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    PR # 31524                                                                   
     We propose a 30 ks ASCA observation of the east part of the Cygnus Lo       
     op supernova remnant, which exhibits the brightest and softest X-ray        
      structure in the remnant. This region is strongly associated with op       
     tical emission. Our goal is to study the soft component of this gas w       
     hich is clearly linked to the interaction with the clouds. ASCA/SIS s       
     pectral resolution will allow us to determine the line ratios (as O V       
     II, O VIII, Fe XVII, Ne IX, Mg XI) and thus to distinguish between eq       
     uilibrium and non-ionization equilibrium models. Using the ASCA/SIS s       
     pectro-imaging capabilities, we will determine how the spectral varia       
     tions from place to place are linked to non-equilibrium ionization ef       
     fects and/or to underabundance of the elements.                             
                                                                                 
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