• DOI:10.1093/mnras/stv1420
• Corpus ID: 51802612

Observations of PSR J1357−6429 at 2.1 GHz with the Australia Telescope Compact Array

@article{Kirichenko2015ObservationsOP,
  title={Observations of PSR J1357−6429 at 2.1 GHz with the Australia Telescope Compact Array},
  author={A. Yu. Kirichenko and Yury Shibanov and Peter S Shternin and S Johnston and Maxim A. Voronkov and A Danilenko and D. P. Barsukov and Dong Lai and Dmitri Zyuzin},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2015},
  volume={452},
  pages={3273-3280}
}

• A. Kirichenko, Y. Shibanov, +6 authors D. Zyuzin
• Published 24 June 2015
• Physics
• Monthly Notices of the Royal Astronomical Society

PSR J1357−6429 is a young and energetic radio pulsar detected in X-rays and γ-rays. It powers a compact pulsar wind nebula
with a jet visible in X-rays and a large-scale plerion detected in X-ray and TeV ranges. Previous multiwavelength studies
suggested that the pulsar has a significant proper motion of about 180 mas yr−1, implying an extremely high transverse velocity of about 2000 km s−1. In order to verify this, we performed radio-interferometric observations of PSR J1357−6429 with the Australia Telescope
Compact Array (ATCA) 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 = 13h57m02 s . 525(14), Dec. =−64°29'29 " . 89(15).

Using both new and archival ATCA data, we did not find any proper motion and estimated its 90 per cent upper limit
as μ < 106 mas yr−1. The pulsar shows a highly polarized single pulse, as was observed earlier 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 discount the claim of an optical counterpart candidate reported
previously.