1E 1547.0-5408: A Radio-emitting Magnetar with a Rotation Period of 2 Seconds

Camilo, F.; Ransom, S. M.; Halpern, J. P.; Reynolds, John E.

doi:10.1086/521826

Cited by 302 publications

(404 citation statements)

References 32 publications

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“…1E 1547.0-5408 was undetected in previous archival radio observations (starting from 1998), implying a flux at least 5 times lower then that recorded in 2008, and consequently suggesting a transient behaviour for the source also at radio wavelengths (F 2008 1.4 GHz = 2.5 ± 0.5 mJy, F 1998 1.4 GHz ≤ 0.5 mJy). The source distance derived from the dispersion measure (Camilo et al 2007) was ∼9 kpc, larger than the value of 4-5 kpc previously proposed by Gelfand & Gaensler (2007) on the basis of a possible association with G327.24−0.13.…”

Section: Introductioncontrasting

confidence: 60%

“…Using data collected in June 2007 with the Parkes radio telescope and the Australia Telescope Compact Array, Camilo et al (2007) unambiguously revealed the magnetar nature of the source, by measuring the spin period and period derivative, P ∼ 2.069 s andṖ ∼ 2.3 × 10 −11 s s −1 . 1E 1547.0-5408 was undetected in previous archival radio observations (starting from 1998), implying a flux at least 5 times lower then that recorded in 2008, and consequently suggesting a transient behaviour for the source also at radio wavelengths (F 2008 1.4 GHz = 2.5 ± 0.5 mJy, F 1998 1.4 GHz ≤ 0.5 mJy).…”

Section: Introductionmentioning

confidence: 99%

“…1E 1547.0-5408 is one of two sources in the magnetar class (the other is XTE J1810−197), which showed transient pulsed radio emission during its outburst (Helfand et al 2006;Camilo et al 2006Camilo et al , 2007Burgay et al 2009). Using data collected in June 2007 with the Parkes radio telescope and the Australia Telescope Compact Array, Camilo et al (2007) unambiguously revealed the magnetar nature of the source, by measuring the spin period and period derivative, P ∼ 2.069 s andṖ ∼ 2.3 × 10 −11 s s −1 .…”

Section: Introductionmentioning

confidence: 99%

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

Bernardini¹,

Israel²,

Stella³

et al. 2011

A&A

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Context. With two consecutive outbursts recorded in four months (October 2008 and January 2009), and a possible third outburst in 2007, 1E 1547.0-5408 is one of the most active transient anomalous X-ray pulsars known so far. Aims. Thanks to extensive X-ray observations, obtained both in the quiescent and active states, 1E 1547.0-5408 represents a very promising laboratory to gain insight into the outburst properties and magnetar emission mechanisms. Methods. We performed a detailed timing and spectral analysis of four Chandra, three INTEGRAL, and one XMM-Newton observations collected over a two week interval after the outburst onset in January 2009. Several Swift pointings, covering a 1.5 year interval, were also analyzed in order to monitor the decay of the X-ray flux. Results. We compare the characteristics of the two outbursts, as well as those of the active and quiescent states. We also discuss the long-term X-ray flux history of 1E 1547.0-5408 since its first detection in 1980, and show that the source displays three flux levels: low, intermediate and high.

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Section: Introductioncontrasting

confidence: 60%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

Bernardini¹,

Israel²,

Stella³

et al. 2011

A&A

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“…The lack of persistent radio emission above 500 MHz (Istomin & Sobyanin 2007;Lazarus et al 2012) and the transient, highly-variable radio emission observed from a subset of these objects (Camilo et al 2007;Malov 2014) suggests that the density of plasma in the magnetospheres of magnetars is lower than in normal radio pulsars (Istomin & Sobyanin 2007;Malov 2014). While gravitational effects are expected to dominate photon trajectories outside of magnetars (Heyl & Shaviv 2002;Kim 2012), it is generally believed that plasma effects should also become important deep within magnetar atmospheres (Lai & Ho 2003).…”

Section: Discussionmentioning

confidence: 99%

Frequency-dependent effects of gravitational lensing within plasma

Rogers

2015

Monthly Notices of the Royal Astronomical Society

117

120

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The interaction between refraction from a distribution of inhomogeneous plasma and gravitational lensing introduces novel effects to the paths of light rays passing by a massive object. The plasma contributes additional terms to the equations of motion, and the resulting ray trajectories are frequency-dependent. Lensing phenomena and circular orbits are investigated for plasma density distributions N ∝ 1/r h with h ≥ 0 in the Schwarzschild space-time. For rays passing by the mass near the plasma frequency refractive effects can dominate, effectively turning the gravitational lens into a mirror. We obtain the turning points, circular orbit radii, and angular momentum for general h. Previous results have shown that light rays behave like massive particles with an effective mass given by the plasma frequency for a constant density h = 0. We study the behaviour for general h and show that when h = 2 the plasma term acts like an additional contribution to the angular momentum of the passing ray. When h = 3 the potential and radii of circular orbits are analogous to those found in studies of massless scalar fields on the Schwarzschild background. As a physically motivated example we study the pulse profiles of a compact object with antipodal hotspots sheathed in a dense plasma, which shows dramatic frequency-dependent shifts from the behaviour in vacuum. Finally, we consider the potential observability and applications of such frequency-dependent plasma effects in general relativity for several types of neutron star.

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“…However, no radio detections of all the other transient AXPs/SGRs have been obtained yet. The pulsed radio emission of AXPs/ SGRs is quite different from that of radio pulsars: they show strong variability on daily timescales, their spectra are very flat with α >-0.5 (where S ν ∝ ν α ), and their average pulse profiles change with time [20,17,19]. Such differences suggest that the radio emitting regions are more complex than the dipolar open field lines along which the radio emission in normal pulsars is thought to originate.…”

Section: Observational Propertiesmentioning

confidence: 97%

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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1E 1547.0-5408: A Radio-emitting Magnetar with a Rotation Period of 2 Seconds

Abstract: The variable X-ray source 1E 1547

Cited by 302 publications

References 32 publications

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

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

Frequency-dependent effects of gravitational lensing within plasma

Pulsars and Magnetars

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