The clustering of H$\beta$+[OIII] and [OII] emitters since $z \sim 5$:
  dependencies with line luminosity and stellar mass
  We investigate the clustering properties of $\sim 7000$ H$\beta$+[OIII] and
[OII] narrowband-selected emitters at $z \sim 0.8 - 4.7$ from the High-$z$
Emission Line Survey. We find clustering lengths, $r_0$, of $1.5 - 4.0h^{-1}$
Mpc and minimum dark matter halo masses of $10^{10.7 - 12.1}\rm{M}_\odot$ for
our $z = 0.8 - 3.2$ H$\beta$+[OIII] emitters and $r_0 \sim 2.0 - 8.3h^{-1}$ Mpc
and halo masses of $10^{11.5 - 12.6}\rm{M}_\odot$ for our $z = 1.5 - 4.7$ [OII]
emitters. We find $r_0$ to strongly increase both with increasing line
luminosity and redshift. By taking into account the evolution of the
characteristic line luminosity, $L^\star(z)$, and using our model predictions
of halo mass given $r_0$, we find a strong, redshift-independent increasing
trend between $L/L^\star(z)$ and minimum halo mass. The faintest
H$\beta$+[OIII] emitters are found to reside in $10^{9.5}\rm{M}_\odot$ halos
and the brightest emitters in $10^{13.0}\rm{M}_\odot$ halos. For [OII]
emitters, the faintest emitters are found in $10^{10.5} \rm{M}_\odot$ halos and
the brightest emitters in $10^{12.6}\rm{M}_\odot$ halos. A redshift-independent
stellar mass dependency is also observed where the halo mass increases from
$10^{11}\rm{M}_\odot$ to $10^{12.5} \rm{M}_\odot$ for stellar masses of
$10^{8.5}\rm{M}_\odot$ to $10^{11.5}\rm{M}_\odot$, respectively. We investigate
the interdependencies of these trends by repeating our analysis in a
$L_\textrm{line} - \rm{M}_\textrm{star}$ grid space for our most populated
samples (H$\beta$+[OIII] $z = 0.84$ and [OII] $z = 1.47$) and find that the
line luminosity dependency is stronger than the stellar mass dependency on halo
mass. For $L > L^\star$ emitters at all epochs, we find a relatively flat trend
with halo masses of $10^{12.5 - 13}\rm{M}_\odot$ which may be due to quenching
mechanisms in massive halos which is consistent with a transitional halo mass
predicted by models.
