An expanding radio nebula produced by a giant flare from the magnetar SGR 1806–20

Gaensler, B. M.; Kouveliotou, C.; Gelfand, Joseph D.; Taylor, G. B.; Eichler, David; Wijers, R. A. M. J.; Granot, Jonathan; Ramírez-Ruiz, E.; Lyubarsky, Yuri; Hunstead, R. W.; Campbell-Wilson, D.; Horst, A. J. van der; McLaughlin, M. A.; Fender, R. P.; Garrett, M. A.; Newton‐McGee, K.; Palmer, D. M.; Gehrels, N.; Woods, Peter

doi:10.1038/nature03498

Cited by 183 publications

(226 citation statements)

References 23 publications

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“…The prompt emission saturated almost all g-ray detectors, except for those on the Geotail spacecraft, which provided a reliable measurement of the peak intensity (Terasawa et al 2005 two giant flares previously observed from other SGRs. Following this event, afterglow emission similar to that commonly observed in g-ray bursts has been observed in the radio band, with a resolved extended structure (Cameron et al 2005;Gaensler et al 2005) and possibly also at hard X-ray energies (Mereghetti et al 2005a). The extremely accurate localization (∼0Љ .1) obtained with the radio data made possible the identification of a variable infrared counterpart (Kosugi et al 2005;Israel et al 2005).…”

Section: Introductionmentioning

confidence: 96%

A First Look with Chandra at SGR 1806-20 after the Giant Flare: Significant Spectral Softening and Rapid Flux Decay

Rea

Tiengo

Mereghetti³

et al. 2005

ApJ

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We report on the results of an ∼30 ks Chandra pointing of the soft gamma-ray repeater SGR 1806Ϫ20, the first X-ray observation with high spectral resolution performed after the 2004 December 27 giant flare. The source was found in a bursting active phase and with a significantly softer spectrum than that of the latest observations before the giant flare. The observed flux in the 2-10 keV range was ∼ ergs cm Ϫ2 s Ϫ1 , about 20% Ϫ11 2.2 # 10 lower than that measured 3 months before the event. This indicates that although its giant flare was ≈100 times more intense than those previously observed in two other soft gamma-ray repeaters, the postflare X-ray flux decay of SGR 1806Ϫ20 has been much faster. The pulsed fraction was ∼3%, a smaller value than that observed before the flare. We discuss the different properties of the postflare evolution of SGR 1806Ϫ20 in comparison to those of SGR 1900ϩ14 and interpret the results as strong evidence that a magnetospheric untwisting occurred (or is occurring) after the giant flare.

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Section: Introductionmentioning

confidence: 96%

A First Look with Chandra at SGR 1806-20 after the Giant Flare: Significant Spectral Softening and Rapid Flux Decay

Rea

Tiengo

Mereghetti³

et al. 2005

ApJ

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“…04, respectively; Kaplan et al 2002;Gaensler et al 2005). However, given that the Gaensler et al (2005) radio position refers to about 20 days after the giant flare of SGR 1806-20, and that the source from which is originating the radio emission is moving at about 4 mas/day (Taylor et al 2005), we also plot the VLA position obtained after 7 days by Cameron et al (2005; 1σ radius if 0. 1), corrected for about 30 mas in right ascension (following Taylor et al 2005); this corresponds to a final 1σ confidence level radius of 0.…”

Section: Naos-conica Observations At Vltmentioning

confidence: 99%

“…Few days after this event, SGR 1806-20 was observed and detected in the radio band for the first time, providing very accurate positions (VLA; Cameron et al 2005;Gaensler et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Discovery and monitoring of the likely IR counterpart of SGR 1806–20 during the 2004 γ-ray burst-active state

Israel¹,

Covino

Mignani

et al. 2005

A&A

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Abstract. The sky region including the Chandra position of SGR 1806-20 was monitored in the IR band during 2004, following its increased high energy bursting activity. Observations were performed using NAOS-CONICA, the adaptive optics IR camera mounted on Yepun VLT, which provided images of unprecedented quality (FWHM better than 0. 1). After the 2004 December 27th giant flare, the source position has been nailed by VLA observations of its radio counterpart, reducing the positional uncertainty to 0. 04. Using IR data from our monitoring campaign, we discovered the likely IR counterpart to SGR 1806-20 based on positional coincidence with the Chandra and VLA uncertainty regions and flux variability of a factor of about 2 correlated with that at higher energies. We compare our findings with other isolated neutron star classes thought to be related, at some level, with SGRs.

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“…Further supporting evidence for this hypothesis comes from a study of the expanding H i shell around the magnetar 1E 1048.1-5937. When the shell was interpreted as a stellar wind bubble blown by the progenitor, a progenitor mass of 30-40 M was inferred (Gaensler et al 2005a). …”

Section: Introductionmentioning

confidence: 99%

The Progenitor Mass of the Magnetar Sgr1900+14

Davies

Figer

Kudritzki

et al. 2009

ApJ

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Magnetars are young neutron stars with extreme magnetic fields (B 10 14 -10 15 G). How these fields relate to the properties of their progenitor stars is not yet clearly established. However, from the few objects associated with young clusters it has been possible to estimate the initial masses of the progenitors, with results indicating that a very massive progenitor star (M prog > 40 M ) is required to produce a magnetar. Here, we present adaptive-optics assisted Keck/ NIRC2 imaging and Keck/NIRSPEC spectroscopy of the cluster associated with the magnetar SGR 1900+14, and report that the initial progenitor star mass of the magnetar was a factor of 2 lower than this limit, M prog = 17±2 M . Our result presents a strong challenge to the concept that magnetars can only result from very massive progenitors. Instead, we favor a mechanism which is dependent on more than just initial stellar mass for the production of these extreme magnetic fields, such as the "fossil-field" model or a process involving close binary evolution.

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An expanding radio nebula produced by a giant flare from the magnetar SGR 1806–20

Cited by 183 publications

References 23 publications

A First Look with Chandra at SGR 1806-20 after the Giant Flare: Significant Spectral Softening and Rapid Flux Decay

A First Look with Chandra at SGR 1806-20 after the Giant Flare: Significant Spectral Softening and Rapid Flux Decay

Discovery and monitoring of the likely IR counterpart of SGR 1806–20 during the 2004 γ-ray burst-active state

The Progenitor Mass of the Magnetar Sgr1900+14

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