Fast as Potoroo: Radio Continuum Detection of a Bow-Shock Pulsar Wind Nebula Powered by Pulsar J1638–4713

IF 4.5 3区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Publications of the Astronomical Society of Australia Pub Date : 2024-03-25 DOI:10.1017/pasa.2024.13

Sanja Lazarević, Miroslav D. Filipović, Shi Dai, Roland Kothes, Adeel Ahmad, Rami Z. E. Alsaberi, Joel C. F. Balzan, Luke A. Barnes, William D. Cotton, Philip G. Edwards, Yjan A. Gordon, Frank Haberl, Andrew M. Hopkins, Bärbel S. Koribalski, Denis Leahy, Chandreyee Maitra, Marko Mićić, Gavin Rowell, Manami Sasaki, Nicholas F. H. Tothill, Grazia Umana, Velibor Velović

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Abstract

We report the discovery of a bow-shock pulsar wind nebula (PWN), named Potoroo, and the detection of a young pulsar J1638–4713 that powers the nebula. We present a radio continuum study of the PWN based on 20-cm observations obtained from the Australian Square Kilometre Array Pathfinder (ASKAP) and MeerKAT. PSR J1638–4713 was identified using Parkes radio telescope observations at frequencies above 3 GHz. The pulsar has the second-highest dispersion measure of all known radio pulsars (1553 pc cm–3), a spin period of 65.74 ms and a spin-down luminosity of Ė = 6.1 × 1036 erg s–1. The PWN has a cometary morphology and one of the greatest projected lengths among all the observed pulsar radio tails, measuring over 21 pc for an assumed distance of 10 kpc. The remarkably long tail and atypically steep radio spectral index are attributed to the interplay of a supernova reverse shock and the PWN. The originating supernova remnant is not known so far. We estimated the pulsar kick velocity to be in the range of 1000 – 2000 km s–1 for ages between 23 and 10 kyr. The X-ray counterpart found in Chandra data, CXOU J163802.6–471358, shows the same tail morphology as the radio source but is shorter by a factor of 10. The peak of the X-ray emission is offset from the peak of the radio total intensity (Stokes I) emission by approximately 4.7”, but coincides well with circularly polarised (Stokes V) emission. No infrared counterpart was found.

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像波托鲁一样快脉冲星 J1638-4713 驱动的弓震脉冲星风星云的射电连续探测

我们报告发现了一个名为 "Potoroo "的弓形冲击脉冲星风星云（PWN），并探测到了为该星云提供能量的一颗年轻脉冲星J1638-4713。我们根据从澳大利亚平方公里阵列探路者（ASKAP）和MeerKAT获得的20厘米观测数据，介绍了对PWN的射电连续波研究。PSR J1638-4713 是通过帕克斯射电望远镜在 3 GHz 以上频率的观测发现的。该脉冲星在所有已知射电脉冲星中具有第二高的色散测量值（1553 pc cm-3），自旋周期为 65.74 ms，自旋下降光度为 Ė = 6.1 × 1036 erg s-1。这颗脉冲星具有彗星形态，是所有观测到的脉冲星射电尾迹中投影长度最大的一个，在假定距离为 10 kpc 的情况下，其投影长度超过 21 pc。超长的尾部和异常陡峭的射电光谱指数归因于超新星反向冲击和PWN的相互作用。目前还不知道超新星残余物的起源。我们估计脉冲星的踢速度在 1000-2000 km s-1 之间，年龄在 23-10 kyr 之间。钱德拉数据中发现的 X 射线对应星 CXOU J163802.6-471358，其尾部形态与射电源相同，但比射电源短 10 倍。X 射线发射的峰值与射电总强度（斯托克斯 I）发射的峰值相差约 4.7"，但与圆偏振（斯托克斯 V）发射非常吻合。没有发现红外线对应物。

本文章由计算机程序翻译，如有差异，请以英文原文为准。

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来源期刊

Publications of the Astronomical Society of Australia 地学天文-天文与天体物理

CiteScore

5.90

自引率

9.50%

发文量

审稿时长

>12 weeks

期刊介绍： Publications of the Astronomical Society of Australia (PASA) publishes new and significant research in astronomy and astrophysics. PASA covers a wide range of topics within astronomy, including multi-wavelength observations, theoretical modelling, computational astronomy and visualisation. PASA also maintains its heritage of publishing results on southern hemisphere astronomy and on astronomy with Australian facilities. PASA publishes research papers, review papers and special series on topical issues, making use of expert international reviewers and an experienced Editorial Board. As an electronic-only journal, PASA publishes paper by paper, ensuring a rapid publication rate. There are no page charges. PASA''s Editorial Board approve a certain number of papers per year to be published Open Access without a publication fee.