  The possibility of detecting proto-galaxies in the UV band is pointed out,
assuming that galaxy formation occured at z $\sim 5-6$. It is shown that the
diffuse gas in collapsing galaxy sized objects with temperatures $\sim
10^{6\pm0.5}$ K, and with a modest amount of metallicity, should copiously
produce emission lines from highly ionized Iron atoms. The expected luminosity
from models of galaxy formation is compared with the sensitivity of HST.
