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Detection of a Glitch in the Pulsar J1709−4429

Lower, Marcus E. and Flynn, Chris and Bailes, Matthew and Barr, Ewan D. and Bateman, Timothy and Bhandari, Shivani and Caleb, Manisha and Campbell-Wilson, Duncan and Day, Cherie and Deller, Adam and Farah, Wael and Green, Anne J. and Gupta, Vivek and Hunstead, Richard W. and Jameson, Andrew and Jankowski, Fabian and Keane, Evan F. and Venkatraman Krishnan, Vivek and Osłowski, Stefan and Parthasarathy, Aditya and Plant, Kathryn and Price, Danny C. and Ravi, Vikram and Shannon, Ryan M. and Temby, David and Torr, Glen and Urquhart, Glenn (2018) Detection of a Glitch in the Pulsar J1709−4429. Research Notes of the AAS, 2 (3). Art. No. 139. ISSN 2515-5172. doi:10.3847/2515-5172/aad7bc.

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Pulsar glitches are thought to result from either quakes in the neutron star crust (Baym et al. 1969), or by a transfer of angular momentum between the superfluid interior and the outer crust (Anderson & Itoh 1975). The event manifests as a sudden increase in the observed spin period and spin-down of the pulsar, which can be followed by a recovery phase where the period exponentially returns to its pre-glitch evolution. We report here the detection of a glitch event in the pulsar J1709−4429 (also known as B1706−44) during regular monitoring observations with the Molonglo Observatory Synthesis Telescope (MOST). MOST is an aperture synthesis radio telescope located 40 km East of Canberra, Australia, operating in the 820–850 MHz frequency range. The UTMOST backend upgrade to the MOST (Bailes et al. 2017) has enabled study of the dynamic radio sky on millisecond timescales, and is well suited to pulsar timing, pulsar searches, observing single pulses from pulsars and discoveries of Fast Radio Bursts (FRBs) (Caleb et al. 2017; Farah et al. 2018). The glitch was found during timing operations, in which we regularly observe over 400 pulsars with up to daily cadence, while commensally searching for Rotating Radio Transients, pulsars, and FRBs.

Item Type:Article
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URLURL TypeDescription Paper
Lower, Marcus E.0000-0001-9208-0009
Bailes, Matthew0000-0003-3294-3081
Caleb, Manisha0000-0002-4079-4648
Deller, Adam0000-0001-9434-3837
Farah, Wael0000-0002-0161-7243
Hunstead, Richard W.0000-0002-3205-8288
Jankowski, Fabian0000-0002-6658-2811
Keane, Evan F.0000-0002-4553-655X
Venkatraman Krishnan, Vivek0000-0001-9518-9819
Parthasarathy, Aditya0000-0002-4140-5616
Plant, Kathryn0000-0001-6360-6972
Price, Danny C.0000-0003-2783-1608
Ravi, Vikram0000-0002-7252-5485
Additional Information:© 2018 The American Astronomical Society. Received 2018 August 2; Accepted 2018 August 2; Published 2018 August 7. The Molonglo Observatory is owned and operated by the University of Sydney. Major support for the UTMOST project has been provided by Swinburne University of Technology. We acknowledge the Australian Research Council grants CE110001020 (CAASTRO) and the Laureate Fellowship FL150100148. This work made use of the gSTAR and OzStar national HPC facilities.
Funding AgencyGrant Number
Swinburne University of TechnologyUNSPECIFIED
Australian Research CouncilCE110001020
Australian Research CouncilFL150100148
Subject Keywords:pulsars: individual (J1709−4429) ; stars: neutron
Issue or Number:3
Record Number:CaltechAUTHORS:20180809-084642931
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Official Citation:Marcus E. Lower et al 2018 Res. Notes AAS 2 139
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:88681
Deposited By: Tony Diaz
Deposited On:09 Aug 2018 15:58
Last Modified:16 Nov 2021 00:28

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