[OII] emitters in MultiDark-Galaxies and DEEP2

We use three semi-analytical models (SAMs) of galaxy formation and evolution run on the same 1 h(-1) Gpc MultiDark Planck2 cosmological simulation to investigate the properties of [O II] emission line galaxies at redshift z similar to 1. We compare model predictions with different observational data sets, including DEEP2-FIREFLY galaxies with absolute magnitudes. We estimate the [O II] luminosity (L[O II]) of our model galaxies using the public code GET EMLINES, which ideally assumes as input the instantaneous star formation rates (SFRs). This property is only available in one of the SAMs under consideration, while the others provide average SFRs, as most models do. We study the feasibility of inferring galaxies' L[O II] from average SFRs in post-processing. We find that the result is accurate for model galaxies with dust attenuated L[O II] less than or similar to 10(42.2) erg s(-1) (< 5 per cent discrepancy). The galaxy properties that correlate the most with the model L[O II] are the SFR and the observed-frame u and g broad-band magnitudes. Such correlations have r-values above 0.64 and a dispersion that varies with L[O II]. We fit these correlations with simple linear relations and use them as proxies for L[O II], together with an observational conversion that depends on SFR and metallicity. These proxies result in [O II] luminosity functions and halo occupation distributions with shapes that vary depending on both the model and the method used to derive L[O II]. The amplitude of the clustering of model galaxies with L[O II] > 10(40.4) erg s(-1) remains overall unchanged on scales above 1 h(-1) Mpc, independently of the L[O II] computation. © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
GFandVGPacknowledge support from the University of Portsmouth through the Dennis Sciama Fellowship award. VGP acknowledges support from the European Research Council under the European Union's Horizon 2020 research and innovation programme (grant agreement No 769130). DS is funded by the Spanish Ministry of Economy and Competitiveness (MINECO) under the 2014 Severo Ochoa Predoctoral Training Programme. DS also wants to thank the Mamua Cafe Bar-team for their kind (g)astronomical support. DS and FP acknowledge funding support from the MINECO grant AYA2014-60641-C2-1-P. AO acknowledges support from the Spanish Ministerio de Economia y Competitividad (MINECO) project No. AYA2015-66211-C2-P-2, and funding from the European Union Horizon 2020 research and innovation programme under grant agreement No. 734374. SAC acknowledges funding from Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET, PIP0387), Agencia Nacional de Promocion Cientifica y Tecnologica (ANPCyT, PICT-2013-0317), and Universidad Nacional de La Plata (11-G124 and 11-G150), Argentina. CVMacknowledges CONICET, Argentina, for the supporting fellowship. AK is supported by the MINECO and the Fondo Europeo de Desarrollo Regional (FEDER, UE) in Spain through grant AYA2015-63810-P as well as by the MICIU/FEDER through grant number PGC2018-094975-C21. He further acknowledges support from the Spanish Red Consolider MultiDark FPA2017-90566-REDC and thanks Christopher Cross for sailing. ARHS acknowledges receipt of the Jim Buckee Fellowship at ICRAR-UWA. GF, VGP and DS wish to thank La Plata Astronomical Observatory for hosting the MultiDark Galaxies workshop in September 2016, during which this work was started. The authors thank the FIREFLY team and the anonymous referee for providing insightful comments. The analysis of DEEP2 data using the FIREFLY code was done on the Sciama High Performance Compute cluster which is supported by the ICG, SEPNet and the University of Portsmouth (UK). The CosmoSim database used in this paper is a service by the Leibniz-Institute for Astrophysics Potsdam (AIP). The MultiDark database was developed in cooperation with the Spanish MultiDark Consolider Project CSD200900064. The authors gratefully acknowledge the Gauss Centre for Supercomputing e.V. (www.gauss-centre.eu) and the Partnership for Advanced Supercomputing in Europe (PRACE, www.praceri.eu) for funding the MultiDark simulation project by providing computing time on the GCS Supercomputer SuperMUC at Leibniz Supercomputing Centre (LRZ, www.lrz.de).The authors thank New Mexico State University (USA) and Instituto de Astrof ' isica de Andalucia CSIC (Spain) for hosting the SKIES& UNIVERSES database for cosmological simulation products. This work has benefited from the publicly available software tools and packages: MATPLOTLIB14 2012-2016 (Hunter 2007); PYTHON SOFTWARE FOUNDATION15 19902017, version 2.7., PYTHONBREW16; we use whenever possible in this work a colour-blind friendly colour palette17 for our plots.