Galaxy clustering dependence on the
  $\left[\mathrm{O\scriptsize{II}}\right]$ emission line luminosity in the
  local Universe
  We study the galaxy clustering dependence on the
$\left[\mathrm{O\scriptsize{II}}\right]$ emission line luminosity in the SDSS
DR7 Main galaxy sample at mean redshift $z\sim0.1$. We select volume-limited
samples of galaxies with different $\left[\mathrm{O\scriptsize{II}}\right]$
luminosity thresholds and measure their projected, monopole and quadrupole
two-point correlation functions. We model these observations using the
1$h^{-1}\rm{Gpc}$ MultiDark Planck cosmological simulation and generate
light-cones with the SUrvey GenerAtoR algorithm. To interpret our results, we
adopt a modified (Sub)Halo Abundance Matching scheme, accounting for the
stellar mass incompleteness of the emission line galaxies. The satellite
fraction constitutes an extra parameter in this model and allows to optimize
the clustering fit on both small and intermediate scales (i.e. $r_p\lesssim
30h^{-1}\rm{Mpc})$, with no need of any velocity bias correction. We find that,
in the local Universe, the $\left[\mathrm{O\scriptsize{II}}\right]$ luminosity
correlates with all the clustering statistics explored and with the galaxy
bias. This latter quantity correlates more strongly with the SDSS $r$-band
magnitude than $\left[\mathrm{O\scriptsize{II}}\right]$ luminosity. In
conclusion, we propose a straightforward method to produce reliable clustering
models, entirely built on the simulation products, which provides robust
predictions of the typical ELG host halo masses and satellite fraction values.
The SDSS galaxy data, MultiDark mock catalogues and clustering results are made
publicly available.
