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Time-domain and spectral properties of pulsars at 154 MHz

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Authors
Bell, M.
Murphy, T.
Johnston, S.
Kaplan, D.
Croft, S.
Hancock, P.
Callingham, J.
Zic, A.
Dobie, D.
Swiggum, J.
Rowlinson, A.
Hurley-Walker, N.
Offringa, A.
Bernardi, G.
Bowman, J.
Briggs, F.
Cappallo, R.
Deshpande, A.
Gaensler, B.
Greenhill, L.
Hazelton, B.
Johnston-Hollitt, M.
Lonsdale, C.
McWhirter, S.
Mitchell, D.
Morales, M.
Morgan, E.
Oberoi, D.
Ord, S.
Prabu, T.
Udaya Shankar, N.
Srivani, K.
Subrahmanyan, R.
Tingay, Steven
Wayth, Randall
Webster, R.
Williams, A.
Williams, C.
Date
2016
Type
Journal Article

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Citation
Bell, M. and Murphy, T. and Johnston, S. and Kaplan, D. and Croft, S. and Hancock, P. and Callingham, J. et al. 2016. Time-domain and spectral properties of pulsars at 154 MHz. Monthly Notices of the Royal Astronomical Society. 461 (1): pp. 908-921.
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Monthly Notices of the Royal Astronomical Society
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Curtin Institute of Radio Astronomy (Physics)
Remarks

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

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Abstract

We present 154 MHz Murchison Widefield Array imaging observations and variability information for a sample of pulsars. Over the declination range −80° < δ < 10°, we detect 17 known pulsars with mean flux density greater than 0.3 Jy. We explore the variability properties of this sample on time-scales of minutes to years. For three of these pulsars, PSR J0953+0755, PSR J0437−4715, and PSR J0630−2834, we observe interstellar scintillation and variability on time-scales of greater than 2 min. One further pulsar, PSR J0034−0721, showed significant variability, the physical origins of which are difficult to determine. The dynamic spectra for PSR J0953+0755 and PSR J0437−4715 show discrete time and frequency structure consistent with diffractive interstellar scintillation and we present the scintillation bandwidth and time-scales from these observations. The remaining pulsars within our sample were statistically non-variable. We also explore the spectral properties of this sample and find spectral curvature in pulsars PSR J0835−4510, PSR J1752−2806, and PSR J0437−4715.