| People | Locations | Statistics |
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| Naji, M. |
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| Motta, Antonella |
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| Aletan, Dirar |
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| Mohamed, Tarek |
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| Ertürk, Emre |
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| Taccardi, Nicola |
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| Kononenko, Denys |
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| Petrov, R. H. | Madrid |
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| Alshaaer, Mazen | Brussels |
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| Bih, L. |
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| Casati, R. |
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| Muller, Hermance |
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| Kočí, Jan | Prague |
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| Šuljagić, Marija |
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| Kalteremidou, Kalliopi-Artemi | Brussels |
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| Azam, Siraj |
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| Ospanova, Alyiya |
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| Blanpain, Bart |
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| Ali, M. A. |
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| Popa, V. |
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| Rančić, M. |
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| Ollier, Nadège |
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| Azevedo, Nuno Monteiro |
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| Landes, Michael |
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| Rignanese, Gian-Marco |
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Enoto, Teruaki
in Cooperation with on an Cooperation-Score of 37%
Topics
Publications (9/9 displayed)
- 2017Soft Gamma-ray Observation of SN2014J with Suzaku
- 2013Spectral Variation of Hard X-Ray Emission from the Crab Nebula with the Suzaku Hard X-Ray Detectorcitations
- 2012Possible Detection of an Emission Cyclotron Resonance Scattering Feature from the Accretion-powered Pulsar 4U 1626-67citations
- 2012The Hard X-ray Imager (HXI) for the ASTRO-H missioncitations
- 2012Spectral comparison of weak short bursts to the persistent X-rays from the magnetar 1E 1547.0-5408 in its 2009 outburstcitations
- 2011Improvements in Calibration of GSO Scintillators in the Suzaku Hard X-Ray Detectorcitations
- 2010Hard x-ray imager (HXI) for the ASTRO-H Missioncitations
- 2008In-Orbit Timing Calibration of the Hard X-Ray Detector on Board Suzakucitations
- 2007Improvement of ceramic YAG(Ce) scintillators to (YGd) <SUB>3</SUB>Al <SUB>5</SUB>O <SUB>12</SUB>(Ce) for gamma-ray detectorscitations
Places of action
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article
Spectral comparison of weak short bursts to the persistent X-rays from the magnetar 1E 1547.0-5408 in its 2009 outburst
Abstract
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 ̃2 × 10<SUP>-9</SUP> to 10<SUP>-7</SUP> erg cm<SUP>-2</SUP>. Thus, the 18 events define a significantly weaker burst sample than has ever been obtained previously, ̃10<SUP>-8</SUP>-10<SUP>-4</SUP> erg cm<SUP>-2</SUP>. 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) × 10<SUP>-8</SUP> erg s<SUP>-1</SUP> 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.