  We present a stable procedure for defining and measuring the two point
angular autocorrelation function, w, of faint (25 < V < 29), barely resolved
and unresolved sources in the HST GOODS and UDF datasets. We construct catalogs
that include close pairs and faint detections. We show for the first time that
on subarcsecond scales, the correlation function exceeds unity. This
correlation function is well fit by a power law with index of 2.5 and a
characteristic angular scale that decrease slowly with magnitude. This is very
different from the purely gravitationalcorrelation function of brighter
galaxies which has a index of 0.7 and a characteristic angular scale which
decreases quickly with magnitude. This observed clustering probably reflects
the presence of giant star-forming regions within galactic-scale potential
wells. Its measurement enables a new approach to measuring the redshift
distribution of the faintest sources in the sky.
