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journal id: "astronomyxandxastrophysics"
| Authors||L. Kuiper, W. Hermsen|
|Title||High-energy characteristics of the schizophrenic pulsar PSR J1846-0258 in Kes 75. Multi-year RXTE and INTEGRAL observations crossing the magnetar-like outburst|
|Journal||Astronomy and Astrophysics|
|Faculty||Faculty of Science|
|Institute/dept.||FNWI: Astronomical Institute Anton Pannekoek (IAP)|
|Abstract||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 similar to 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 (similar to 3-30 keV), RXTE HEXTE (similar to 15-250 keV) and INTEGRAL ISGRI (similar to 20-300 keV). The pulsed spectrum over the full similar to 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 PSRJ1846-0258/Kes-75 before outburst during 2003-2006 with a power-law-shape spectrum over the 20300 keV energy range with photon index Gamma = 1.80 +/- 0.06 and energy flux (20-300 keV) of (6.62 +/- 0.35) x 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 (Gamma = 1.75(-0.31)(+ 0.27) - 0.31) with an indication for a 52% (2.3 sigma) 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 Delta nu/nu in the range (2.0-4.4) x 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 similar to 3-300 keV pulsed spectrum measured with the PCA, HEXTE, and ISGRI was fitted with a power-law model with Gamma = 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 magnetar-like outburst, the 3-30 keV pulsed spectrum can be represented with two power laws, a soft component with index Gamma(s) = 2.96 +/- 0.06 and a hard component with the pre-outburst value Gamma(h) similar to 1.2. Above similar to 9 keV, all spectra during outburst are consistent with the latter single power-law shape with index similar to 1.2. The 2-10 keV flux increased by a factor similar to 5 and the 10-30 keV flux increased with only 35%. After similar to 120 days the soft outburst and the enhancement of the hard non-thermal component both vanish.
Conclusions. The varying temporal and spectral characteristics of PSR J1846-0258 can be explained in a scenario of a young high-B-field pulsar in which a major glitch triggered a sudden release of energy. Resonant cyclotron upscattering could subsequently generate the decaying/cooling soft pulsed component measured during outburst between 3 and 10 keV. The (variation in the) non-thermal hard X-ray component can be explained with synchr|
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