Giant pulses from J1823−3021A observed with the MeerKAT telescope. Issue 1 (19th August 2020)

• Record Type: Journal Article
• Authors: Abbate, F; Bailes, M; Buchner, S J; Camilo, F; Freire, P C C; Geyer, M; Jameson, A; Kramer, M; Possenti, A; Ridolfi, A; Serylak, M; Spiewak, R; Stappers, B W; Venkatraman Krishnan, V
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 498:Issue 1(2020)
• Page Start: 875
• Page End: 882
• Publication Date: 2020-08-19
• Subjects: pulsars: individual: J1823−3021A; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa2510
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: The millisecond pulsar J1823−3021A is a very active giant pulse emitter in the globular cluster NGC 6624. New observations with the MeerKAT radio telescope have revealed 14350 giant pulses over 5 h of integration time, with an average wait time of about 1 s between giant pulses. The giant pulses occur in phases compatible with the ordinary radio emission, follow a power-law distribution with an index of −2.63 ± 0.02, and contribute 4 per cent of the total integrated flux. The spectral index of the giant pulses follows a Gaussian distribution centred around −1.9 with a standard deviation of 0.6 and is on average flatter than the integrated emission, which has a spectral index of −2.81 ± 0.02. The waiting times between the GPs are accurately described by a Poissonian distribution, suggesting that the time of occurrence of a GP is independent from the times of occurrence of other GPs. 76 GPs show multiple peaks within the same rotation, a rate that is also compatible with the mutual independence of the GP times of occurrence. We studied the polarization properties of the giant pulses finding, on average, linear polarization only at the 1 per cent level and circular polarization at the 3 per cent level, similar to the polarization percentages of the total integrated emission. In four cases, it was possible to measure the RM of the GPs that are highly variable and, in two cases, is inconsistent with the mean RM of the total integrated pulsar signal.