Universal conditional distribution function of [OII] luminosity of
  galaxies, and prediction for the [OII] luminosity function at redshift $z<3$
  The star-forming emission line galaxies (ELGs) with strong [OII] doublet are
one of the main spectroscopic targets for the ongoing and upcoming fourth
generation galaxy redshift surveys. In this work, we measure the [OII]
luminosity $L_{\mathrm{[OII]}}$ and the near-ultraviolet band absolute
magnitude $M_{\mathrm{NUV}}$ for a large sample of galaxies in the redshift
range of $0.6\leq z <1.45$ from the Public Data Release 2 (PDR-2) of the VIMOS
Public Extragalactic Redshift Survey (VIPERS). We aim to construct the
intrinsic relationship between the $L_{\mathrm{[OII]}}$ and $M_{\mathrm{NUV}}$
through Bayesian analysis. In particular, we develop two different methods to
properly correct for the incompleteness effect and observational errors in the
[OII] emission line measurement. Our results indicate that the conditional
distribution of $L_{\mathrm{[OII]}}$ at a given $M_{\mathrm{NUV}}$ can be well
described by a universal probability distribution function (PDF), which is
independent of $M_{\mathrm{NUV}}$ or redshift. Convolving the
$L_{\mathrm{[OII]}}$ conditional PDF with the NUV Luminosity function (LF)
available in the literature, we make a prediction for [OII] LFs at $z<3$. The
predicted [OII] LFs are in good agreement with the observational results from
the literature. Finally, we utilize the predicted [OII] LFs to estimate the
number counts of [OII] emitters for the Subaru Prime Focus Spectrograph (PFS)
survey. This universal conditional PDF of $L_{\mathrm{[OII]}}$ provides a novel
way to optimize the source targeting strategy for [OII] emitters in future
galaxy redshift surveys, and to model [OII] emitters in theories of galaxy
formation.
