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

TL;DR

This study measures the proper motion of pulsar PSR J1709-4429, analyzes its association with a supernova remnant, and explores the dynamics of its pulsar wind nebula through deep X-ray imaging over several years.

Contribution

First measurement of PSR J1709-4429's proper motion using multi-epoch Chandra data, clarifying its relationship with SNR G343.1-2.3 and revealing PWN dynamics.

Findings

Proper motion of 13 ± 3 mas/yr at PA 86 ± 9 degrees.

Pulsar likely did not originate at the SNR center.

PWN exhibits dynamic features with possible jet structures.

Abstract

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.