[CII] line intensity mapping the epoch of reionization with the
  Prime-Cam on FYST
  We predict the three-dimensional intensity power spectrum (PS) of the [CII]
158$\,\mu$m line throughout the epoch of (and post) reionization at redshifts
from $\approx$ 3.5 to 8. We study the detectability of the PS in a line
intensity mapping (LIM) survey with the Fred Young Submillimeter Telescope
(FYST).
  We created mock [CII] tomographic scans in redshift bins at $z\approx$ 3.7,
4.3, 5.8, and 7.4 using the Illustris TNG300-1 $\Lambda$CDM simulation and
adopting a relation between the star formation activity and the [CII]
luminosity ($L_{[CII]}$) of galaxies. A star formation rate (SFR) was assigned
to a dark matter halo in the Illustris simulation in two ways: (i) we adopted
the SFR computed in the Illustris simulation and, (ii) we matched the abundance
of the halos with the SFR traced by the observed dust-corrected ultraviolet
luminosity function of high-redshift galaxies. The $L_{[CII]}$ is related to
the SFR from a semi-analytic model of galaxy formation, from a hydrodynamical
simulation of a high-redshift galaxy, or from a high-redshift [CII] galaxy
survey. The [CII] intensity PS was computed from mock tomographic scans to
assess its detectability with the anticipated observational capability of the
FYST.
  The amplitude of the predicted [CII] intensity power spectrum varies by more
than a factor of 10, depending on the choice of the halo-to-galaxy SFR and the
SFR-to-$L_{[CII]}$ relations. In the planned $4^{\circ} \times 4^{\circ}$ FYST
LIM survey, we expect a detection of the [CII] PS up to $z \approx$ 5.8, and
potentially even up to $z \approx $ 7.4. The design of the envisioned FYST LIM
survey enables a PS measurement not only in small (<10 Mpc) shot
noise-dominated scales, but also in large (>50 Mpc) clustering-dominated scales
making it the first LIM experiment that will place constraints on the
SFR-to-$L_{[CII]}$ and the halo-to-galaxy SFR relations simultaneously.
