Detailed high-energy characteristics of AXP 1RXS J170849-400910

Hartog, P. R. den; Kuiper, L.; Hermsen, W.

doi:10.1051/0004-6361:200809772

Cited by 71 publications

(53 citation statements)

References 69 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Another piece of evidence for the AXP‐like behaviour of SGR 0501+4516 and the SGR‐like behaviour of 1E 1547.0−5408 is the photon index of the variable hard X‐ray component. As shown in , the photon index we measure from the INTEGRAL spectrum is Γ∼ 0.8, which is close to the one reported for AXPs, while the variable hard X‐ray emission during the 2009 January outburst of 1E 1547.0−5408 has a photon index of Γ∼ 1.4–1.6 (den Hartog, Kuiper & Hermsen 2009), typical of SGRs.…”

Section: Discussionsupporting

confidence: 85%

The first outburst of the new magnetar candidate SGR 0501+4516

Rea¹,

Israel²,

Turolla³

et al. 2009

Monthly Notices of the Royal Astronomical Society

110

124

View full text Add to dashboard Cite

We report here on the outburst onset and evolution of the new soft gamma‐ray repeater SGR 0501+4516. We monitored the new SGR with XMM–Newton starting on 2008 August 23, 1 day after the source became burst active, and continuing with four more observations in the following month, with the last one on 2008 September 30. Combining the data with the Swift X‐ray telescope (Swift–XRT) and Suzaku data, we modelled the outburst decay over a 3‐month period, and we found that the source flux decreased exponentially with a time‐scale of tc= 23.8 d. In the first XMM–Newton observation, a large number of short X‐ray bursts were observed, the rate of which decayed drastically in the following observations. We found large changes in the spectral and timing behaviour of the source during the first month of the outburst decay, with softening emission as the flux decayed, and the non‐thermal soft X‐ray spectral component fading faster than the thermal one. Almost simultaneously to our second and fourth XMM–Newton observations (on 2008 August 29 and September 2), we observed the source in the hard X‐ray range with INTEGRAL, which clearly detected the source up to ∼100 keV in the first pointing, while giving only upper limits during the second pointing, discovering a variable hard X‐ray component fading in less than 10 days after the bursting activation. We performed a phase‐coherent X‐ray timing analysis over about 160 days starting with the burst activation and found evidence of a strong second derivative period component []. Thanks to the phase connection, we were able to study the phase‐resolved spectral evolution of SGR 0501+4516 in great detail. We also report on the ROSAT quiescent source data, taken back in 1992 when the source exhibits a flux ∼80 times lower than that measured during the outburst, and a rather soft, thermal spectrum.

show abstract

Section: Discussionsupporting

confidence: 85%

The first outburst of the new magnetar candidate SGR 0501+4516

Rea¹,

Israel²,

Turolla³

et al. 2009

Monthly Notices of the Royal Astronomical Society

110

124

View full text Add to dashboard Cite

show abstract

“…The soft component can plausibly be explained with a resonant cyclotron scattering origin. The hard non-thermal power-law spectra of 4U 0142+61 and 1RXS J170849-400910 have been measured with INTEGRAL up to ∼200 keV and could have a similar origin in the outer magnetosphere as the hard non-thermal X-ray spectra measured for young radio pulsars, as has been discussed in den Hartog et al (2008b). Furthermore, and most interestingly, we found that during the outburst the pulse profile in this energy range below ∼9 keV, while completely dominated by the soft flux enhancement, is identical to the pulse profile before and after the outburst when the emission was purely non-thermal (Fig.…”

