PSR J1709-4429’s Proper Motion and its Relationship to SNR G343.1-2.3

Kavli Affiliate: Roger W. Romani

| First 5 Authors: Martijn de Vries, Roger W. Romani, Oleg Kargaltsev, George Pavlov, Bettina Posselt

| Summary:

We have obtained a deep 670 ks CXO ACIS image of the remarkable pulsar wind
nebula (PWN) of PSR J1709-4429, in 4 epochs during 2018-2019. Comparison with
an archival 2004 data set provides a pulsar proper motion mu = 13 pm 3 mas/yr
at a PA of 86 pm 9 degree (1 sigma 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 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.

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