From spin noise to systematics: stochastic processes in the first International Pulsar Timing Array data release

被引：95

作者：

Lentati, L. ^{[1
]}

Shannon, R. M. ^{[2
,3
]}

Coles, W. A. ^{[4
]}

Verbiest, J. P. W. ^{[5
,6
]}

van Haasteren, R. ^{[7
]}

Ellis, J. A. ^{[7
]}

Caballero, R. N. ^{[6
]}

Manchester, R. N. ^{[2
]}

Arzoumanian, Z. ^{[8
,9
]}

Babak, S. ^{[10
]}

Bassa, C. G. ^{[11
]}

Bhat, N. D. R. ^{[3
]}

Brem, P. ^{[10
]}

Burgay, M. ^{[12
]}

Burke-Spolaor, S. ^{[13
]}

Champion, D. ^{[6
]}

Chatterjee, S. ^{[14
]}

Cognard, I. ^{[15
,16
]}

Cordes, J. M. ^{[14
]}

Dai, S. ^{[2
,17
]}

Demorest, P. ^{[13
]}

Desvignes, G. ^{[6
]}

Dolch, T. ^{[14
,18
]}

Ferdman, R. D. ^{[19
]}

Fonseca, E. ^{[20
]}

Gair, J. R. ^{[21
]}

Gonzalez, M. E. ^{[22
]}

Graikou, E. ^{[6
]}

Guillemot, L. ^{[15
,16
]}

Hessels, J. W. T. ^{[13
,23
]}

Hobbs, G. ^{[2
]}

Janssen, G. H. ^{[11
]}

Jones, G. ^{[24
]}

Karuppusamy, R. ^{[6
]}

Keith, M. ^{[25
]}

Kerr, M. ^{[2
]}

Kramer, M. ^{[6
]}

Lam, M. T. ^{[14
]}

Lasky, P. D. ^{[26
]}

Lassus, A. ^{[6
]}

Lazarus, P. ^{[6
]}

Lazio, T. J. W. ^{[7
]}

Lee, K. J. ^{[27
]}

Levin, L. ^{[25
,28
]}

Liu, K. ^{[6
]}

Lynch, R. S. ^{[29
]}

Madison, D. R. ^{[30
]}

McKee, J. ^{[25
]}

McLaughlin, M. ^{[28
]}

McWilliams, S. T. ^{[28
]}

机构：

[1] Univ Cambridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England

[2] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Box 76, Epping, NSW 1710, Australia

[3] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia

[4] Univ Calif San Diego, ECE Dept, La Jolla, CA 92093 USA

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

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

[7] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

[8] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol USRA, Code 662, Greenbelt, MD 20771 USA

[9] NASA, Goddard Space Flight Ctr, X Ray Astrophys Lab, Code 662, Greenbelt, MD 20771 USA

[10] Albert Einstein Inst, MPI Gravitat Phys, D-14476 Golm, Germany

[11] ASTRON, Postbus 2, NL-7900 AA Dwingeloo, Netherlands

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

[13] Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA

[14] Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA

[15] Univ Orleans, CNRS, Lab Phys & Chim Environm & Espace LPC2E, F-45071 Orleans, France

[16] Observ Paris, CNRS, INSU, Stn Radioastron Nancay, F-18330 Nancay, France

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

[18] Hillsdale Coll, Dept Phys, 33 E Coll St, Hillsdale, MI 49242 USA

[19] McGill Univ, Dept Phys, Rutherford Phys Bldg,3600 Univ St, Montreal, PQ H3A 2T8, Canada

[20] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada

[21] Univ Edinburgh, Sch Math, Kings Bldg, Edinburgh EH9 3JZ, Midlothian, Scotland

[22] Vancouver Coastal Hlth, Dept Nucl Med, 899 W 12th Ave, Vancouver, BC V5Z 1M9, Canada

[23] Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

[24] Columbia Univ, Dept Phys, 538 W 120th St, New York, NY 10027 USA

[25] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England

[26] Monash Univ, Sch Phys & Astron, Monash Ctr Astrophys MoCA, Clayton, Vic 3800, Australia

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

[28] W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA

[29] Natl Radio Astron Observ, POB 2, Green Bank, WV 24944 USA

[30] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA

[31] CALTECH, TAPIR, MC 350-17, Pasadena, CA 91125 USA

[32] Lafayette Coll, Dept Phys, Easton, PA 18042 USA

[33] Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA

[34] Univ Paris Diderot Paris7, APC UFR Phys, Batiment Condorcet,10 Rue Alice Domont & Leonie D, F-75205 Paris 13, France

[35] Swinburne Univ Technol, Ctr Astrophys & Supercomputing, POB 218, Hawthorn, Vic 3122, Australia

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

[37] Univ Wisconsin, Dept Phys, Ctr Gravitat Cosmol & Astrophys, POB 413, Milwaukee, WI 53201 USA

[38] Oberlin Coll, Dept Phys & Astron, Oberlin, OH 44074 USA

[39] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA

[40] Univ Paris Diderot, CNRS, INSU, Lab Univ & Theories LUTh,Observ Paris, 5 Pl Jules Janssen, F-92190 Meudon, France

[41] Chinese Acad Sci, Xinjiang Astron Observ, 150 Sci 1 St, Urumqi 830011, Xinjiang, Peoples R China

[42] Huazhong Univ Sci & Technol, Sch Phys, Wuhan 430074, Hubei Province, Peoples R China

[43] Southwest Univ, Sch Phys Sci & Technol, Chongqing 400715, Peoples R China

[44] Univ Western Australia, Sch Phys, Crawley, WA 6009, Australia

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2016年 / 458卷 / 02期

基金：

加拿大自然科学与工程研究理事会; 澳大利亚研究理事会; 欧洲研究理事会; 美国国家科学基金会;

关键词：

methods: data analysis; pulsars: general; BLACK-HOLE BINARIES; FREQUENCY GRAVITATIONAL-RADIATION; MILLISECOND PULSAR; PRECISION; DISPERSION; LIMITS; WAVES; VARIABILITY; SCATTERING; SHAPELETS;

D O I：

10.1093/mnras/stw395

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We analyse the stochastic properties of the 49 pulsars that comprise the first International Pulsar Timing Array (IPTA) data release. We use Bayesian methodology, performing model selection to determine the optimal description of the stochastic signals present in each pulsar. In addition to spin-noise and dispersion-measure (DM) variations, these models can include timing noise unique to a single observing system, or frequency band. We show the improved radio-frequency coverage and presence of overlapping data from different observing systems in the IPTA data set enables us to separate both system and band-dependent effects with much greater efficacy than in the individual pulsar timing array (PTA) data sets. For example, we show that PSR J1643-1224 has, in addition to DM variations, significant band-dependent noise that is coherent between PTAs which we interpret as coming from time-variable scattering or refraction in the ionized interstellar medium. Failing to model these different contributions appropriately can dramatically alter the astrophysical interpretation of the stochastic signals observed in the residuals. In some cases, the spectral exponent of the spin-noise signal can vary from 1.6 to 4 depending upon the model, which has direct implications for the long-term sensitivity of the pulsar to a stochastic gravitational-wave (GW) background. By using a more appropriate model, however, we can greatly improve a pulsar's sensitivity to GWs. For example, including system and band-dependent signals in the PSR J0437-4715 data set improves the upper limit on a fiducial GW background by similar to 60 per cent compared to a model that includes DM variations and spin-noise only.

引用

页码：2161 / 2187

页数：27

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