Measuring Interstellar Delays of PSR J0613-0200 over 7 years, using the Large European Array for Pulsars
Autor: | M. Gaikwad, Kejia Lee, S. Sanidas, C. G. Bassa, Siyuan Chen, John Antoniadis, Mitchell B. Mickaliger, Gemma H. Janssen, Weiwei Zhu, Benjamin Stappers, Long Wang, H. Hu, G. Mall, Delphine Perrodin, Olaf Wucknitz, Michael Kramer, Caterina Tiburzi, Ramesh Karuppusamy, Ismaël Cognard, R. A. Main, J. W. McKee, Kang Liu |
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Přispěvatelé: | Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), ITA, GBR, FRA, DEU, CAN, GRC, NLD, CHN |
Rok vydání: | 2020 |
Předmět: |
Astronomy
Astrophysics::High Energy Astrophysical Phenomena FOS: Physical sciences Astrophysics 01 natural sciences law.invention Telescope pulsars: individual: PSR J0613−0200 Pulsar Millisecond pulsar law pulsars: general 0103 physical sciences 010303 astronomy & astrophysics Physics High Energy Astrophysical Phenomena (astro-ph.HE) Scintillation 010308 nuclear & particles physics Scattering Gravitational wave Spectral density Astronomy and Astrophysics Pulse (physics) Space and Planetary Science [SDU]Sciences of the Universe [physics] [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] Astrophysics - High Energy Astrophysical Phenomena |
Zdroj: | Monthly Notices of the Royal Astronomical Society Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P-Oxford Open Option A, 2020, 499 (1), pp.1468-1479. ⟨10.1093/mnras/staa2955⟩ Monthly Notices of the Royal Astronomical Society, 499, 1, pp. 1468-1479 Monthly Notices of the Royal Astronomical Society, 499, 1468-1479 |
ISSN: | 0035-8711 1365-2966 |
DOI: | 10.48550/arxiv.2009.10707 |
Popis: | Using data from the Large European Array for Pulsars (LEAP), and the Effelsberg telescope, we study the scintillation parameters of the millisecond pulsar J0613-0200 over a 7 year timespan. The "secondary spectrum" -- the 2D power spectrum of scintillation -- presents the scattered power as a function of time delay, and contains the relative velocities of the pulsar, observer, and scattering material. We detect a persistent parabolic scintillation arc, suggesting scattering is dominated by a thin, anisotropic region. The scattering is poorly described by a simple exponential tail, with excess power at high delays; we measure significant, detectable scattered power at times out to $\sim 5 \mu s$, and measure the bulk scattering delay to be between 50 to 200\,ns with particularly strong scattering throughout 2013. These delays are too small to detect a change of the pulse profile shape, yet they would change the times-of-arrival as measured through pulsar timing. The arc curvature varies annually, and is well fit by a one-dimensional scattering screen $\sim 40\%$ of the way towards the pulsar, with a changing orientation during the increased scattering in 2013. Effects of uncorrected scattering will introduce time delays correlated over time in individual pulsars, and may need to be considered in gravitational wave analyses. Pulsar timing programs would benefit from simultaneously recording in a way that scintillation can be resolved, in order to monitor the variable time delays caused by multipath propagation. Comment: 12 pages, 10 figures. Published in MNRAS |
Databáze: | OpenAIRE |
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