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. © 2007. The American Astronomical Society. All rights reserved.

Original language	English
Pages (from-to)	487-493
Number of pages	6
Journal	Astrophysical Journal
Volume	654
Issue number	1 I
DOIs	https://doi.org/10.1086/510576
Publication status	Published - 1 Jan 2007

Keywords

Astrometry
Pulsars: individual (PSR J0538+2817)
Stars: kinematics
Supernovae: individual (S147)

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10.1086/510576

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@article{3a0dff8d9a204742948dc85b1dab4846,

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. {\textcopyright} 2007. The American Astronomical Society. All rights reserved.",

keywords = "Astrometry, Pulsars: individual (PSR J0538+2817), Stars: kinematics, Supernovae: individual (S147)",

author = "Ng, {C. Y.} and Romani, {Roger W.} and Brisken, {Walter F.} and Shami Chatterjee and Michael Kramer",

year = "2007",

month = jan,

day = "1",

doi = "10.1086/510576",

language = "English",

volume = "654",

pages = "487--493",

journal = "Astrophysical Journal",

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publisher = "American Astronomical Society",

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TY - JOUR

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

Y1 - 2007/1/1

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. © 2007. The American Astronomical Society. All rights reserved.

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. © 2007. The American Astronomical Society. All rights reserved.

KW - Astrometry

KW - Pulsars: individual (PSR J0538+2817)

KW - Stars: kinematics

KW - Supernovae: individual (S147)

U2 - 10.1086/510576

DO - 10.1086/510576

M3 - Article

SN - 1538-4357

VL - 654

SP - 487

EP - 493

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 I

ER -

The origin and motion of PSR J0538+2817 in S147

Abstract

Keywords

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