Section: Magnetar-like Outburst Below 10 Kevsupporting

confidence: 54%

High-energy characteristics of the schizophrenic pulsar PSR J1846-0258 in Kes 75

Kuiper

Hermsen

2009

A&A

Self Cite

View full text Add to dashboard Cite

Aims. PSR J1846−0258 is a young rotation-powered pulsar with one of the highest surface magnetic field strengths, located in the centre of SN-remnant Kes-75. In June 2006 a magnetar-like outburst took place. Using multi-year RXTE and INTEGRAL observations covering the epoch of the outburst, we aim to study the temporal and spectral characteristics of PSR J1846−0258 over a broad ∼3-300 keV energy range to derive constraints on theoretical scenarios aiming to explain this schizophrenic behaviour. Methods. We explored all publically available RXTE observations of PSR J1846−0258 to generate accurate ephemerides over the period January 30, 2000-November 7, 2007. Phase-folding procedures yielded pulse profiles for RXTE PCA (∼3-30 keV), RXTE HEXTE (∼15-250 keV) and INTEGRAL ISGRI (∼20-300 keV). The pulsed spectrum over the full ∼3-300 keV energy range was derived, as well as the total spectrum (including the pulsar wind nebula) over the 20-300 keV band with the ISGRI. The timing, spatial, and spectral analyses were applied for epochs before, during, and after the magnetar-like outburst to study the evolution of the high-energy characteristics. Results. ISGRI detected PSR J1846−0258/Kes-75 before outburst during 2003-2006 with a power-law-shape spectrum over the 20-300 keV energy range with photon index Γ = 1.80 ± 0.06 and energy flux (20-300 keV) of (6.62 ± 0.35) × 10 −11 erg/cm 2 s. More than 90 days after the onset of the outburst, still during the decay phase, the same spectral shape was measured (Γ = 1.75 +0.27 −0.31 ) with an indication for a 52% (2.3σ) enhanced total emission, while one year after the outburst the hard X-ray non-thermal emission of PSR J1846−0258/Kes-75 was found to be back to its pre-outburst values. PCA monitoring of PSR J1846−0258 before the outburst yielded phase-coherent ephemerides confirming the earlier derived breaking index of the spindown. During the outburst, incoherent solutions have been derived. We show that the radiative outburst was triggered by a major spin-up glitch near MJD 53 883 ± 3 with a glitch size Δν/ν in the range (2.0−4.4) × 10 −6 . Using all pre-outburst observations of ISGRI and HEXTE for the first time pulse profiles have been obtained up to 150 keV with a broad single asymmetric pulse. The pulse shape did not vary with energy over the 2.9-150 keV energy range, nor did it change during the magnetar-like outburst. The time-averaged pre-outburst ∼3-300 keV pulsed spectrum measured with the PCA, HEXTE, and ISGRI was fitted with a power-law model with Γ = 1.20 ± 0.01. A fit with a curved power-law model gives an improved fit. Around 150 keV the pulsed fraction approaches 100%. For the first 32 days of the magnetarlike outburst, the 3-30 keV pulsed spectrum can be represented with two power laws, a soft component with index Γ s = 2.96 ± 0.06 and a hard component with the pre-outburst value Γ h ∼ 1.2. Above ∼9 keV, all spectra during outburst are consistent with the latter single power-law shape with index ∼1.2. The 2-10 keV flux increased by a factor ∼5 and the 10...

show abstract

“…Such double-peaked pulse profiles are occasionally seen in the hard X-ray tails of magnetars for certain energy bands -see for example Kuiper et al, 2004, for RXTE/HEXTE data above 50 keV for 1E 1841-045; den Hartog et al 2008a for 4U 0142+61 in the window 20-50 keV; and An et al, 2013An et al, , 2015 for NuSTAR data between 24 keV and 35 keV on 1E 1841-045. Generally, such bifurcated peaks are either poorly resolved or completely absent in magnetar pulse profiles above 10 keV.…”

Section: Upscattering Emission From Toroidal Surfaces Of Field Linesmentioning

confidence: 96%

Resonant Inverse Compton Scattering Spectra from Highly Magnetized Neutron Stars

Wadiasingh

Baring

Gonthier

et al. 2018

ApJ

View full text Add to dashboard Cite

Hard, non-thermal, persistent pulsed X-ray emission extending between 10 keV and ∼ 150 keV has been observed in nearly ten magnetars. For inner-magnetospheric models of such emission, resonant inverse Compton scattering of soft thermal photons by ultra-relativistic charges is the most efficient production mechanism. We present angle-dependent upscattering spectra and pulsed intensity maps for uncooled, relativistic electrons injected in inner regions of magnetar magnetospheres, calculated using collisional integrals over field loops. Our computations employ a new formulation of the QED Compton scattering cross section in strong magnetic fields that is physically correct for treating important spindependent effects in the cyclotron resonance, thereby producing correct photon spectra. The spectral cut-off energies are sensitive to the choices of observer viewing geometry, electron Lorentz factor, and scattering kinematics. We find that electrons with energies < ∼ 15 MeV will emit most of their radiation below 250 keV, consistent with inferred turnovers for magnetar hard X-ray tails. More energetic electrons still emit mostly below 1 MeV, except for viewing perspectives sampling field line tangents. Pulse profiles may be singly-or doubly-peaked dependent upon viewing geometry, emission locale, and observed energy band. Magnetic pair production and photon splitting will attenuate spectra to hard X-ray energies, suppressing signals in the Fermi-LAT band. The resonant Compton spectra are strongly polarized, suggesting that hard X-ray polarimetry instruments such as X-Calibur, or a future Compton telescope, can prove central to constraining model geometry and physics.

show abstract

Detailed high-energy characteristics of AXP 1RXS J170849-400910

Cited by 71 publications

References 69 publications

The first outburst of the new magnetar candidate SGR 0501+4516

The first outburst of the new magnetar candidate SGR 0501+4516

High-energy characteristics of the schizophrenic pulsar PSR J1846-0258 in Kes 75

Resonant Inverse Compton Scattering Spectra from Highly Magnetized Neutron Stars

Contact Info

Product

Resources

About