Artículo de revista
The evolution of the star formation rate function and cosmic star formation rate density of galaxies at z ∼ 1–4
Fecha
2017Registro en:
MNRAS 464, 4977–4994 (2017)
10.1093/mnras/stw2680
Autor
Katsianis, Antonios
Tescari, E.
Blanc Mendiberri, Guillermo
Sargent, M.
Institución
Resumen
We investigate the evolution of the galaxy star formation rate function (SFRF) and cosmic star
formation rate density (CSFRD) of z ∼ 1–4 galaxies, using cosmological smoothed particle
hydrodynamic (SPH) simulations and a compilation of ultraviolet (UV), infrared (IR) and
Hα observations. These tracers represent different populations of galaxies with the IR light
being a probe of objects with high star formation rates and dust contents, while UV and
Hα observations provide a census of low star formation galaxies where mild obscuration
occurs. We compare the above SFRFs with the results of SPH simulations run with the code
P-GADGET3(XXL). We focus on the role of feedback from active galactic nuclei (AGN) and
supernovae in form of galactic winds. The AGN feedback prescription that we use decreases
the simulated CSFRD at z < 3 but is not sufficient to reproduce the observed evolution at
higher redshifts. We explore different wind models and find that the key factor for reproducing
the evolution of the observed SFRF and CSFRD at z ∼ 1–4 is the presence of a feedback
prescription that is prominent at high redshifts (z ≥ 4) and becomes less efficient with time.
We show that variable galactic winds which are efficient at decreasing the SFRs of low-mass
objects are quite successful in reproducing the observables.
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