Multi-instrument X-ray monitoring of the January 2009 outburst from the recurrent magnetar candidate 1E 1547.0-5408

Bernardini, F.; Israel, G. L.; Stella, L.; Turolla, R.; Esposito, P.; Rea, N.; Zane, S.; Tiengo, A.; Campana, S.; Götz, D.; Mereghetti, S.; Romano, P.

doi:10.1051/0004-6361/201016197

Cited by 48 publications

(59 citation statements)

References 43 publications

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“…After submission of our manuscript, we became aware of the work by Bernardini et al (2011) on the 2009 outburst of 1E 1547−5408 using Swift XRT data. A preliminary comparison of their results with ours shows general agreement.…”

Section: Discussionmentioning

confidence: 99%

The 2009 Outburst of Magnetar 1e 1547--5408: Persistent Radiative and Burst Properties

Scholz¹,

Kaspi²

2011

ApJ

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The magnetar 1E 1547−5408 recently exhibited two periods of outburst, beginning on 2008 October 3 and 2009 January 22. Here we present an analysis of the persistent radiative evolution and a statistical study of the burst properties during the 2009 outburst using the Swift X-ray Telescope (XRT). We find that the 1-10 keV flux increased by a factor of ∼ 500 and hardened significantly, peaking ∼ 6 hours after the onset of the outburst. The observed pulsed fraction exhibited an anticorrelation with phase-averaged flux. Properties of the several hundred X-ray bursts during the 2009 outburst were determined and compared to those from other magnetar outburst events. We find that the peaks of the bursts occur randomly in phase but that the folded counts that compose the bursts exhibit a pulse which is misaligned with the persistent pulse phase. We also report a correlation between burst hardness and flux. We compare the hardness-flux evolution of the persistent emission of both outbursts to those from other magnetars and find that although there does exist an overall trend, the degree of hardening for a given increase in flux is not uniform from source to source. These results are discussed in the context of previous results and within the magnetar model.

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Section: Discussionmentioning

confidence: 99%

The 2009 Outburst of Magnetar 1e 1547--5408: Persistent Radiative and Burst Properties

Scholz¹,

Kaspi²

2011

ApJ

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“…They further claim that this behavior is similar to the one observed in AXP 1E2259+586 and not in agreement with an SGR persistent emission. Although the persistent emission energy release cannot be directly measured by GBM or SPI-ACS, Bernardini et al (2011) have shown that for that same time period, it can be at most a factor of five higher in the 13-200 keV than in the 1-10 keV range. The energy released in bursts during a week is thus comparable to the energy released in the persistent emission during an eightmonth period (Scholz & Kaspi 2011), and we conclude that SGR J1550−5418 exhibits similar energetics behavior as other SGR sources .…”

Section: Burst Energeticsmentioning

confidence: 99%

SGR J1550–5418 BURSTS DETECTED WITH THEFERMIGAMMA-RAY BURST MONITOR DURING ITS MOST PROLIFIC ACTIVITY

Horst

Kouveliotou

Gorgone

et al. 2012

ApJ

118

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We have performed detailed temporal and time-integrated spectral analysis of 286 bursts from SGR J1550−5418 detected with the Fermi Gamma-ray Burst Monitor (GBM) in 2009 January, resulting in the largest uniform sample of temporal and spectral properties of SGR J1550−5418 bursts. We have used the combination of broadband and high time-resolution data provided with GBM to perform statistical studies for the source properties. We determine the durations, emission times, duty cycles, and rise times for all bursts, and find that they are typical of SGR bursts. We explore various models in our spectral analysis, and conclude that the spectra of SGR J1550−5418 bursts in the 8-200 keV band are equally well described by optically thin thermal bremsstrahlung (OTTB), a power law (PL) with an exponential cutoff (Comptonized model), and two blackbody (BB) functions (BB+BB). In the spectral fits with the Comptonized model, we find a mean PL index of −0.92, close to the OTTB index of −1. We show that there is an anti-correlation between the Comptonized E peak and the burst fluence and average flux. For the BB+BB fits, we find that the fluences and emission areas of the two BB functions are correlated. The low-temperature BB has an emission area comparable to the neutron star surface area, independent of the temperature, while the hightemperature BB has a much smaller area and shows an anti-correlation between emission area and temperature. We compare the properties of these bursts with bursts observed from other SGR sources during extreme activations, and discuss the implications of our results in the context of magnetar burst models.

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“…In quiescence, luminosities as low as ∼ 10 31 erg s −1 have been observed. The outburst duty cycle of transient AXPs/SGRs is still poorly known: multiple out-bursts have been observed only in SGR 1627−41 and 1E 1547.0−5408 [46,11].…”

Section: Observational Propertiesmentioning

confidence: 99%

Pulsars and Magnetars

Mereghetti

2013

Braz J Phys

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The high-energy sources known as anomalous X-ray pulsars (AXPs) and soft γ-ray repeaters (SGRs) are well explained as magnetars: isolated neutron stars powered by their own magnetic energy. After explaining why it is generally believed that the traditional energy sources at work in other neutron stars (accretion, rotation, residual heat) cannot power the emission of AXPs/SGRs, I review the observational properties of the twenty AXPs/SGRs currently known and describe the main features of the magnetar model. In the last part of this review I discuss the recent discovery of magnetars with low external dipole field and some of the relations between AXPs/SGRs and other classes of isolated neutron stars.

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Multi-instrument X-ray monitoring of the January 2009 outburst from the recurrent magnetar candidate 1E 1547.0-5408

Cited by 48 publications

References 43 publications

The 2009 Outburst of Magnetar 1e 1547--5408: Persistent Radiative and Burst Properties

The 2009 Outburst of Magnetar 1e 1547--5408: Persistent Radiative and Burst Properties

SGR J1550–5418 BURSTS DETECTED WITH THEFERMIGAMMA-RAY BURST MONITOR DURING ITS MOST PROLIFIC ACTIVITY

Pulsars and Magnetars

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