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Article: The origin and motion of PSR J0538+2817 in S147

TitleThe origin and motion of PSR J0538+2817 in S147
Authors
KeywordsAstrometry
Pulsars: Individual (Psr J0538+2817)
Stars: Kinematics
Supernovae: Individual (S147)
Issue Date2007
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637X
Citation
Astrophysical Journal, 2007, v. 654 n. 1 I, p. 487-493 How to Cite?
AbstractWe 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.
Persistent Identifierhttp://hdl.handle.net/10722/180484
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorNg, CYen_US
dc.contributor.authorRomani, RWen_US
dc.contributor.authorBrisken, WFen_US
dc.contributor.authorChatterjee, Sen_US
dc.contributor.authorKramer, Men_US
dc.date.accessioned2013-01-28T01:38:45Z-
dc.date.available2013-01-28T01:38:45Z-
dc.date.issued2007en_US
dc.identifier.citationAstrophysical Journal, 2007, v. 654 n. 1 I, p. 487-493en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/10722/180484-
dc.description.abstractWe 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.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637Xen_US
dc.relation.ispartofAstrophysical Journalen_US
dc.subjectAstrometryen_US
dc.subjectPulsars: Individual (Psr J0538+2817)en_US
dc.subjectStars: Kinematicsen_US
dc.subjectSupernovae: Individual (S147)en_US
dc.titleThe origin and motion of PSR J0538+2817 in S147en_US
dc.typeArticleen_US
dc.identifier.emailNg, CY: stephen_ng@hku.hken_US
dc.identifier.authorityNg, CY=rp01706en_US
dc.description.naturelink_to_OA_fulltexten_US
dc.identifier.doi10.1086/510576en_US
dc.identifier.scopuseid_2-s2.0-33846549132en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-33846549132&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume654en_US
dc.identifier.issue1 Ien_US
dc.identifier.spage487en_US
dc.identifier.epage493en_US
dc.identifier.isiWOS:000243221800034-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridNg, CY=24830903500en_US
dc.identifier.scopusauthoridRomani, RW=35248859100en_US
dc.identifier.scopusauthoridBrisken, WF=6602418286en_US
dc.identifier.scopusauthoridChatterjee, S=35500782800en_US
dc.identifier.scopusauthoridKramer, M=23968081200en_US
dc.customcontrol.immutablejt 130807-

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