[OII] emitters in MultiDark-Galaxies and DEEP2. (arXiv:1908.05626v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Favole_G/0/1/0/all/0/1">G. Favole</a> (ESAC), <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_Perez_V/0/1/0/all/0/1">V. Gonzalez-Perez</a> (Lancaster, Portsmouth), <a href="http://arxiv.org/find/astro-ph/1/au:+Orsi_A/0/1/0/all/0/1">A. Orsi</a> (CEFCA), <a href="http://arxiv.org/find/astro-ph/1/au:+Stoppacher_D/0/1/0/all/0/1">D. Stoppacher</a> (Madrid), <a href="http://arxiv.org/find/astro-ph/1/au:+Comparat_J/0/1/0/all/0/1">J. Comparat</a> (MPE), <a href="http://arxiv.org/find/astro-ph/1/au:+Cora_S/0/1/0/all/0/1">S. A. Cora</a> (La Plata), <a href="http://arxiv.org/find/astro-ph/1/au:+Vega_Martinez_C/0/1/0/all/0/1">C. A. Vega-Martinez</a> (La Plata), <a href="http://arxiv.org/find/astro-ph/1/au:+Stevens_A/0/1/0/all/0/1">A. R. H. Stevens</a> (ICRAR), <a href="http://arxiv.org/find/astro-ph/1/au:+Maraston_C/0/1/0/all/0/1">C. Maraston</a> (Portsmouth), <a href="http://arxiv.org/find/astro-ph/1/au:+Croton_D/0/1/0/all/0/1">D. Croton</a> (Swinburne), <a href="http://arxiv.org/find/astro-ph/1/au:+Knebe_A/0/1/0/all/0/1">A. Knebe</a> (Madrid), <a href="http://arxiv.org/find/astro-ph/1/au:+Benson_A/0/1/0/all/0/1">A. J. Benson</a> (Carnegie), <a href="http://arxiv.org/find/astro-ph/1/au:+Montero_Dorta_A/0/1/0/all/0/1">A. D. Montero-Dorta</a> (Sao Paulo), <a href="http://arxiv.org/find/astro-ph/1/au:+Padilla_N/0/1/0/all/0/1">N. Padilla</a> (PUC), <a href="http://arxiv.org/find/astro-ph/1/au:+Prada_F/0/1/0/all/0/1">F. Prada</a> (IAA), <a href="http://arxiv.org/find/astro-ph/1/au:+Thomas_D/0/1/0/all/0/1">D. Thomas</a> (Portsmouth)
We use three semi-analytic models (SAMs) of galaxy formation and evolution We use three semi-analytic models (SAMs) of galaxy formation and evolution http://arxiv.org/icons/sfx.gif
run on the same $1 h^{-1}$Gpc MultiDark Planck 2 cosmological simulation to
investigate the properties of [OII] emission line galaxies over the redshift
range $0.6
run on the same $1 h^{-1}$Gpc MultiDark Planck 2 cosmological simulation to
investigate the properties of [OII] emission line galaxies over the redshift
range $0.6<z<1.2$. We compare model predictions with different observational
data sets, including DEEP2-Firefly galaxies with absolute magnitudes. We
estimate the [OII] luminosity (L[OII]) using a public code and simple relations
derived both from the models and observations. The public code ideally uses as
input instantaneous star formation rates (SFRs), which are only provided by one
of the SAMs under study. We use this SAM to study the feasibility of inferring
galaxies’ L[OII] for models that only provide SFRs averaged across full
snapshot intervals. We find that the L[OII] post-processing computation from
average SFRs is accurate for model galaxies with
log(L[OII]/$rm{erg,s^{-1}}$)$lesssim42.5$ ($<5$% discrepancy). We also
explore how to derive the [OII] luminosity from simple relations using the
global properties that are usually output by SAMs. Besides the SFR, the model
L[OII] is best correlated with the observed-frame $u$ and $g$ broad-band
magnitudes. These correlations have coefficients (r-values) above 0.65 and a
dispersion that varies with L[OII]. We use these correlations and an
observational one based on SFR and metallicity to derive L[OII]. Using these
simple relations result in [OII] luminosity functions with shapes that vary
depending on both the model and the method used. Nevertheless, for two of the
three studied models, the amplitude of the clustering at scales above
$1h^{-1}$Mpc remains unchanged independently of the method used to derived the
L[OII].
