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

摘要

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.