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Article: Deep Chandra observation of the pulsar wind nebula powered by pulsar PSR J1846-0258 in the supernova remnant KES 75

TitleDeep Chandra observation of the pulsar wind nebula powered by pulsar PSR J1846-0258 in the supernova remnant KES 75
Authors
KeywordsPulsars: Individual (Psr J1846-0258)
Stars: Winds, Outflows
Supernovae: Individual (Kes 75)
X-Rays: Ism
Issue Date2008
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637X/
Citation
Astrophysical Journal, 2008, v. 686 n. 1, p. 508-519 How to Cite?
AbstractWe present the results of detailed spatial and spectral analysis of the pulsar wind nebula (PWN) in supernova remnant Kes 75 (G29.7-0.3) using a deep exposure with Chandra X-Ray Observatory. The PWN shows a complex morphology with clear axisymmetric structure. We identified a one-sided jet and two bright clumps aligned with the overall nebular elongation, and an arclike feature perpendicular to the jet direction. We interpret the arc as an equatorial torus or wisp and the clumps could be shock interaction between the jets and the surrounding medium. Spatial modeling of the features with a torus and jet model indicates a position angle 207° ± 8° for the PWN symmetry axis. The lack of any observable counter jet implies a flow velocity larger than 0.4 c. Comparing to an archival observation 6 yr earlier, some small-scale features in the PWN demonstrate strong variability: the flux of the inner jet doubles, and the peak of the northern clump broadens and shifts 2′ outward. As recently reported from RXTE observations, magnetar-like bursts of the central pulsar occurred coincidentally 7 days before the Chandra exposure. Accompanied with the bursts is a temporary increase in the pulsar flux: during the Chandra observation, the pulsar luminosity is 6 times larger than in quiescent state, and shows substantial spectral softening from Γ = 1.1 to 1.9 with an emerging thermal component. © 2008. The American Astronomy Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/180489
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.authorSlane, POen_US
dc.contributor.authorGaensler, BMen_US
dc.contributor.authorHughes, JPen_US
dc.date.accessioned2013-01-28T01:38:46Z-
dc.date.available2013-01-28T01:38:46Z-
dc.date.issued2008en_US
dc.identifier.citationAstrophysical Journal, 2008, v. 686 n. 1, p. 508-519en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/10722/180489-
dc.description.abstractWe present the results of detailed spatial and spectral analysis of the pulsar wind nebula (PWN) in supernova remnant Kes 75 (G29.7-0.3) using a deep exposure with Chandra X-Ray Observatory. The PWN shows a complex morphology with clear axisymmetric structure. We identified a one-sided jet and two bright clumps aligned with the overall nebular elongation, and an arclike feature perpendicular to the jet direction. We interpret the arc as an equatorial torus or wisp and the clumps could be shock interaction between the jets and the surrounding medium. Spatial modeling of the features with a torus and jet model indicates a position angle 207° ± 8° for the PWN symmetry axis. The lack of any observable counter jet implies a flow velocity larger than 0.4 c. Comparing to an archival observation 6 yr earlier, some small-scale features in the PWN demonstrate strong variability: the flux of the inner jet doubles, and the peak of the northern clump broadens and shifts 2′ outward. As recently reported from RXTE observations, magnetar-like bursts of the central pulsar occurred coincidentally 7 days before the Chandra exposure. Accompanied with the bursts is a temporary increase in the pulsar flux: during the Chandra observation, the pulsar luminosity is 6 times larger than in quiescent state, and shows substantial spectral softening from Γ = 1.1 to 1.9 with an emerging thermal component. © 2008. The American Astronomy 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/0004-637X/en_US
dc.relation.ispartofAstrophysical Journalen_US
dc.subjectPulsars: Individual (Psr J1846-0258)en_US
dc.subjectStars: Winds, Outflowsen_US
dc.subjectSupernovae: Individual (Kes 75)en_US
dc.subjectX-Rays: Ismen_US
dc.titleDeep Chandra observation of the pulsar wind nebula powered by pulsar PSR J1846-0258 in the supernova remnant KES 75en_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.doi10.1086/591146en_US
dc.identifier.scopuseid_2-s2.0-53849115069en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-53849115069&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume686en_US
dc.identifier.issue1en_US
dc.identifier.spage508en_US
dc.identifier.epage519en_US
dc.identifier.isiWOS:000259822200041-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridNg, CY=24830903500en_US
dc.identifier.scopusauthoridSlane, PO=7003826185en_US
dc.identifier.scopusauthoridGaensler, BM=34769921200en_US
dc.identifier.scopusauthoridHughes, JP=35483904100en_US
dc.customcontrol.immutablejt 130807-

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