  We examine the impact of fiber assignment on clustering measurements from
fiber-fed spectroscopic galaxy surveys. We identify new effects which were
absent in previous, relatively shallow galaxy surveys such as Baryon
Oscillation Spectroscopic Survey . Specifically, we consider deep surveys
covering a wide redshift range from z=0.6 to z=2.4, as in the Subaru Prime
Focus Spectrograph survey. Such surveys will have more target galaxies than we
can place fibers on. This leads to two effects. First, it eliminates
fluctuations with wavelengths longer than the size of the field of view, as the
number of observed galaxies per field is nearly fixed to the number of
available fibers. We find that we can recover the long-wavelength fluctuation
by weighting galaxies in each field by the number of target galaxies. Second,
it makes the preferential selection of galaxies in under-dense regions. We
mitigate this effect by weighting galaxies using the so-called individual
inverse probability. Correcting these two effects, we recover the underlying
correlation function at better than 1 percent accuracy on scales greater than
10 Mpc/h.
