X-ray observation and analysis of the composite supernova remnant G327.1-1.1

Based on the data from the observation of the supernova remnant (SNR) G327. 1-1.1 by the Advanced Satellite for Cosmology and Astrophysics (ASCA) and R OSAT, we find that G327.1-1.1 is a composite remnant with both a nonthermal emission component and a diffuse thermal emission component. The nontherma l component is well fitted by a power-law model with photon index Gamma sim ilar to 2.2. This component is attributed to the emission from the synchrot ron nebula powered by an undiscovered central pulsar. The thermal component has a temperature of about 0.4 keV. We attribute it to the emission from t he shock-heat swept-up interstellar medium (ISM). Its age, explosion energy , and density of ambient medium are derived from the observed thermal compo nent. Some characteristics of the synchrotron nebula are also derived. We h ave searched for the pulsed signal but have not found it. The soft X-ray (0 .4-2 keV) and hard X-ray (2-10 keV) images are different, but they both elo ngate in the southeast-northwest direction. And this X-ray southeast-northw est elongation is in positional coincidence with the radio ridge in the Mol onglo Observatory Synthesis Telescope (MOST) 843 MHz radio map. We present a possibility that the X-ray nonthermal emission mainly comes from the trai l produced by a quickly moving undiscovered pulsar, and the long radio ridg e is formed when the pulsar is moving out of the boundary of the plerionic structure.