Modeling the connection between ultraviolet and infrared galaxy
  populations across cosmic times
  Using a phenomenological approach, we self-consistently model the redshift
evolution of the ultraviolet (UV) and infrared (IR) luminosity functions across
cosmic time, as well as a range of observed IR properties of UV-selected galaxy
population. This model is an extension of the 2SFM (2 star-formation modes)
formalism, which is based on the observed "main-sequence" of star-forming
galaxies, i.e. a strong correlation between their stellar mass and their star
formation rate (SFR), and a secondary population of starbursts with an excess
of star formation. The balance between the UV light from young, massive stars
and the dust-reprocessed IR emission is modeled following the empirical
relation between the attenuation (IRX for IR excess hereafter) and the stellar
mass, assuming a scatter of 0.4\,dex around this relation. We obtain a good
overall agreement with the measurements of the IR luminosity function up to z~3
and the UV luminosity functions up to z~6, and show that a scatter on the IRX-M
relation is mandatory to reproduce these observables. We also naturally
reproduce the observed, flat relation between the mean IRX and the UV
luminosity at L$_{\rm UV}>$10$^{9.5}$ L$_\odot$. Finally, we perform
predictions of the UV properties and detectability of IR-selected samples and
the vice versa, and discuss the results in the context of the UV-rest-frame and
sub-millimeter surveys of the next decade.
