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

Desvignes, G. and Mingarelli, C. M. F. (2016) High-precision timing of 42 millisecond pulsars with the European Pulsar Timing Array. Monthly Notices of the Royal Astronomical Society, 458 (3). pp. 3341-3380. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20160603-093637424

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Abstract

We report on the high-precision timing of 42 radio millisecond 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 binary MSPs 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^(+0.5)_(−0.35) M_⊙, m_c=0.21^(+0.06)_(−0.04) M_⊙ and m_p=1.25^(+0.6)_(−0.4) M_⊙, m_c=0.23^(+0.07)_(−0.05) M_⊙, 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.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1093/mnras/stw483DOIArticle
http://mnras.oxfordjournals.org/content/458/3/3341.abstractPublisherArticle
http://arxiv.org/abs/1602.08511arXivDiscussion Paper
Additional Information:© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2016 February 26. Received 2016 February 26. In original form 2015 September 2. First published online March 2, 2016. The authors would like to thank D. Schnitzeler for providing us with the M2 and M3 distances used in this work, P. Freire, M. Bailes, T. Tauris and N. Wex for useful discussions, P. Demorest for his contribution to the pulsar instrumentation at the NRT. Part of this work is based on observations with the 100-m telescope of the Max-Planck-Institut für Radioastronomie (MPIfR) at Effelsberg in Germany. Pulsar research at the Jodrell Bank Centre for Astrophysics and the observations using the Lovell Telescope are supported by a consolidated grant from the STFC in the UK. The Nançay radio observatory is operated by the Paris Observatory, associated with the French Centre National de la Recherche Scientifique (CNRS). We acknowledge financial support from ‘Programme National de Cosmologie et Galaxies’ (PNCG) of CNRS/INSU, France. The WSRT is operated by the Netherlands Institute for Radio Astronomy (ASTRON) with support from the Netherlands Foundation for Scientific Research (NWO). CGB, GHJ, RK, KL, KJL, DP acknowledge the support from the ‘LEAP’ ERC Advanced Grant (337062). RNC acknowledges the support of the International Max Planck Research School Bonn/Cologne and the Bonn-Cologne Graduate School. JG and AS are supported by the Royal Society. JWTH acknowledges funding from an NWO Vidi fellowship and CGB, JWTH acknowledge the support from the ERC Starting Grant ‘DRAGNET’ (337062). KJL is supported by the National Natural Science Foundation of China (Grant No.11373011). PL acknowledges the support of the International Max Planck Research School Bonn/Cologne. CMFM was supported by a Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme. SO is supported by the Alexander von Humboldt Foundation. This research was in part supported by ST's appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. RvH is supported by NASA Einstein Fellowship grant PF3-140116. The authors acknowledge the use of the HYDRA and HERCULES computing cluster from Rechenzentrum Garching. This research has made extensive use of NASA's Astrophysics Data System, the ATNF Pulsar Catalogue and the PYTHON Uncertainties package, http://pythonhosted.org/uncertainties/.
Funders:
Funding AgencyGrant Number
Science and Technology Facilities Council (STFC)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)UNSPECIFIED
European Research Council (ERC)337062
International Max Planck Research School (IMPRS) for Astronomy and AstrophysicsUNSPECIFIED
Bonn-Cologne Graduate School of Physics and AstronomyUNSPECIFIED
Royal SocietyUNSPECIFIED
National Natural Science Foundation of China11373011
Marie Curie FellowshipUNSPECIFIED
Alexander von Humboldt FoundationUNSPECIFIED
Institut national des sciences de l'Univers (INSU)UNSPECIFIED
NASA Einstein FellowshipPF3-140116
NASA Postdoctoral ProgramUNSPECIFIED
Subject Keywords:proper motions stars: distances pulsars: general
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory2016-30
Issue or Number:3
Record Number:CaltechAUTHORS:20160603-093637424
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20160603-093637424
Official Citation:G. Desvignes, R. N. Caballero, L. Lentati, J. P. W. Verbiest, D. J. Champion, B. W. Stappers, G. H. Janssen, P. Lazarus, S. Osłowski, S. Babak, C. G. Bassa, P. Brem, M. Burgay, I. Cognard, J. R. Gair, E. Graikou, L. Guillemot, J. W. T. Hessels, A. Jessner, C. Jordan, R. Karuppusamy, M. Kramer, A. Lassus, K. Lazaridis, K. J. Lee, K. Liu, A. G. Lyne, J. McKee, C. M. F. Mingarelli, D. Perrodin, A. Petiteau, A. Possenti, M. B. Purver, P. A. Rosado, S. Sanidas, A. Sesana, G. Shaifullah, R. Smits, S. R. Taylor, G. Theureau, C. Tiburzi, R. van Haasteren, and A. Vecchio High-precision timing of 42 millisecond pulsars with the European Pulsar Timing Array MNRAS (May 21, 2016) Vol. 458 3341-3380 doi:10.1093/mnras/stw483 first published online March 2, 2016
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:67646
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:03 Jun 2016 17:38
Last Modified:03 Oct 2019 10:07

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