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Conference Paper: On the extended emission of the magnetar 1E 1547.0-5408

TitleOn the extended emission of the magnetar 1E 1547.0-5408
Authors
Olausen, SKaspi, VMNg, CYDib, RZhu, WGavriil, FWoods, P
KeywordsMagnetar
Neutron Star
Issue Date2011
PublisherAmerican Institute of Physics. The Journal's web site is located at http://proceedings.aip.org/
Citation
AIP Conference Proceedings, 2011, v. 1357 n. 1, p. 193-194 How to Cite?
DOI: http://dx.doi.org/10.1063/1.3615114
AbstractRecently, Vink & Bamba (2009) detected extended emission around the magnetar 1E 1547.0-5408 in quiescence and characterized it as the result of a pulsar wind nebula (PWN). From analysis of a February 2010 XMM-Newton observation of the source, as well as three archival XMM-Newton observations, we confirm the detection of extended emission. However, we find that its X-ray flux is highly variable and tightly correlated with the X-ray flux of the magnetar itself. We conclude that it is most likely due to a dust-scattering halo and not a PWN as previously claimed. © 2011 American Institute of Physics.
Persistent Identifierhttp://hdl.handle.net/10722/180717
ISSN
0094-243X
2023 SCImago Journal Rankings: 0.152
ISI Accession Number ID
WOS:000295993400050
References
References in Scopus

 

DC FieldValueLanguage
dc.contributor.authorOlausen, Sen_US
dc.contributor.authorKaspi, VMen_US
dc.contributor.authorNg, CYen_US
dc.contributor.authorDib, Ren_US
dc.contributor.authorZhu, Wen_US
dc.contributor.authorGavriil, Fen_US
dc.contributor.authorWoods, Pen_US
dc.date.accessioned2013-01-28T01:41:46Z-
dc.date.available2013-01-28T01:41:46Z-
dc.date.issued2011en_US
dc.identifier.citationAIP Conference Proceedings, 2011, v. 1357 n. 1, p. 193-194-
dc.identifier.issn0094-243Xen_US
dc.identifier.urihttp://hdl.handle.net/10722/180717-
dc.description.abstractRecently, Vink & Bamba (2009) detected extended emission around the magnetar 1E 1547.0-5408 in quiescence and characterized it as the result of a pulsar wind nebula (PWN). From analysis of a February 2010 XMM-Newton observation of the source, as well as three archival XMM-Newton observations, we confirm the detection of extended emission. However, we find that its X-ray flux is highly variable and tightly correlated with the X-ray flux of the magnetar itself. We conclude that it is most likely due to a dust-scattering halo and not a PWN as previously claimed. © 2011 American Institute of Physics.en_US
dc.languageengen_US
dc.publisherAmerican Institute of Physics. The Journal's web site is located at http://proceedings.aip.org/-
dc.relation.ispartofAIP Conference Proceedingsen_US
dc.subjectMagnetaren_US
dc.subjectNeutron Staren_US
dc.titleOn the extended emission of the magnetar 1E 1547.0-5408en_US
dc.typeConference_Paperen_US
dc.identifier.emailNg, CY: stephen_ng@hku.hken_US
dc.identifier.authorityNg, CY=rp01706en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1063/1.3615114en_US
dc.identifier.scopuseid_2-s2.0-80052947333en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-80052947333&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume1357en_US
dc.identifier.issue1-
dc.identifier.spage193en_US
dc.identifier.epage194en_US
dc.identifier.isiWOS:000295993400050-
dc.publisher.placeUnited Statesen_US
dc.identifier.scopusauthoridOlausen, S=36669077400en_US
dc.identifier.scopusauthoridKaspi, VM=7006755510en_US
dc.identifier.scopusauthoridNg, CY=24830903500en_US
dc.identifier.scopusauthoridDib, R=8609966700en_US
dc.identifier.scopusauthoridZhu, W=55483175400en_US
dc.identifier.scopusauthoridGavriil, F=6602456240en_US
dc.identifier.scopusauthoridWoods, P=35560112800en_US
dc.identifier.issnl0094-243X-

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