High-precision timing of 42 millisecond pulsars with the European Pulsar Timing Array

被引：369

作者：

Desvignes, G. ^{[1
]}

Caballero, R. N. ^{[1
]}

Lentati, L. ^{[2
]}

Verbiest, J. P. W. ^{[1
,3
]}

Champion, D. J. ^{[1
]}

Stappers, B. W. ^{[4
]}

Janssen, G. H. ^{[4
,5
]}

Lazarus, P. ^{[1
]}

Oslowski, S. ^{[1
,3
]}

Babak, S. ^{[6
]}

Bassa, C. G. ^{[4
,5
]}

Brem, P. ^{[6
]}

Burgay, M. ^{[7
]}

Cognard, I. ^{[8
,9
]}

Gair, J. R. ^{[10
]}

Graikou, E. ^{[1
]}

Guillemot, L. ^{[8
,9
]}

Hessels, J. W. T. ^{[5
,11
]}

Jessner, A. ^{[1
]}

Jordan, C. ^{[4
]}

Karuppusamy, R. ^{[1
]}

Kramer, M. ^{[1
,4
]}

Lassus, A. ^{[1
]}

Lazaridis, K. ^{[1
]}

Lee, K. J. ^{[1
,12
]}

Liu, K. ^{[1
]}

Lyne, A. G. ^{[4
]}

McKee, J. ^{[4
]}

Mingarelli, C. M. F. ^{[1
,13
,14
]}

Perrodin, D. ^{[7
]}

Petiteau, A. ^{[15
]}

Possenti, A. ^{[7
]}

Purver, M. B. ^{[4
]}

Rosado, P. A. ^{[16
,17
]}

Sanidas, S. ^{[4
]}

Sesana, A. ^{[6
,14
]}

Shaifullah, G. ^{[1
]}

Smits, R. ^{[5
]}

Taylor, S. R. ^{[10
,18
]}

Theureau, G. ^{[8
,9
,19
]}

Tiburzi, C. ^{[1
]}

van Haasteren, R. ^{[13
]}

Vecchio, A. ^{[14
]}

机构：

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

[2] Univ Cambridge, Inst Astron, Battcock Ctr Astrophys, Madingley Rd, Cambridge CB3 0HA, England

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

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

[5] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands

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

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

[8] Univ Orleans, LPC2E, CNRS, F-45071 Orleans, France

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

[10] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

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

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

[13] CALTECH, TAPIR Theoret Astrophys, Pasadena, CA 91125 USA

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

[15] Univ Paris 07, APC, UFR Phys, Batiment Condorcet, F-75205 Paris 13, France

[16] Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia

[17] Albert Einstein Inst, Max Planck Inst Gravitat Phys, Callinstr 38, D-30167 Hannover, Germany

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

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

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2016年 / 458卷 / 03期

基金：

中国国家自然科学基金; 欧洲研究理事会;

关键词：

proper motions; stars: distances; pulsars: general; LARGE-AREA TELESCOPE; RELATIVISTIC CELESTIAL MECHANICS; ORBIT BINARY PULSARS; SHAPIRO DELAY; PROPER MOTION; NEUTRON-STAR; TRIGONOMETRIC PARALLAXES; GALACTIC DISTRIBUTION; GENERAL-RELATIVITY; PSR J1713+0747;

D O I：

10.1093/mnras/stw483

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on the high-precision timing of 42 radiomillisecond pulsars (MSPs) observed by the European Pulsar Timing Array (EPTA). This EPTA Data Release 1.0 extends up to mid-2014 and baselines range from 7-18 yr. It forms the basis for the stochastic gravitational-wave background, anisotropic background, and continuous-wave limits recently presented by the EPTA elsewhere. The Bayesian timing analysis performed with TEMPONEST yields the detection of several new parameters: seven parallaxes, nine proper motions and, in the case of six binary pulsars, an apparent change of the semimajor axis. We find the NE2001 Galactic electron density model to be a better match to our parallax distances (after correction from the Lutz-Kelker bias) than the M2 and M3 models by Schnitzeler. However, we measure an average uncertainty of 80 per cent (fractional) for NE2001, three times larger than what is typically assumed in the literature. We revisit the transverse velocity distribution for a set of 19 isolated and 57 binaryMSPs and find no statistical difference between these two populations. We detect Shapiro delay in the timing residuals of PSRs J1600-3053 and J1918-0642, implying pulsar and companion masses m(p) = 1.22(-0.35)(+0.5) M-circle dot, m(c) = 0.21(-0.04)(+0.06) M-circle dot and m(p) = 1.25(-0.4)(+0.6)M(circle dot), m(c) = 0.23(-0.05)(+0.07) M-circle dot, respectively. Finally, we use the measurement of the orbital period derivative to set a stringent constraint on the distance to PSRs J1012+5307 and J1909-3744, and set limits on the longitude of ascending node through the search of the annual-orbital parallax for PSRs J1600-3053 and J1909-3744.

引用

页码：3341 / 3380

页数：40

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