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The emission and scintillation properties of RRAT J2325−0530 at 154 MHz and 1.4 GHz

  • B. W. Meyers (a1) (a2), S. E. Tremblay (a1), N. D. R. Bhat (a1), R. M. Shannon (a3) (a4), S. M. Ord (a2), C. Sobey (a5), M. Johnston-Hollitt (a1), M. Walker (a6) and R. B. Wayth (a1)...

Abstract

Rotating Radio Transients (RRATs) represent a relatively new class of pulsar, primarily characterised by their sporadic bursting emission of single pulses on time scales of minutes to hours. In addition to the difficulty involved in detecting these objects, low-frequency ( $ \lt 300\,\text{MHz}$ ) observations of RRATs are sparse, which makes understanding their broadband emission properties in the context of the normal pulsar population problematic. Here, we present the simultaneous detection of RRAT J2325−0530 using the Murchison Widefield Array (154 MHz) and Parkes radio telescope ( $1.4\,\text{GHz}$ ). On a single-pulse basis, we produce the first polarimetric profile of this pulsar, measure the spectral index ( $\alpha={-2.2\pm 0.1}$ ), pulse energy distributions, and present the pulse rates in the context of detections in previous epochs. We find that the distribution of time between subsequent pulses is consistent with a Poisson process and find no evidence of clustering over the $\sim\!1.5\,\text{h}$ observations. Finally, we are able to quantify the scintillation properties of RRAT J2325−0530 at 1.4 GHz, where the single pulses are modulated substantially across the observing bandwidth, and show that this characterisation is feasible even with irregular time sampling as a consequence of the sporadic emission behaviour.

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Corresponding author

Author for correspondence: Bradley W. Meyers, E-mail: bradley.meyers@postgrad.curtin.edu.au

References

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Keywords

The emission and scintillation properties of RRAT J2325−0530 at 154 MHz and 1.4 GHz

  • B. W. Meyers (a1) (a2), S. E. Tremblay (a1), N. D. R. Bhat (a1), R. M. Shannon (a3) (a4), S. M. Ord (a2), C. Sobey (a5), M. Johnston-Hollitt (a1), M. Walker (a6) and R. B. Wayth (a1)...

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