searches for GWs associated with Fermi GBM events once the advanced LIGO and Virgo detectors begin operation.

引用

页数：17

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