The thousand-pulsar-array programme on MeerKAT VII: polarisation properties of pulsars in the Magellanic Clouds

Author:

Johnston S1ORCID,Parthasarathy A2ORCID,Main R A2,Ridley J P3,Koribalski B S1ORCID,Bailes M45,Buchner S J6ORCID,Geyer M6ORCID,Karastergiou A78,Keith M J9,Kramer M2ORCID,Serylak M1011,Shannon R M45ORCID,Spiewak R945,Krishnan V Venkatraman2

Affiliation:

1. Australia Telescope National Facility, CSIRO Space and Astronomy, PO Box 76, Epping NSW 1710, Australia

2. Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany

3. School of Engineering, Murray State University, Murray, KY 42071, USA

4. Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia

5. ARC Centre of Excellence for Gravitational Wave Discovery (OzGrav)

6. South African Radio Astronomy Observatory (SARAO), 2 Fir Street, Black River Park, Observatory, Cape Town 7925, South Africa

7. Department of Astrophysics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK

8. Department of Physics and Electronics, Rhodes University, PO Box 94, Grahamstown 6140, South Africa

9. Department of Physics and Astronomy, Jodrell Bank Centre for Astrophysics, University of Manchester, Manchester M13 9PL, UK

10. SKA Observatory, Jodrell Bank, Lower Withington, Macclesfield, SK11 9FT, United Kingdom

11. Department of Physics and Astronomy, University of the Western Cape, Bellville, Cape Town 7535, South Africa

Abstract

ABSTRACT The Magellanic Clouds are the only external galaxies known to host radio pulsars. The dispersion and rotation measures of pulsars in the Clouds can aid in understanding their structure, and studies of the pulsars themselves can point to potential differences between them and their Galactic counterparts. We use the high sensitivity of the MeerKAT telescope to observe 17 pulsars in the Small and Large Magellanic Clouds in addition to five foreground (Galactic) pulsars. We provide polarisation profiles for 18 of these pulsars, improved measurements of their dispersion and rotation measures, and derive the mean parallel magnetic field along the lines of sight. The results are broadly in agreement with expectations for the structure and strength of the magnetic field in the Large and Small Magellanic Clouds. The Magellanic Cloud pulsars have profiles which are narrower than expected from the period-width relationship and we show this is due to selection effects in pulsar surveys rather than any intrinsic difference between the population of Galactic and Magellanic objects.

Funder

Department of Science and Innovation

Swinburne University of Technology

AAL

RMS

Australian Research Council

Max Planck Society

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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