Multi-year RXTE and INTEGRAL observations crossing the magnetar-like outburst

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 also the epoch of the outburst we aim to study the temporal and spectral characterisitics 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 have been 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 20300 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/cm2s. 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 showed that the radiative outburst was triggered by a major spin-up glitch near MJD 53883 ± 3 with a glitch size ∆ν/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%. 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 Γs = 2.96 ± 0.06 and a hard component with the pre-outburst value Γh ∼ 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 10-30 keV flux increased with only 35%. After ∼ 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-Bfield 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 synchrotron emission in a slot-gap or outer-gap pulsar model.