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   PR # 22121
    We show that the hot, wind-shocked cavities in ultracompact (UC) HII 
    regions can produce strong Fe XXV 6.7 keV line emission.  The        
    observed z-scale height and longitude distribution of 6.7 keV line   
    emission from the galactic disk accurately match those of UC HII     
    regions and the predicted line fluxes are similar to the observed    
    values.  We propose to measure the 6.7 keV Fe line and continuum     
    emission toward two isolated UC HII regions with the ASCA satellite  
    using the SIS and GIS detectors.  The main goals are to identify a   
    possible source of the 6.7 keV line emission and to use the observed 
    high S/N spectra to develop empirical models of the hot, wind-shocked
    central cavities of UC HII regions.                                  
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