On the Extended Emission of the Magnetar 1E 1547.0–5408 | Zendy

S. A. Olausen | Zendy; V. M. Kaspi | Zendy; Cherry Ng | Zendy; Rim Dib | Zendy; Weiwei Zhu | Zendy; F. P. Gavriil | Zendy; Peter Woods | Zendy; M. Burgay | Zendy; Nicolò D’Amico | Zendy; P. Esposito | Zendy; A. Pellizzoni | Zendy; Andrea Possenti | Zendy

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On the Extended Emission of the Magnetar 1E 1547.0–5408

Author(s) -

S. A. Olausen,

V. M. Kaspi,

Cherry Ng,

Rim Dib,

Weiwei Zhu,

F. P. Gavriil,

Peter Woods,

M. Burgay,

Nicolò D’Amico,

P. Esposito,

A. Pellizzoni,

Andrea Possenti

Publication year - 2011

Publication title -

aip conference proceedings

Language(s) - English

Resource type - Conference proceedings

SCImago Journal Rank - 0.177

H-Index - 75

eISSN - 1551-7616

pISSN - 0094-243X

DOI - 10.1063/1.3615114

Subject(s) - magnetar , physics , astrophysics , halo , pulsar , flux (metallurgy) , pulsar wind nebula , astronomy , nebula , stars , materials science , galaxy , metallurgy

Recently, 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.link_to_subscribed_fulltex

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