Radio-interferometric observations of PSR J1357−6429 at 2.1 GHz

A. Kirichenko1, Yu. Shibanov1, P. Shternin1, S. Johnston2, M. A. Voronkov2, A. Danilenko1, D. Barsukov1, D. Lai,3 D. Zyuzin1

1Ioffe Institute, Polytekhnicheskaya 26, 194021, St. Petersburg, Russia
2CSIRO Astronomy and Space Science, Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, Australia
3Department of Astronomy, Cornell University, Ithaca, NY 14853, USA

PSR J1357−6429 is a young and energetic radio pulsar detected in X-rays and gamma-rays. It powers a compact pulsar wind nebula with a jet visible in X-rays and a large scale plerion detected in the radio, X-ray and TeV ranges. Previous multiwavelength studies suggested that the pulsar has a significant proper motion of about 180 mas/yr implying an extremely high transverse velocity of about 2000 km/s. In order to verify that, we performed radio-interferometric observations of PSR J1357−6429 with the Australia Telescope Compact Array in the 2.1 GHz band. We detected the pulsar with a mean flux density of 212 ± 5 μJy and obtained the most accurate pulsar position, RA = 13:57:02.525(14) and Dec = −64:29:29.89(15). Using the new and archival ATCA data, we did not find any proper motion and estimated its 90 per cent upper limit |μ|<100 mas/yr. The pulsar shows a highly polarised single pulse, as it was earlier observed at 1.4 GHz. Spectral analysis revealed a shallow spectral index αν = 0.5 ± 0.1. Based on our new radio position of the pulsar, we disclaim its optical counterpart candidate reported before.

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