TY - JOUR
T1 - Fast as Potoroo
T2 - radio continuum detection of a bow-shock pulsar wind nebula powered by pulsar J1638-4713
AU - Lazarević, Sanja
AU - Filipović, Miroslav D.
AU - Dai, Shi
AU - Kothes, Roland
AU - Ahmad, Adeel
AU - Alsaberi, Rami Z.E.
AU - Balzan, Joel C.F.
AU - Barnes, Luke A.
AU - Cotton, William D.
AU - Edwards, Philip G.
AU - Gordon, Yjan A.
AU - Haberl, Frank
AU - Hopkins, Andrew M.
AU - Koribalski, Bärbel S.
AU - Leahy, Denis
AU - Maitra, Chandreyee
AU - Mićić, Marko
AU - Rowell, Gavin
AU - Sasaki, Manami
AU - Tothill, Nicholas F.H.
AU - Umana, Grazia
AU - Velović, Velibor
N1 - Publisher Copyright:
© The Author(s), 2024. Published by Cambridge University Press on behalf of Astronomical Society of Australia.
PY - 2024
Y1 - 2024
N2 - 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 (1 553 pc cm), a spin period of 65.74 ms and a spin-down luminosity of erg s. 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 1 000-2 000 km s 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) emission by approximately 4.7, but coincides well with circularly polarised (Stokes) emission. No infrared counterpart was found.
AB - 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 (1 553 pc cm), a spin period of 65.74 ms and a spin-down luminosity of erg s. 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 1 000-2 000 km s 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) emission by approximately 4.7, but coincides well with circularly polarised (Stokes) emission. No infrared counterpart was found.
KW - ISM: individual (Potoroo)
KW - outflows
KW - pulsars: individual (PSR J1638-4713)
KW - radiation mechanism: non-thermal radio continuum: ISM
KW - stars: winds
KW - X-rays: individual (CXOU J163802.6-471358)
UR - http://www.scopus.com/inward/record.url?scp=85190111986&partnerID=8YFLogxK
U2 - 10.1017/pasa.2024.13
DO - 10.1017/pasa.2024.13
M3 - Article
AN - SCOPUS:85190111986
SN - 1323-3580
VL - 41
JO - Publications of the Astronomical Society of Australia
JF - Publications of the Astronomical Society of Australia
M1 - e032
ER -