TY - JOUR

T1 - Radio pulsations from the γ-ray millisecond pulsar PSR J2039-5617

AU - Corongiu, A.

AU - Mignani, R. P.

AU - Seyffert, A. S.

AU - Clark, C. J.

AU - Venter, C.

AU - Nieder, L.

AU - Possenti, A.

AU - Burgay, M.

AU - Belfiore, A.

AU - De Luca, A.

AU - Ridolfi, A.

AU - Wadiasingh, Z.

N1 - Funding Information: We credit the contributions of A. Harding and T. Johnson on the analysis of the pulsar radio and ?-ray light curves, which paved the way to the modelling reported in this paper. The Parkes radio telescope is part of the Australia Telescope National Facility that is funded by the Australian Government for operation as a National Facility managed by CSIRO. We acknowledge the use of public data from the Swift data archive. This work is based on the research supported wholly/in part by the National Research Foundation of South Africa (NRF; Grant Numbers 87613, 90822, 92860, 93278, and 99072). The Grantholder acknowledges that opinions, findings and conclusions or recommendations expressed in any publication generated by the NRF supported research is that of the author(s), and that the NRF accepts no liability whatsoever in this regard. The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat `a l'Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucl?aire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. This work performed in part under DOE Contract DE- AC02-76SF00515. CJC acknowledges support from the ERC under the European Union's Horizon 2020 research and innovation programme (grant agreement no. 715051; Spiders). AR gratefully acknowledges financial support by the research grant 'iPeska' (P.I. Andrea Possenti) funded under the INAF national call Prin-SKA/CTAapprovedwith the Presidential Decree 70/2016.

PY - 2021/3

Y1 - 2021/3

N2 - The predicted nature of the candidate redback pulsar 3FGL J2039.6-5618 was recently confirmed by the discovery of gamma-ray millisecond pulsations (Clark et al., hereafter Paper I), which identify this gamma-ray source as PSR J2039-5617. We observed this object with the Parkes radio telescope in 2016 and 2019. We detect radio pulsations at 1.4 and 3.1 GHz, at the 2.6 ms period discovered in gamma-rays, and also at 0.7 GHz in one 2015 archival observation. In all bands, the radio pulse profile is characterized by a single relatively broad peak which leads the main gamma-ray peak. At 1.4 GHz, we found clear evidence of eclipses of the radio signal for about half of the orbit, a characteristic phenomenon in redback systems, which we associate with the presence of intra-binary gas. From the dispersion measure of 24.57 +/- 0.03 pc cm(-3), we derive a pulsar distance of 0.9 +/- 0.2 or 1.7 +/- 0.7 kpc, depending on the assumed Galactic electron density model. The modelling of the radio and gamma-ray light curves leads to an independent determination of the orbital inclination, and to a determination of the pulsar mass, qualitatively consistent to the results in Paper I.

AB - The predicted nature of the candidate redback pulsar 3FGL J2039.6-5618 was recently confirmed by the discovery of gamma-ray millisecond pulsations (Clark et al., hereafter Paper I), which identify this gamma-ray source as PSR J2039-5617. We observed this object with the Parkes radio telescope in 2016 and 2019. We detect radio pulsations at 1.4 and 3.1 GHz, at the 2.6 ms period discovered in gamma-rays, and also at 0.7 GHz in one 2015 archival observation. In all bands, the radio pulse profile is characterized by a single relatively broad peak which leads the main gamma-ray peak. At 1.4 GHz, we found clear evidence of eclipses of the radio signal for about half of the orbit, a characteristic phenomenon in redback systems, which we associate with the presence of intra-binary gas. From the dispersion measure of 24.57 +/- 0.03 pc cm(-3), we derive a pulsar distance of 0.9 +/- 0.2 or 1.7 +/- 0.7 kpc, depending on the assumed Galactic electron density model. The modelling of the radio and gamma-ray light curves leads to an independent determination of the orbital inclination, and to a determination of the pulsar mass, qualitatively consistent to the results in Paper I.

KW - Pulsars: general

KW - Pulsars: individual: (J2039-5617)

UR - http://www.scopus.com/inward/record.url?scp=85103251032&partnerID=8YFLogxK

U2 - 10.48550/arXiv.2007.14889

DO - 10.48550/arXiv.2007.14889

M3 - Article

VL - 502

SP - 935

EP - 952

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 1

ER -