High Energy Pulsations from PSR J2022+3842

PSR J2022+3842 is a young, energetic pulsar with a characteristic age of 8.9 kyr and spin down power 3.0 x 10³⁷ erg s^-1 . Located in supernova remnant G76.9+1.0, and spatially coincident with a Fermi LAT source, pulsations with a period of ~48.6 ms have been reported in radio by the GBT, as well in the X-ray band by Chandra, RXTE, and XMM-Newton. Large amounts of timing noise typical of young pulsars combined with the radio-faint nature of this pulsar makes deriving a global timing solution that smoothly connects all individual observations challenging. Analysis with the Fermi LAT, although complicated by high levels of background in the surrounding Cygnus region, can help bridge these gaps. In this work we present an analysis of data from NuSTAR and NICER showing strong pulsations from PSR J2022+3842 in the 3-79 keV and 0.5-12 keV energy ranges, respectively. Analyzing over 10 years of Pass 8 LAT data at energies > 60 MeV, we confirm a previous tentative detection of this gamma-ray pulsar. Using the combined X-ray, radio, and gamma-ray observations, we study its properties in the context of other young pulsars, with a particular interest in comparing PSR J2022+3842 to soft gamma-ray pulsars.