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PSR J1119-6127 is a radio pulsar that behaved magnetar like bursts, and weperformed a comprehensive investigation of this pulsar using the archivalhigh-energy observations obtained after its outburst in 2016 July. After the2016 outburst, specific regions on the neutron star surface were heated up to >0.3 and > 1 keV from about 0.2 keV. A hard non-thermal spectral component witha photon index < 0.5 related to the magnetospheric emission can be resolvedfrom the NuSTAR spectra above 10 keV. We find that the thermal emitting regionsdid not cool down and gradually shrank by about (20-35)% four months after theoutburst. Hard X-ray pulsations were detected with NuSTAR immediately after theoutburst, at 5 sigma confidence level and with a background-subtracted pulsedfraction of (40+-10)%. However, the signal became undetectable after a fewdays. Using Fermi data, we found that the gamma-ray emission in 0.5-300 GeV wassuppressed along with the disappearance of the radio pulsations. This is likelycaused by a reconfiguration of the magnetic field. We also discovered that thetiming noise evolved dramatically, and the spin-down rate significantlyincreased after the 2016 glitch. We proposed that post-outburst temporal andspectral behaviors from radio to gamma-ray bands were caused by changes of themagnetosphere structure, pair plasma injection and the shrinking emission siteson the neutron star.

Investigation of the High-Energy Emission from the Magnetar-like Pulsar PSR J1119-6127 after the 2016 Outburst