Diving below the Spin-down Limit: Constraints on Gravitational Waves from the Energetic Young Pulsar PSR J0537-6910

被引：32

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. ^{[23
,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
]}

Arun, K. G. ^{[43
]}

Asada, H. ^{[44
]}

Asali, Y. ^{[45
]}

Ashton, G. ^{[6
]}

Aso, Y. ^{[46
,47
]}

机构：

[1] CALTECH, LIGO, 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 Claude Bernard Lyon 1, CNRS, Univ Lyon, Inst Lumiere Matiere, 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] Chennai Math Inst, Chennai 603103, Tamil Nadu, India

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

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

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

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

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

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

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

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2021年 / 913卷 / 02期

基金：

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

关键词：

Gravitational waves; SUPERNOVA REMNANT; R-MODE; BIG GLITCHER; 1ST SEARCH; ROTATION; HISTORY; N157B;

D O I：

10.3847/2041-8213/abffcd

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a search for quasi-monochromatic gravitational-wave signals from the young, energetic X-ray pulsar PSR J0537-6910 using data from the second and third observing runs of LIGO and Virgo. The search is enabled by a contemporaneous timing ephemeris obtained using Neutron star Interior Composition Explorer (NICER) data. The NICER ephemeris has also been extended through 2020 October and includes three new glitches. PSR J0537-6910 has the largest spin-down luminosity of any pulsar and exhibits fRequent and strong glitches. Analyses of its long-term and interglitch braking indices provide intriguing evidence that its spin-down energy budget may include gravitational-wave emission from a time-varying mass quadrupole moment. Its 62 Hz rotation frequency also puts its possible gravitational-wave emission in the most sensitive band of the LIGO/Virgo detectors. Motivated by these considerations, we search for gravitational-wave emission at both once and twice the rotation frequency from PSR J0537-6910. We find no signal, however, and report upper limits. Assuming a rigidly rotating triaxial star, our constraints reach below the gravitational-wave spin-down limit for this star for the first time by more than a factor of 2 and limit gravitational waves from the l = m = 2 mode to account for less than 14% of the spin-down energy budget. The fiducial equatorial ellipticity is constrained to less than about 3 x10(-5), which is the third best constraint for any young pulsar.

引用

页数：15

共 15 条

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