Discovery of an X-ray Synchrotron Nebula Associated with the Radio   Pulsar PSR B1853+01 in the Supernova Remnant W44
  We report the detection using ASCA data of a hard X-ray source in the vicinity of the radio pulsar PSR B1853+01 which is located within the supernova remnant (SNR) W44. PSR B1853+01, a 267ms pulsar, has to date only been detected in the radio band. Previous observations at soft X-ray energies (e.g., with ROSAT HRI) have failed to detect any significant X-ray emission (pulsed or unpulsed) from the pulsar. Over the 0.5--4.0keV band, the ASCA data show soft thermal emission from W44 with a morphology very similar to that observed earlier by Einstein and ROSAT. In the high energy band (4.0--9.5 keV), the SNR is, for the most part, invisible, although a source coincident with the position of PSR B1853+01 is evident. The observed ASCA spectra, extracted from a region around the PSR position, are consistent with a power-law origin (photon index =~2.3) for the X-ray emission from this source at a flux level (flux density ~~0.5 10^-6 Jy at 1 keV) consistent with previous upper limits. Timing analysis of the hard X-ray source failed to detect pulsations at the pulsar's period. We conclude that the new hard source in W44 represents an X-ray synchrotron nebula associated with PSR B1853+01. 
Ilana M. Harrus, John P. Hughes, and David J. Helfand