Anomalous X‐Ray Pulsars and Soft Gamma‐Ray Repeaters in Supernova Remnants

Gaensler, B. M.; Slane, Patrick; Gotthelf, E. V.; Vasisht, Gautam

doi:10.1086/322358

Cited by 170 publications

(230 citation statements)

References 115 publications

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“…Halpern et al (2005) discovered transient radio emission from the transient AXP XTE J1810-197 which appeared sharply modulated at the rotation period with peak flux densities >1 Jy (Camilo et al 2006), orders of magnitude brighter than the reported upper limits for this or any other AXP. Gaensler et al (2001) have observed 4U 0142+61 with the VLA (1.4 GHz), but only a 5σ upper limit of 0.27 mJy could be extracted from the data.…”

Section: Introductionmentioning

confidence: 93%

The first multi-wavelength campaign of AXP 4U 0142+61 from radio to hard X-rays

Hartog

Kuiper

Hermsen

et al. 2007

Astrophys Space Sci

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For the first time a quasi-simultaneous multiwavelength campaign has been performed on an Anomalous X-ray Pulsar from the radio to the hard X-ray band. 4U 0142+61 was an INTEGRAL target for 1 Ms in July 2005. During these observations it was also observed in the X-ray band with Swift and RXTE, in the optical and NIR with Gemini North and in the radio with the WSRT. In this paper we present the source-energy distribution. The spectral results obtained in the individual wave bands do not connect smoothly; apparently components of different origin contribute to the total spectrum. Remarkable is that the INTEGRAL hard X-ray spectrum (power-law index 0.79 ± 0.10) is now measured up to an energy of ∼230 keV with no indication of a spectral break. Extrapolation of the INTEGRAL power-law spectrum to lower energies passes orders of magnitude underneath the NIR and optical fluxes,

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Section: Introductionmentioning

confidence: 93%

The first multi-wavelength campaign of AXP 4U 0142+61 from radio to hard X-rays

Hartog

Kuiper

Hermsen

et al. 2007

Astrophys Space Sci

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“…GögüY et al (2001 suggested that the difference between these values for the two SGRs is a result of a difference in an intrinsic physical property of the sources, such as the strength of magnetic field or the size of the active region. Given the generally softer persistent emission spectra of AXPs compared to SGRs, as well as the less frequent outbursts of the AXPs, it is reasonable to suspect that the two source classes also differ by some physical property; age (Kouveliotou et al 1998;Gaensler et al 2001), magnetic field , and progenitor mass (Gaensler 2004) have been proposed. The similarity of the burst durations of all three sources implies, however, that the physical property resulting in different mean burst durations must be different from the one that results in different average spectra and outburst frequency.…”

Section: Similarities Between Axp and Sgr Burstsmentioning

confidence: 99%

A Comprehensive Study of the X‐Ray Bursts from the Magnetar Candidate 1E 2259+586

Gavriil

Kaspi

Woods

2004

ApJ

118

164

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We present a statistical analysis of the X-ray bursts observed from the 2002 June 18 outburst of the anomalous X-ray pulsar (AXP) 1E 2259+586, observed with the Proportional Counter Array (PCA) aboard the Rossi X-Ray Timing Explorer. We show that the properties of these bursts are similar to those of soft gamma repeaters (SGRs). We find the following similarities: the burst durations follow a lognormal distribution that peaks at 99 ms, the differential burst fluence distribution is well described by a power law of index À1.7, the burst fluences are positively correlated with the burst durations, the distribution of waiting times is well described by a log normal distribution of mean 47 s, and the bursts are generally asymmetric, with shorter rise than fall times. However, we find several quantitative differences between the AXP and SGR bursts. Specifically, the AXP bursts we observed exhibit a wider range of durations, the correlation between burst fluence and duration is flatter than for SGRs, the observed AXP bursts are on average less energetic than observed SGR bursts, and the more energetic AXP bursts have the hardest spectra-the opposite of what is seen for SGRs. Unlike the case of SGRs, we find a correlation of burst phase with pulsed intensity. We conclude that the bursts are sufficiently similar that AXPs and SGRs can be considered united as a source class, yet there are some interesting differences that may help determine what physically differentiates the two closely related manifestations of neutron stars.

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“…4 we have drawn the spectral energy density of AXP 4U 0142+61 from radio (VLA, <0.27 mJy at 5σ Gaensler et al 2001) to X-ray (ASCA, White et al 1996). Both observed and dereddened fluxes are shown, using a reddening of 5.1 mag as derived from the X-ray absorption.…”

Section: The Spectral Energy Densitymentioning

confidence: 99%

“…Two of the five sources are associated with supernova remnants (Gaensler et al 2001), indicating that AXPs are young objects. For none of the sources, there is any evidence for orbital motion (from timing, e.g., Wilson et al 1999;Mereghetti et al 1998).…”

Section: Introductionmentioning

confidence: 99%

The Anomalous X-ray Pulsar 4U 0142+61: Variability in the infrared and a spectral break in the optical

Hulleman

Kerkwijk

Kulkarni

2004

A&A

129

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Abstract. We present new optical and infrared observations of the counterpart to the Anomalous X-ray Pulsar (AXP) 4U 0142+61 taken with the Keck I telescope. The counterpart is found to be variable in the infrared. This contrasts with our optical observations, which do not show any evidence for variability. Apart from the variability the AXP shows a remarkable spectral energy distribution. In particular, we find a sudden drop in flux going from V to B, presumably due to a spectral feature. We compare our results to those obtained for the two other securely identified AXP counterparts, to 1E 2259+586 and 1E 1048.1−5937. 4U 0142+61 is very similar to the former source in its X-ray timing and spectral properties, and we find that this similarity extends to the quiescent infrared to X-ray flux ratio. For 1E 1048.1−5937, which has different X-ray properties, the situation is less clear: in one observation, the infrared to X-ray flux ratio was much larger, but another observation gave an upper limit which is consistent with that observed for 4U 0142+61. Assuming the quiescent ratios are all similar, we estimate the optical and infrared brightnesses for the three AXPs that remain to be identified as well as for the four Soft Gamma-ray Repeaters. We also discuss briefly how the observed optical and infrared emission might arise, in particular in the context of the magnetar model.

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Anomalous X‐Ray Pulsars and Soft Gamma‐Ray Repeaters in Supernova Remnants

Cited by 170 publications

References 115 publications

The first multi-wavelength campaign of AXP 4U 0142+61 from radio to hard X-rays

The first multi-wavelength campaign of AXP 4U 0142+61 from radio to hard X-rays

A Comprehensive Study of the X‐Ray Bursts from the Magnetar Candidate 1E 2259+586

The Anomalous X-ray Pulsar 4U 0142+61: Variability in the infrared and a spectral break in the optical

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