Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 765, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/765/1/L19
Keywords
pulsars: general; pulsars: individual (PSR J0357+3205); stars: neutron
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Funding
- European Commission Seventh Framework Programme (FP7) [267251]
- Canadian Space Agency
- Science and Technology Facilities Council [ST/H00260X/1] Funding Source: researchfish
- STFC [ST/H00260X/1] Funding Source: UKRI
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The middle-aged PSR J0357+3205 is a nearby, radio-quiet, bright gamma-ray pulsar discovered by the Fermi mission. Our previous Chandra observation revealed a huge, very peculiar structure of diffuse X-ray emission originating at the pulsar position and extending for >9' on the plane of the sky. To better understand the nature of such a nebula, we have studied the proper motion of the parent pulsar. We performed relative astrometry on Chandra images of the field spanning a time baseline of 2.2 yr, unveiling a significant angular displacement of the pulsar counterpart, corresponding to a proper motion of 0.'' 165 +/- 0.'' 030 yr(-1) at a position angle (P.A.) of 314 degrees +/- 8 degrees. At a distance of similar to 500 pc, the space velocity of the pulsar would be of similar to 390 km s(-1) assuming no inclination with respect to the plane of the sky. The direction of the pulsar proper motion is aligned very well with the main axis of the X-ray nebula (P.A. = 315 degrees.5 +/- 1 degrees.5), pointing to a physical, yet elusive, link between the nebula and the pulsar space velocity. No optical emission in the H alpha line is seen in a deep image collected at the Gemini telescope, which implies that the interstellar medium into which the pulsar is moving is fully ionized.
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