The low-frequency characteristics of PSR J0437–4715 observed with the Murchison Wide-Field Array

Bhat, N. D. R. ; Ord, S. M. ; Tremblay, S. E. ; Tingay, S. J. ; Deshpande, A. A. ; van Straten, W. ; Oronsaye, S. ; Bernardi, G. ; Bowman, J. D. ; Briggs, F. ; Cappallo, R. J. ; Corey, B. E. ; Emrich, D. ; Goeke, R. ; Greenhill, L. J. ; Hazelton, B. J. ; Hewitt, J. N. ; Johnston-Hollitt, M. ; Kaplan, D. L. ; Kasper, J. C. ; Kratzenberg, E. ; Lonsdale, C. J. ; Lynch, M. J. ; McWhirter, S. R. ; Mitchell, D. A. ; Morales, M. F. ; Morgan, E. ; Oberoi, D. ; Prabu, T. ; Rogers, A. E. E. ; Roshi, D. A. ; Udaya Shankar, N. ; Srivani, K. S. ; Subrahmanyan, R. ; Waterson, M. ; Wayth, R. B. ; Webster, R. L. ; Whitney, A. R. ; Williams, A. ; Williams, C. L. (2014) The low-frequency characteristics of PSR J0437–4715 observed with the Murchison Wide-Field Array The Astrophysical Journal, 791 (2). Article ID L32-6 pages. ISSN 0004-637X

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We report on the detection of the millisecond pulsar PSR J0437–4715 with the Murchison Wide-field Array (MWA) at a frequency of 192 MHz. Our observations show rapid modulations of pulse intensity in time and frequency that arise from diffractive scintillation effects in the Interstellar Medium (ISM), as well as prominent drifts of intensity maxima in the time-frequency plane that arise from refractive effects. Our analysis suggests that the scattering screen is located at a distance of ∼80-120 pc from the Sun, in disagreement with a recent claim that the screen is closer (∼10 pc). Comparisons with higher frequency data from Parkes reveal a dramatic evolution of the pulse profile with frequency, with the outer conal emission becoming comparable in strength to that from the core and inner conal regions. As well as demonstrating the high time resolution science capabilities currently possible with the MWA, our observations underscore the potential to conduct low-frequency investigations of timing-array millisecond pulsars, which may lead to increased sensitivity in the detection of nanoHertz gravitational waves via the accurate characterization of ISM effects.

Item Type:Article
Source:Copyright of this article belongs to American Astronomical Society.
Keywords:Instrumentation: Interferometers; Methods: Observational; Pulsars: General; Pulsars: Individual (PSR J0437-4715)
ID Code:114351
Deposited On:21 May 2018 06:20
Last Modified:21 May 2018 06:20

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