Mon. Not. R. Astron. Soc., 427, 2824-2840 (2012/December-3)
Spectral comparison of weak short bursts to the persistent X-rays from the magnetar 1E 1547.0-5408 in its 2009 outburst.
ENOTO T., NAKAGAWA Y.E., SAKAMOTO T. and MAKISHIMA K.
Abstract (from CDS):
In 2009 January, the 2.1-s anomalous X-ray pulsar 1E 1547.0-5408 evoked intense burst activity. A follow-up Suzaku observation on January 28 recorded enhanced persistent emission in both soft and hard X-rays. Through a reanalysis of the same Suzaku data, 18 short bursts were identified in the X-ray events recorded by the Hard X-ray Detector (HXD) and the X-ray Imaging Spectrometer (XIS). Their spectral peaks appear in the HXD–PIN band, and their 10–70 keV X-ray fluences range from ∼ 2x10–9 to 10–7erg/cm2. Thus, the 18 events define a significantly weaker burst sample than has ever been obtained previously, ∼ 10–8–10–4 erg/cm2. In the ∼ 0.8 to ∼ 300 keV band, the spectra of the three brightest bursts can be represented successfully by a two-blackbody model, or a few alternative models. A spectrum that is constructed by stacking 13 weaker short bursts with fluences in the range (0.2–2) x 10–8 erg/s is less curved, and its ratio to the persistent emission spectrum becomes constant at ∼ 170 above ∼ 8 keV. As a result, the two-blackbody model was able to reproduce the stacked weaker-burst spectrum only after adding a power-law model, for which the photon index is fixed at 1.54 as measured by the persistent spectrum. These results imply that there is a possibility that the spectrum composition that employs an optically thick component and a hard power-law component can describe the wide-band spectra of both the persistent and weak-burst emissions, despite the fact that their fluxes differ by two orders of magnitude. Based on the spectral similarity, we discuss a possible connection between the unresolved short bursts and the persistent emission.
© 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS
stars: magnetars - pulsars: individual: 1E 1547.0-5408 - pulsars: individual: SGR J1550-5418 - pulsars: individual: PSR J1550-5418 - pulsars: individual: G327.24-013 - ISM: supernova remnant
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