Empowering line intensity mapping to study early galaxies
  Line intensity mapping is a superb tool to study the collective radiation
from early galaxies. However, the method is hampered by the presence of strong
foregrounds, mostly produced by low-redshift interloping lines. We present here
a general method to overcome this problem which is robust against foreground
residual noise and based on the cross-correlation function $\psi_{\alpha L}(r)$
between diffuse line emission and Ly$\alpha$ emitters (LAE). We compute the
diffuse line (Ly$\alpha$ is used as an example) emission from galaxies in a
$(800{\rm Mpc})^3$ box at $z = 5.7$ and $6.6$. We divide the box in slices and
populate them with $14000(5500)$ LAEs at $z = 5.7(6.6)$, considering duty
cycles from $10^{-3}$ to $1$. Both the LAE number density and slice volume are
consistent with the expected outcome of the Subaru HSC survey. We add gaussian
random noise with variance $\sigma_{\rm N}$ up to 100 times the variance of the
Ly$\alpha$ emission, $\sigma_\alpha$, to simulate foregrounds and compute
$\psi_{\alpha L}(r)$. We find that the signal-to-noise of the observed
$\psi_{\alpha L}(r)$ does not change significantly if $\sigma_{\rm N} \le 10
\sigma_\alpha$ and show that in these conditions the mean line intensity,
$I_{Ly\alpha}$, can be precisely recovered independently of the LAE duty cycle.
Even if $\sigma_{\rm N} = 100 \sigma_\alpha$, $I_\alpha$ can be constrained
within a factor $2$. The method works equally well for any other line (e.g. HI
21 cm, [CII], HeII) used for the intensity mapping experiment.
