ASCA data analysis of the young supernova remnant G41.1-0.3 Original Research Article

We fit the ASCA SIS spectral data of SNR G41.1-0.3 with both a two-component NEI model and an EI model. Hard (≳ 2 keV) X-ray emission arises essentially from the hot component, containing S and Fe K lines. The cool component, which was found to be arriving at an ionization equilibrium, generates mainly Mg, Si, Fe L lines, and continuum, contributing essentially to the soft emission. The high emission measure of the cool component suggests that the remnant evolves in a cloudy medium. We did not find powerlaw, bremsstrahlung, and blackbody components, as well as pulsed signals. the ASCA SIS images were restored and compared with the ROSAT HRI and 20cm VLA maps. The X-ray image might suggest a bipolar structure for the remnant that encounters a denser medium in the west. Relevant parameters of the remnant were derived.