  The early stage in the formation of a galaxy inevitably involves a spatially
extended distribution of infalling, cold gas. If a central luminous quasar
turned on during this phase, it would result in significant extended Lyman
alpha emission, possibly accompanied by other lines. For halos condensing at
redshifts between 3 < z < 8 and having virial temperatures between 2 x 10^5 K
and 2 x 10^6 K, this emission results in a ``fuzz'' of characteristic angular
diameter of a few arcseconds, and surface brightness between 10^-18 and 10^-16
erg/s/cm^2/asec^2. The fuzz around bright, high redshift quasars could be
detected in deep narrow band imaging with current telescopes, providing a
direct constraint on galaxy formation models. The absence of detectable fuzz
might suggest that most that most of the protogalaxy's gas settles to a
self-gravitating disk before a quasar turns on. However, continued gas infall
from large radii, or an on-going merger spreading cold gas over a large solid
angle, during the luminous quasar phase could also result in extended
Ly$\alpha$ emission, and can be constrained by deep narrow band imaging.
