[O ii] emitters in MultiDark-Galaxies and DEEP2

• Autores: Favole, G; González Pérez, Carlos Federico; Stoppacher, D; Orsi, Á; Comparat, J; Cora, Sofia Alejandra; Vega Martínez, Cristian Antonio; Stevens, A. R. H.; Maraston, C.; Croton, D.; Knebe, A.; Benson, Silvia; Montero Dorta, A. D.; Padilla, Natalia Soledad; Prada, Federico; Thomas, Pablo Daniel
• Año de publicación: 2020
• Idioma: inglés
• Tipo de recurso: artículo
• Materia: galaxies: distances and redshifts; galaxies: haloes; galaxies: statistics; large-scale structure of Universe; cosmology: observations; cosmology: theory
• Institución: Consejo Nacional de Investigaciones Científicas y Técnicas

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 ∼ 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] 1042.2 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] >1040.4 erg s−1 remains overall unchanged on scales above 1 h−1 Mpc, independently of the L[O II] computation.
Fil: Favole, G. Institute Of Cosmology And Gravitation; Reino Unido
Fil: González Pérez, Carlos Federico. Institute Of Cosmology And Gravitation; Reino Unido
Fil: Stoppacher, D. Universidad Autónoma de Madrid; España
Fil: Orsi, Á. Centro de Estudios de Fisica del Cosmos de Aragon; España
Fil: Comparat, J. Max-planck-institut F¨ur Extraterrestrische Physik; Alemania
Fil: Cora, Sofia Alejandra. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Vega Martínez, Cristian Antonio. Universidad de La Serena; Chile
Fil: Stevens, A. R. H.. International Centre For Radio Astronomy Research; Australia
Fil: Maraston, C.. Institute Of Cosmology And Gravitation; Reino Unido
Fil: Croton, D.. Centre For Astrophysics And Supercomputing, Swinburne; Australia
Fil: Knebe, A.. Departamento de Física Teórica, Universidad Autónoma D; España
Fil: Benson, Silvia. Carnegie Observatories; Estados Unidos
Fil: Montero Dorta, A. D.. Univesidad de Sao Paulo; Brasil
Fil: Padilla, Natalia Soledad. Pontificia Universidad Católica de Chile; Chile
Fil: Prada, Federico. Instituto de Astrofísica de Andalucía; España
Fil: Thomas, Pablo Daniel. Institute Of Cosmology And Gravitation; Reino Unido