The origin and motion of PSR J0538+2817 in S147

C. Y. Ng; Roger W. Romani; Walter F. Brisken; Shami Chatterjee; Michael Kramer

doi:10.1086/510576

The origin and motion of PSR J0538+2817 in S147

C. Y. Ng, Roger W. Romani, Walter F. Brisken, Shami Chatterjee, Michael Kramer

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Abstract

We report on Very Long Baseline Array (VLBA) astrometry and Chandra imaging of PSR J0538+2817 in the supernova remnant S147. We measure a parallax distance of 1.47_-0.27^+0.42 kpc along with a high-precision proper motion, giving a transverse velocity V⊥ = 400_-73⁺¹¹⁴ km s^-1. A small extended wind nebula is detected around the pulsar; the symmetry axis of this structure suggests that the spin axis lies 12° ± 4° from the velocity vector (two-dimensional), but the emission is too faint for robust model-independent statements. The neutron star is hot, consistent with the young ∼40 kyr kinematic age. The pulsar progenitor is likely a runaway from a nearby cluster, with NGC 1960 (M36) a leading candidate.

Original language	English (US)
Pages (from-to)	487-493
Number of pages	7
Journal	Astrophysical Journal
Volume	654
Issue number	1 I
DOIs	https://doi.org/10.1086/510576
State	Published - Jan 1 2007
Externally published	Yes

Keywords

Astrometry
Stars: kinematics
Supernovae: individual (S147)

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title = "The origin and motion of PSR J0538+2817 in S147",

abstract = "We report on Very Long Baseline Array (VLBA) astrometry and Chandra imaging of PSR J0538+2817 in the supernova remnant S147. We measure a parallax distance of 1.47-0.27+0.42 kpc along with a high-precision proper motion, giving a transverse velocity V⊥ = 400-73+114 km s-1. A small extended wind nebula is detected around the pulsar; the symmetry axis of this structure suggests that the spin axis lies 12° ± 4° from the velocity vector (two-dimensional), but the emission is too faint for robust model-independent statements. The neutron star is hot, consistent with the young ∼40 kyr kinematic age. The pulsar progenitor is likely a runaway from a nearby cluster, with NGC 1960 (M36) a leading candidate.",

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T1 - The origin and motion of PSR J0538+2817 in S147

AU - Ng, C. Y.

AU - Romani, Roger W.

AU - Brisken, Walter F.

AU - Chatterjee, Shami

AU - Kramer, Michael

PY - 2007/1/1

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N2 - We report on Very Long Baseline Array (VLBA) astrometry and Chandra imaging of PSR J0538+2817 in the supernova remnant S147. We measure a parallax distance of 1.47-0.27+0.42 kpc along with a high-precision proper motion, giving a transverse velocity V⊥ = 400-73+114 km s-1. A small extended wind nebula is detected around the pulsar; the symmetry axis of this structure suggests that the spin axis lies 12° ± 4° from the velocity vector (two-dimensional), but the emission is too faint for robust model-independent statements. The neutron star is hot, consistent with the young ∼40 kyr kinematic age. The pulsar progenitor is likely a runaway from a nearby cluster, with NGC 1960 (M36) a leading candidate.

AB - We report on Very Long Baseline Array (VLBA) astrometry and Chandra imaging of PSR J0538+2817 in the supernova remnant S147. We measure a parallax distance of 1.47-0.27+0.42 kpc along with a high-precision proper motion, giving a transverse velocity V⊥ = 400-73+114 km s-1. A small extended wind nebula is detected around the pulsar; the symmetry axis of this structure suggests that the spin axis lies 12° ± 4° from the velocity vector (two-dimensional), but the emission is too faint for robust model-independent statements. The neutron star is hot, consistent with the young ∼40 kyr kinematic age. The pulsar progenitor is likely a runaway from a nearby cluster, with NGC 1960 (M36) a leading candidate.

KW - Astrometry

KW - Stars: kinematics

KW - Supernovae: individual (S147)

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IS - 1 I

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The origin and motion of PSR J0538+2817 in S147

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