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   PR # 21531
    Strong optical FeII emission seems to be connected with the X-ray    
    properties of active galaxies. One model to explain the observed     
    strength of the FeII lines requires a strong, hard X-ray component   
    (irradiating an accretion disk). Relatively short ASCA observations  
    allow to establish the presence of such a component and thus to      
    assess the likelihood of the accretion disk model. One of the        
    alternatives for an explanation of the FeII emission lines could be  
    associated with a 3-6 keV temperature Raymond-Smith spectrum. It is  
    proposed to perform the ASCA observations for two objects with       
    particularly interesting properties (such as strong FeII lines, steep
    soft X-ray spectra, narrow-line Seyfert 1 spectra) for which Rosat   
   data are available.           
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