The second data release from the European Pulsar Timing Array V. Search for continuous gravitational wave signals

被引：8

作者：

Antoniadis, J. ^{[1
,2
]}

Arumugam, P. ^{[3
]}

Arumugam, S. ^{[4
]}

Babak, S. ^{[5
]}

Bagchi, M. ^{[6
,7
]}

Nielsen, A-S Bak ^{[2
,8
]}

Bassa, C. G. ^{[9
]}

Bathula, A. ^{[10
]}

Berthereau, A. ^{[11
,12
]}

Bonetti, M. ^{[13
,14
,15
]}

Bortolas, E. ^{[13
,14
,15
]}

Brook, P. R. ^{[16
,17
]}

Burgay, M. ^{[18
]}

Caballero, R. N. ^{[19
]}

Chalumeau, A. ^{[13
]}

Champion, D. J. ^{[2
]}

Chanlaridis, S. ^{[1
]}

Chen, S. ^{[20
]}

Cognard, I ^{[11
,12
]}

Dandapat, S. ^{[21
]}

Deb, D. ^{[6
]}

Desai, S. ^{[22
]}

Desvignes, G. ^{[2
]}

Dhanda-Batra, N. ^{[23
]}

Dwivedi, C. ^{[24
]}

Falxa, M. ^{[5
,11
]}

Ferdman, R. D. ^{[25
]}

Franchini, A. ^{[13
,14
]}

Gair, J. R. ^{[26
]}

Goncharov, B. ^{[27
,28
]}

Gopakumar, A. ^{[21
]}

Graikou, E. ^{[2
]}

Griessmeier, J-M ^{[11
,12
]}

Guillemot, L. ^{[11
,12
]}

Guo, Y. J. ^{[2
]}

Gupta, Y. ^{[29
]}

Hisano, S. ^{[30
]}

Hu, H. ^{[2
]}

Iraci, F. ^{[18
,31
]}

Izquierdo-Villalba, D. ^{[13
,14
]}

Jang, J. ^{[2
]}

Jawor, J. ^{[2
]}

Janssen, G. H. ^{[9
,32
]}

Jessner, A. ^{[2
]}

Joshi, B. C. ^{[3
,29
]}

Kareem, F. ^{[33
,34
]}

Karuppusamy, R. ^{[2
]}

Keane, E. F. ^{[35
]}

Keith, M. J. ^{[36
]}

Kharbanda, D. ^{[22
]}

机构：

[1] FORTH, Inst Astrophys, N Plastira 100, Iraklion 70013, Greece

[2] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany

[3] Indian Inst Technol Roorkee, Dept Phys, Roorkee 247667, Uttar Pradesh, India

[4] IIT Hyderabad, Dept Elect Engn, Kandi 502284, Telangana, India

[5] Univ Paris Cite, Astroparticule & Cosmol, CNRS, F-75013 Paris, France

[6] Inst Math Sci, CIT Campus, Chennai 600113, Tamil Nadu, India

[7] Homi Bhabha Natl Inst, Training Sch Complex, Mumbai 400094, Maharashtra, India

[8] Univ Bielefeld, Fak Phys, Postfach 100131, D-33501 Bielefeld, Germany

[9] Netherlands Inst Radio Astron, ASTRON, Oude Hoogeveensedijk 4, NL-7991 PD Dwingeloo, Netherlands

[10] Indian Inst Sci Educ & Res, Dept Phys Sci, Mohali 140306, Punjab, India

[11] Univ Orleans, Lab Phys & Chim Environm & Espace, CNRS, F-45071 Orleans 02, France

[12] Univ Orleans, Univ PSL, Observ Radioastron Nancay, Observ Paris, F-18330 Nancay, France

[13] Univ Milano Bicocca, Dipartimento Fis G Occhialini, Piazza Sci 3, I-20126 Milan, Italy

[14] Ist Nazl Fis Nucl, Sez Milano Bicocca, Piazza Sci 3, I-20126 Milan, Italy

[15] INAF Osservatorio Astron Brera, Via Brera 20, I-20121 Milan, Italy

[16] Univ Birmingham, Inst Gravitat Wave Astron, Birmingham B15 2TT, W Midlands, England

[17] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England

[18] INAF Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy

[19] Hellen Open Univ, Sch Sci & Technol, Patras 26335, Greece

[20] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China

[21] Tata Inst Fundamental Res, Dept Astron & Astrophys, Homi Bhabha Rd, Mumbai 400005, Maharashtra, India

