Common-red-signal analysis with 24-yr high-precision timing of the European Pulsar Timing Array: inferences in the stochastic gravitational-wave background search

被引:244
作者
Chen, S. [1 ,2 ]
Caballero, R. N. [3 ]
Guo, Y. J. [4 ]
Chalumeau, A. [1 ,2 ,5 ]
Liu, K. [4 ]
Shaifullah, G. [6 ,7 ]
Lee, K. J. [3 ,7 ,8 ]
Babak, S. [5 ,9 ]
Desvignes, G. [4 ,10 ]
Parthasarathy, A. [4 ]
Hu, H. [4 ]
van der Wateren, E. [11 ,12 ]
Antoniadis, J. [4 ,13 ,14 ]
Nielsen, A-S Bak [4 ,15 ]
Bassa, C. G. [11 ]
Berthereau, A. [1 ,2 ]
Burgay, M. [16 ]
Champion, D. J. [4 ]
Cognard, I [1 ,2 ]
Falxa, M. [5 ]
Ferdman, R. D. [17 ]
Freire, P. C. C. [4 ]
Gair, J. R. [18 ]
Graikou, E. [4 ]
Guillemot, L. [1 ,2 ]
Jang, J. [4 ]
Janssen, G. H. [11 ,12 ]
Karuppusamy, R. [4 ]
Keith, M. J. [19 ]
Kramer, M. [4 ,19 ]
Liu, X. J. [19 ,20 ]
Lyne, A. G. [19 ]
Main, R. A. [4 ]
McKee, J. W. [21 ]
Mickaliger, M. B. [19 ]
Perera, B. B. P. [22 ]
Perrodin, D. [16 ]
Petiteau, A. [5 ]
Porayko, N. K. [4 ]
Possenti, A. [16 ,23 ]
Samajdar, A. [6 ]
Sanidas, S. A. [19 ]
Sesana, A. [6 ,7 ]
Speri, L. [18 ]
Stappers, B. W. [19 ]
Theureau, G. [1 ,2 ,24 ]
Tiburzi, C. [11 ]
Vecchio, A. [25 ,26 ]
Verbiest, J. P. W. [4 ,15 ]
Wang, J. [15 ]
机构
[1] Univ Orleans, Lab Phys & Chim Environm & Espace LPC2E, CNRS, UMR7328, F-45071 Orleans, France
[2] Univ Orleans, Stn Radioastron Nancay, Observ Paris, PSL Univ,CNRS, F-18330 Nancay, France
[3] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China
[4] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany
[5] Univ Paris, Astroparticule & Cosmol, CNRS, F-75013 Paris, France
[6] Univ Milano Bicocca, Dipartimento Fis G Occhialini, Piazza Sci 3, I-20126 Milan, Italy
[7] Ist Nazl Fis Nucl, Sez Milano Bicocca, Piazza Sci 3, I-20126 Milan, Italy
[8] Chinese Acad Sci, Natl Astron Observ, Beijing 100101, Peoples R China
[9] Moscow Inst Phys & Technol, Moscow 141700, Russia
[10] Univ Paris, Univ PSL, Sorbonne Univ, LESIA,Observ Paris,CNRS, 5 Pl Jules Janssen, F-92195 Meudon, France
[11] Netherlands Inst Radio Astron, ASTRON, Oude Hoogeveensedijk 4, NL-7991 PD Dwingeloo, Netherlands
[12] Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands
[13] FORTH, Inst Astrophys, N Plastira 100, Iraklion 70013, Greece
[14] Argelander Inst Astron, Hugel 71, D-53117 Bonn, Germany
[15] Univ Bielefeld, Fak Phys, Postfach 100131, D-33501 Bielefeld, Germany
[16] INAF Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy
[17] Univ East Anglia, Fac Sci, Sch Phys, Norwich NR4 7TJ, Norfolk, England
[18] Max Planck Inst Gravitat Phys, Albert Einstein Inst, Muhlenberg 1, D-14476 Golm, Germany
[19] Univ Manchester, Jodrell Bank Ctr Astrophys, Dept Phys & Astron, Manchester M13 9PL, Lancs, England
[20] Beijing Normal Univ Zhuhai, Adv Inst Nat Sci, Lab Gravitat Waves & Cosmol, Zhuhai 519087, Peoples R China
[21] Univ Toronto, Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada
[22] Arecibo Observ, HC3 Box 53995, Arecibo, PR 00612 USA
[23] Univ Cagliari, Dipartimento Fis, SP Monserrato Sestu Km 0, I-09042 Monserrato, CA, Italy
[24] Univ Paris, Univ PST, Observ Paris, Lab Univers & Theories LUTh,CNRS, F-92190 Meudon, France
[25] Univ Birmingham, Inst Gravitat Wave Astron, Birmingham B15 2TT, W Midlands, England
[26] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England
[27] Peking Univ, Dept Astron, Beijing 100871, Peoples R China
基金
英国科学技术设施理事会; 加拿大自然科学与工程研究理事会; 欧洲研究理事会;
关键词
gravitational waves; methods: data analysis; pulsars: general; BLACK-HOLE BINARIES; YR DATA SET; SOLAR-SYSTEM; MILLISECOND PULSAR; GENERAL-RELATIVITY; SPIN NOISE; LIMITS; RADIATION; TIME; DISPERSION;
D O I
10.1093/mnras/stab2833
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present results from the search for a stochastic gravitational-wave background (GWB) as predicted by the theory of General Relativity using six radio millisecond pulsars from the Data Release 2 (DR2) of the European Pulsar Timing Array (EPTA) covering a timespan up to 24 yr. A GWB manifests itself as a long-term low-frequency stochastic signal common to all pulsars, a common red signal (CRS), with the characteristic Hellings-Downs (HD) spatial correlation. Our analysis is performed with two independent pipelines, ENTERPRISE, and TEMPONEST+FORTYTWO, which produce consistent results. A search for a CRS with simultaneous estimation of its spatial correlations yields spectral properties compatible with theoretical GWB predictions, but does not result in the required measurement of the HD correlation, as required for GWB detection. Further Bayesian model comparison between different types of CRSs, including a GWB, finds the most favoured model to be the common uncorrelated red noise described by a power law with A = 5.13(-2.73)(+4.20) x 10(-15) and. = 3.78 (+0.69)(-0.59) (95 per cent credible regions). Fixing the spectral index to gamma = 13/3 as expected from the GWB by circular, inspiralling supermassive black hole binaries results in an amplitude of A = 2.95(-0.72)(+0.89) x 10(-15). We implement three different models, BAYESEPHEM, LINIMOSS, and EPHEMGP, to address possible Solar system ephemeris (SSE) systematics and conclude that our results may only marginally depend on these effects. This work builds on the methods and models from the studies on the EPTA DR1. We show that under the same analysis framework the results remain consistent after the data set extension.
引用
收藏
页码:4970 / 4993
页数:24
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