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Wide-band profile domain pulsar timing analysis
Lentati, L.1; Kerr, M.2; Dai, S.2; Hobson, M. P.1; Shannon, R. M.2,3; Hobbs, G.2; Bailes, M.4; Bhat, N. D. Ramesh3; Burke-Spolaor, S.5; Coles, W.6; Dempsey, J.7; Lasky, P. D.8; Levin, Y.8; Manchester, R. N.2; Oslowski, S.9,10; Ravi, V.11; Reardon, D. J.8; Rosado, P. A.4; Spiewak, R.4,12; van Straten, W.4; Toomey, L.2; Wang, J.13; Wen, L.14; You, X.15; Zhu, X.14
2017-04-01
Source PublicationMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
ISSN0035-8711
Volume466Issue:3Pages:3706-3727
Contribution Rank13
Abstract

We extend profile domain pulsar timing to incorporate wide-band effects such as frequencydependent profile evolution and broad-band shape variation in the pulse profile. We also incorporate models for temporal variations in both pulse width and in the separation in phase of the main pulse and interpulse. We perform the analysis with both nested sampling and Hamiltonian Monte Carlo methods. In the latter case, we introduce a new parametrization of the posterior that is extremely efficient in the low signal-to-noise regime and can be readily applied to a wide range of scientific problems. We apply this methodology to a series of simulations, and to between seven and nine years of observations for PSRs J1713+0747,J1744-1134 and J1909-3744 with frequency coverage that spans 700-3600 Mhz. We use a smooth model for profile evolution across the full frequency range, and compare smooth and piecewise models for the temporal variations in dispersion measure (DM). We find that the profile domain framework consistently results in improved timing precision compared to the standard analysis paradigm by as much as 40 per cent for timing parameters. Incorporating smoothness in the DM variations into the model further improves timing precision by as much as 30 per cent. For PSR J1713+0747, we also detect pulse shape variation uncorrelated between epochs, which we attribute to variation intrinsic to the pulsar at a level consistent with previously published analyses. Not accounting for this shape variation biases the measured arrival times at the level of similar to 30 ns, the same order of magnitude as the expected shift due to gravitational waves in the pulsar timing band.

Correspondent Emailltl21@cam.ac.uk
KeywordMethods: Data Analysis Pulsars: General Pulsars: Individual
SubtypeArticle
DOI10.1093/mnras/stw3359
WOS HeadingsScience & Technology ; Physical Sciences
Indexed BySCI
Language英语
WOS Keyword37 Millisecond Pulsars ; Gravitational-waves ; Precision ; Dispersion ; Limits ; Scintillation ; Efficient ; Emission ; Arrival ; Physics
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000398418600088
Funding OrganizationCommonwealth of Australia for operation as a National Facility ; Junior Research Fellowship at Trinity Hall College, Cambridge University
Citation statistics
Cited Times:9[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.xao.ac.cn/handle/45760611-7/1465
Collection射电天文研究室_脉冲星研究团组
射电天文研究室
Corresponding AuthorLentati, L.
Affiliation1.Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England
2.CSIRO Astron & Space Sci, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia
3.Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia
4.Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia
5.Natl Radio Astron Observ, Array Operat Ctr, POB O, Soccoro, NM 87801 USA
6.Univ Calif San Diego, Dept Elect & Comp Engn, La Jolla, CA 92093 USA
7.CSIRO Informat Management & Technol, POB 225, Dickson, ACT 2602, Australia
8.Monash Univ, Sch Phys & Astron, Monash Ctr Astrophys, Clayton, Vic 3800, Australia
9.Univ Bielefeld, Fak Phys, Postfach 100131, D-33501 Bielefeld, Germany
10.Max Planck Inst Radio Astron, Hugel 69, D-53121 Bonn, Germany
11.CALTECH, Cahill Ctr Astron & Astrophys, MC 249-17, Pasadena, CA 91125 USA
12.Univ Wisconsin, Dept Phys, POB 413, Milwaukee, WI 53201 USA
13.Chinese Acad Sci, Xinjiang Astron Observ, 150 Sci 1 St, Xinjiang 830011, Peoples R China
14.Univ Western Australia, Sch Phys, Crawley, WA 6009, Australia
15.Southwest Univ, Sch Phys Sci & Technol, Chongqing 400715, Peoples R China
Recommended Citation
GB/T 7714
Lentati, L.,Kerr, M.,Dai, S.,et al. Wide-band profile domain pulsar timing analysis[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2017,466(3):3706-3727.
APA Lentati, L..,Kerr, M..,Dai, S..,Hobson, M. P..,Shannon, R. M..,...&Zhu, X..(2017).Wide-band profile domain pulsar timing analysis.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,466(3),3706-3727.
MLA Lentati, L.,et al."Wide-band profile domain pulsar timing analysis".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 466.3(2017):3706-3727.
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