Search for anisotropic gravitational-wave backgrounds using data from Advanced LIGO and Advanced Virgo's first three observing runs

被引：50

作者：

Abbott, R. ^{[1
]}

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

Abraham, S. ^{[3
]}

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

Ackley, K. ^{[6
]}

Adams, A. ^{[7
]}

Adams, C. ^{[8
]}

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

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

Affeldt, C. ^{[10
,11
]}

Agarwal, D. ^{[3
]}

Agathos, M. ^{[12
,13
]}

Agatsuma, K. ^{[14
]}

Aggarwal, N. ^{[15
]}

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

Aiello, L. ^{[17
,18
,19
]}

Ain, A. ^{[20
,21
]}

Ajith, P. ^{[22
]}

Akutsu, T. ^{[23
,24
]}

Aleman, K. M. ^{[25
]}

Allen, G. ^{[26
]}

Allocca, A. ^{[5
,27
]}

Altin, P. A. ^{[9
]}

Amato, A. ^{[28
]}

Anand, S. ^{[1
]}

Ananyeva, A. ^{[1
]}

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

Anderson, W. G. ^{[29
]}

Ando, M. ^{[30
,31
]}

Angelova, S., V ^{[32
]}

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

Antelis, J. M. ^{[35
]}

Antier, S. ^{[36
]}

Appert, S. ^{[1
]}

Arai, Koya ^{[37
]}

Arai, Koji ^{[1
]}

Arai, Y. ^{[37
]}

Araki, S. ^{[38
]}

Araya, A. ^{[39
]}

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

Areeda, J. S. ^{[25
]}

Arene, M. ^{[36
]}

Aritomi, N. ^{[30
]}

Arnaud, N. ^{[40
,41
]}

Aronson, S. M. ^{[42
]}

Asada, H. ^{[43
]}

Asali, Y. ^{[44
]}

Ashton, G. ^{[6
]}

Aso, Y. ^{[45
,46
]}

Aston, S. M. ^{[8
]}

机构：

[1] CALTECH, LIGO Lab, 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, Dipartimento Farm, I-84084 Salerno, Italy

[5] Complesso Univ Monte S Angelo, Sez Napoli, Ist Nazl Fis Nucl, I-80126 Naples, Italy

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

[7] Christopher Newport Univ, Newport News, VA 23606 USA

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

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

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

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

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

[13] Friedrich Schiller Univ Jena, Theoret Phys Inst, D-07743 Jena, Germany

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

[15] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys CI, Evanston, IL 60208 USA

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

[17] Cardiff Univ, Grav Explorat Inst, Cardiff CF24 3AA, Wales

[18] Gran Sasso Sci Inst GSSI, I-67100 Laquila, Italy

[19] Ist Nazl Fis Nucl, Lab Nazl Gran Sasso, I-67100 Assergi, Italy

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

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

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

[23] Natl Astron Observ Japan NAOJ, Gravitat Wave Sci Project, Mitaka, Tokyo 1818588, Japan

[24] Natl Astron Observ Japan NAOJ, Adv Technol Ctr, Mitaka, Tokyo 1818588, Japan

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

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

[27] Univ Napoli Federico II, Complesso Univ Monte S Angelo, I-80126 Naples, Italy

[28] Univ Lyon, CNRS, Inst Lumiere Matiere, Univ Claude Bernard Lyon 1, F-69622 Villeurbanne, France

[29] Univ Wisconsin, Milwaukee, WI 53201 USA

[30] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan

[31] Univ Tokyo, Res Ctr Early Universe RESCEU, Bunkyo Ku, Tokyo 1130033, Japan

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

[33] Univ Udine, Dipartimento Matemat & Informat, I-33100 Udine, Italy

[34] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy

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

[36] Univ Paris, CNRS, Astroparticule & Cosmol, F-75006 Paris, France

[37] Univ Tokyo, Inst Cosm Ray Res ICRR, KAGRA Observ, Kashiwa, Chiba 2778582, Japan

[38] High Energy Accelerator Res Org KEK, Accelerator Lab, Tsukuba, Ibaraki 3050801, Japan

[39] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130032, Japan

[40] Univ Paris Saclay, IJCLab, CNRS IN2P3, F-91405 Orsay, France

[41] European Gravitat Observ EGO, I-56021 Pisa, Italy

[42] Univ Florida, Gainesville, FL 32611 USA

[43] Hirosaki Univ, Dept Math & Phys, Hirosaki, Aomori 0368561, Japan

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

[45] Natl Astron Observ Japan NAOJ, Kamioka Branch, Kamioka Cho, Hida City, Gifu 5061205, Japan

[46] Grad Univ Adv Studies SOKENDAI, Mitaka, Tokyo 1818588, Japan

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

[48] Univ Grenoble Alpes, Lab Annecy Phys Particules LAPP, Univ Savoie Mt Blanc, CNRS IN2P3, F-74941 Annecy, France

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

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

来源：

PHYSICAL REVIEW D | 2021年 / 104卷 / 02期

基金：

匈牙利科学研究基金会; 中国国家自然科学基金; 美国能源部; 瑞士国家科学基金会; 美国国家科学基金会; 俄罗斯基础研究基金会; 新加坡国家研究基金会; 俄罗斯科学基金会; 澳大利亚研究理事会;

关键词：

CROSS-CORRELATION SEARCH; UPPER LIMITS; RADIATION;

D O I：

10.1103/PhysRevD.104.022005

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report results from searches for anisotropic stochastic gravitational-wave backgrounds using data from the first three observing runs of the Advanced LIGO and Advanced Virgo detectors. For the first time, we include Virgo data in our analysis and run our search with a new efficient pipeline called PyStoch on data folded over one sidereal day. We use gravitational-wave radiometry (broadband and narrow band) to produce sky maps of stochastic gravitational-wave backgrounds and to search for gravitational waves from point sources. A spherical harmonic decomposition method is employed to look for gravitationalwave emission from spatially-extended sources. Neither technique found evidence of gravitational-wave signals. Hence we derive 95% confidence-level upper limit sky maps on the gravitational-wave energy flux from broadband point sources, ranging from F-a,F-Theta < (0.013-7.6) x 10(-8) erg cm(-2) s(-1) Hz(-1), and on the (normalized) gravitational-wave energy density spectrum from extended sources, ranging from Omega(a,Theta) < (0.57-9.3) x 10(-9) sr(-1), depending on direction (Theta) and spectral index (alpha). These limits improve upon previous limits by factors of 2.9-3.5. We also set 95% confidence level upper limits on the frequencydependent strain amplitudes of quasimonochromatic gravitational waves coming from three interesting targets, Scorpius X-1, SN 1987A and the Galactic Center, with best upper limits range from h(0) < (1.7-2.1) x 10(-25), a factor of >= 2.0 improvement compared to previous stochastic radiometer searches.

引用

页数：25

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