Improving astrophysical parameter estimation via offline noise subtraction for Advanced LIGO

被引：83

作者：

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

Vitale, S. ^{[2
]}

Lundgren, A. P. ^{[3
]}

Evans, M. ^{[2
]}

Kawabe, K. ^{[1
]}

Dwyer, S. E. ^{[1
]}

Izumi, K. ^{[1
]}

Schofield, R. M. S. ^{[4
]}

Effler, A. ^{[5
]}

Sigg, D. ^{[1
]}

Fritschel, P. ^{[2
]}

Drago, M. ^{[3
]}

Nitz, A. ^{[3
]}

Abbott, B. P. ^{[6
]}

Abbott, R. ^{[6
]}

Abbott, T. D. ^{[7
]}

Adams, C. ^{[5
]}

Adhikari, R. X. ^{[6
]}

Adya, V. B. ^{[3
]}

Ananyeva, A. ^{[6
]}

Appert, S. ^{[6
]}

Arai, K. ^{[6
]}

Aston, S. M. ^{[5
]}

Austin, C. ^{[7
]}

Ballmer, S. W. ^{[8
]}

Barker, D. ^{[1
]}

Barr, B. ^{[9
]}

Barsotti, L. ^{[2
]}

Bartlett, J. ^{[1
]}

Bartos, I ^{[10
]}

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

Bell, A. S. ^{[9
]}

Betzwieser, J. ^{[5
]}

Billingsley, G. ^{[6
]}

Birch, J. ^{[5
]}

Biscans, S. ^{[2
]}

Blair, C. D. ^{[5
]}

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

Bork, R. ^{[6
]}

Brooks, A. F. ^{[6
]}

Cao, H. ^{[11
]}

Ciani, G. ^{[10
]}

Clara, F. ^{[1
]}

Cooper, S. J. ^{[12
]}

Corban, P. ^{[5
]}

Countryman, S. T. ^{[13
]}

Covas, P. B. ^{[14
]}

Cowart, M. J. ^{[5
]}

Coyne, D. C. ^{[6
]}

Cumming, A. ^{[9
]}

机构：

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

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

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

[4] Univ Oregon, Eugene, OR 97403 USA

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

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

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

[8] Syracuse Univ, Syracuse, NY 13244 USA

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

[10] Univ Florida, Gainesville, FL 32611 USA

[11] Univ Adelaide, OzGrav, Adelaide, SA 5005, Australia

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

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

[14] Univ Illes Balears, IAC3 IEEC, E-07122 Palma De Mallorca, Spain

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

[16] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England

[17] Stanford Univ, Stanford, CA 94305 USA

[18] Calif State Univ Los Angeles, 5151 State Univ Dr, Los Angeles, CA 90032 USA

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

[20] Univ Mississippi, University, MS 38677 USA

[21] Inst Nacl Pesquisas Espaciais, BR-12227010 Seto Jose Dos Campos, SP, Brazil

[22] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada

[23] Univ Michigan, Ann Arbor, MI 48109 USA

[24] Amer Univ, Washington, DC 20016 USA

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

[26] Univ Western Australia, OzGrav, Crawley, WA 6009, Australia

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

[28] Univ Washington Bothell, 18115 Campus Way NE, Washington, WA 98011 USA

[29] Univ Minnesota, Minneapolis, MN 55455 USA

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

[31] Hobart & William Smith Coll, Geneva, NY 14456 USA

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

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

[34] Lomonosov Moscow State Univ, Fac Phys, Moscow 119991, Russia

[35] Univ Texas Rio Grande Valley, Brownsville, TX 78520 USA

[36] Eotvos Lorand Univ, Inst Phys, Pazmany Ps 1-A, H-1117 Budapest, Hungary

[37] Univ Washington, Seattle, WA 98195 USA

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

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

[40] Univ Maryland, College Pk, MD 20742 USA

来源：

PHYSICAL REVIEW D | 2019年 / 99卷 / 04期

基金：

美国国家科学基金会;

关键词：

D O I：

10.1103/PhysRevD.99.042001

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Advanced LIGO detectors have recently completed their second observation run successfully. The run lasted for approximately 10 months and led to multiple new discoveries. The sensitivity to gravitational waves was partially limited by laser noise. Here, we utilize auxiliary sensors that witness these correlated noise sources, and use them for noise subtraction in the time domain data. This noise and line removal is particularly significant for the LIGO Hanford Observatory, where the improvement in sensitivity is greater than 20%. Consequently, we were also able to improve the astrophysical estimation for the location, masses, spins, and orbital parameters of the gravitational wave progenitors.

引用

页数：9

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