TY - JOUR
T1 - PSR J1709-4429's proper motion and its relationship to SNR G343.1-2.3
AU - De Vries, Martijn
AU - Romani, Roger W.
AU - Kargaltsev, Oleg
AU - Pavlov, George
AU - Posselt, Bettina
AU - Slane, Patrick
AU - Bucciantini, Niccolo
AU - Ng, C. Y.
AU - Klingler, Noel
N1 - Publisher Copyright:
© 2021 Institute of Physics Publishing. All rights reserved.
PY - 2021/2/10
Y1 - 2021/2/10
N2 - We have obtained a deep (670 ks) CXO ACIS image of the remarkable pulsar wind nebula (PWN) of PSR J1709 -4429, in four epochs during 2018-2019. Comparison with an archival 2004 data set provides a pulsar proper motion μ=13 ± 3 mas yr-1at a PA of 86° ± 9° (1σ combined statistical and systematic uncertainties), precluding birth near the center of SNR G343.1-2.3. At the pulsar's characteristic age of 17 kyr, the association can be preserved through a combination of progenitor wind, birth kick, and PWN outflow. Associated TeV emission may, however, indicate an explosion in an earlier supernova. Inter-epoch comparison of the X-ray images shows that the PWN is dynamic, but we are unable to conclusively measure flow speeds from blob motion. The pulsar has generated a radio/X-ray wind bubble, and we argue that the PWN's long narrow jets are swept back by shocked pulsar wind venting from this cavity. These jets may trace the polar magnetic field lines of the PWN flow, an interesting challenge for numerical modeling.
AB - We have obtained a deep (670 ks) CXO ACIS image of the remarkable pulsar wind nebula (PWN) of PSR J1709 -4429, in four epochs during 2018-2019. Comparison with an archival 2004 data set provides a pulsar proper motion μ=13 ± 3 mas yr-1at a PA of 86° ± 9° (1σ combined statistical and systematic uncertainties), precluding birth near the center of SNR G343.1-2.3. At the pulsar's characteristic age of 17 kyr, the association can be preserved through a combination of progenitor wind, birth kick, and PWN outflow. Associated TeV emission may, however, indicate an explosion in an earlier supernova. Inter-epoch comparison of the X-ray images shows that the PWN is dynamic, but we are unable to conclusively measure flow speeds from blob motion. The pulsar has generated a radio/X-ray wind bubble, and we argue that the PWN's long narrow jets are swept back by shocked pulsar wind venting from this cavity. These jets may trace the polar magnetic field lines of the PWN flow, an interesting challenge for numerical modeling.
UR - http://www.scopus.com/inward/record.url?scp=85101526073&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85101526073&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/abcebe
DO - 10.3847/1538-4357/abcebe
M3 - Article
AN - SCOPUS:85101526073
SN - 0004-637X
VL - 908
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 50
ER -