[22] IIT Hyderabad, Dept Phys, Kandi 502284, Telangana, India

[23] Univ Delhi, Dept Phys & Astrophys, Delhi 110007, India

[24] Indian Inst Space Sci & Technol, Dept Earth & Space Sci, Valiamala 695547, Kerala, India

[25] Univ East Anglia, Fac Sci, Sch Phys, Norwich NR4 7TJ, Norfolk, England

[26] Albert Einstein Inst, Max Planck Inst Gravitat Phys, Muhlenberg 1, D-14476 Potsdam, Germany

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

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

[29] Natl Ctr Radio Astrophys, Pune Univ Campus, Pune 411007, Maharashtra, India

[30] Kumamoto Univ, Grad Sch Sci & Technol, Kumamoto 8608555, Japan

[31] Univ Cagliari, Dipartimento Fis, SP Monserrato Sestu Km 0,700, I-09042 Monserrato, cA, Italy

[32] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands

[33] Indian Inst Sci Educ & Res Kolkata, Dept Phys Sci, Mohanpur 741246, India

[34] Indian Inst Sci Educ & Res Kolkata, Ctr Excellence Space Sci India, Kolkata 741246, India

[35] Trinity Coll Dublin, Sch Phys, Dublin D02 PN40, Ireland

[36] Univ Manchester, Jodrell Bank Ctr Astrophys, Dept Phys & Astron, Manchester M13 9PL, Lancs, England

[37] St Xaviers Coll Autonomous, Dept Phys, Mumbai 400001, Maharashtra, India

[38] Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China

[39] Chinese Acad Sci, Natl Astron Observ, Beijing 100101, Peoples R China

[40] Univ Hull, EA Milne Ctr Astrophys, Cottingham Rd, Kingston Upon Hull HU6 7RX, N Humberside, England

[41] Univ Hull, Ctr Excellence Data Sci Artificial Intelligence &, Cottingham Rd, Kingston Upon Hull HU6 7RX, N Humberside, England

[42] Dept Phys, BITS Pilani Hyderabad Campus, Hyderabad 500078, Telangana, India

[43] Indian Inst Sci, Joint Astron Programme, Bengaluru 560012, Karnataka, India

[44] Arecibo Observ, HC3 Box 53995, Arecibo, PR 00612 USA

[45] Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France

[46] Raman Res Inst India, Bengaluru 560080, Karnataka, India

[47] Univ Potsdam, Inst Phys & Astron, Haus 28,Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany

[48] IISER Bhopal, Dept Phys, Bhopal Bypass Rd, Bhopal 462066, Madhya Pradesh, India

[49] Ollscoil Gaillimhe Univ Galway, Univ Rd, Galway H91 TK33, Ireland

[50] Univ Wisconsin Milwaukee, Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53211 USA

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 690卷

基金：

英国科学技术设施理事会; 欧洲研究理事会;

关键词：

gravitational waves; methods: data analysis; pulsars: general; SUPERMASSIVE BLACK-HOLE; LIMITS;

D O I：

10.1051/0004-6361/202348568

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the results of a search for continuous gravitational wave signals (CGWs) in the second data release (DR2) of the European Pulsar Timing Array (EPTA) Collaboration. The most significant candidate event from this search has a gravitational wave frequency of 4-5 nHz. Such a signal could be generated by a supermassive black hole binary (SMBHB) in the local Universe. We present the results of a follow-up analysis of this candidate using both Bayesian and frequentist methods. The Bayesian analysis gives a Bayes factor of 4 in favour of the presence of the CGW over a common uncorrelated noise process. In contrast, the frequentist analysis estimates the p-value of the candidate to be < 1%, also assuming the presence of common uncorrelated red noise. However, comparing a model that includes both a CGW and a gravitational wave background (GWB) to a GWB only, the Bayes factor in favour of the CGW model is only 0.7. Therefore, we cannot conclusively determine the origin of the observed feature, nor can we rule it out as a CGW source. We present results of simulations that demonstrate that data containing a weak gravitational wave background can be misinterpreted as data including a CGW and vice versa, providing two plausible explanations for the EPTA DR2 data. Further investigations combining data from all PTA collaborations will be needed to reveal the true origin of this feature.

引用

页数：14

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