Possible evidence for extended X-ray emission surrounding PSR B0656+14 with eROSITA

Abstract

Extended very-high-energy ${\hat{I}}^3$-ray emission from middle-aged pulsars as revealed recently by several groundbased ${\hat{I}}^3$-ray experiments has strong implication on the transport of high-energy particles in the interstellar medium surrounding those pulsars. The ${\hat{I}}^3$-ray emission is widely believed to be produced by high-energy electrons and positrons accelerated by the pulsar wind nebulae when scattering off the interstellar radiation field via the inverse Compton process. Consequently, multiwavelength counterparts of the ${\hat{I}}^3$-ray halos are expected to be present, which have not yet been detected. In this work we report the possible detection of extended X-ray emission from a $\sim 0.2\degr$ radius region around PSR B0656+14 with eROSITA. In spite that there are uncertainties of the on-orbit point spread function of the pointing mode, the radial profile of PSR B0656+14 is found to be broader than that of a star at similar observational conditions, indicating that emission is possibly from the expected extended halo around the pulsar. The spectrum of the emission can be described by a power-law function with an index of $\sim 3.7$. Its surface brightness declines with radius faster than the prediction of the particle diffusion and synchrotron radiation in a uniform magnetic field, suggesting the existence of a radial gradient of the magnetic field strength as $\sim r^{-1}$. The magnetic field strength in the X-ray emitting region is constrained to be $4-10\hat{I}¼$G.

21 pages, 3+8 figures, 1+1 tables; Published in ApJ