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tokens: ( z ∼ 7) and with the cosmic SFR derived by Bouwens et al. ( 2015 ; or Finkelstein et al. 2015 ) up to z ∼ 10. We conclude that gaea is able to reproduce the overall evolution of the LFs, GSMF, and cosmic SFR over the redshift range 0 z 10. It is worth stressing that the good level of agreement shown in this Letter is obtained without any retuning of the feedback parameters (which have been calibrated by Hirschmann et al. 2016 against lower-redshift observables). Our findings agree with recent results from the MUFASA simulation suite (Davé et al. 2016 ), which implements a kinetic feedback scheme with scalings based on the parameterization provided in Muratov et al. ( 2015 ). They show that the MUFASA runs are able to reproduce the evolution of cosmic SFR and the GSMF at and the evolution of its low-mass end slope up to z ∼ 6 (where the simulated volume is too small to efficiently sample the high-mass end of the GSMF). A critical point of the analysis presented here is the treatment of dust attenuation. In this Letter, we consider both intrinsic and dust-attenuated magnitudes. Despite the simplified dust model adopted, we show that the bright ends of the corresponding LFs bracket the observed LFs. Our results are in qualitative agreement with the Bouwens et al. ( 2009 ) inferences based on the UV continuum of the sources, i.e., that dust attenuation should decrease at increasing redshifts, becoming negligible at . We note that a significant level of dust attenuation is required by the fiducial feedback scheme to match the shape of the observed LFs, in agreement with previous studies (Lo Faro et al. 2009 ; Lacey et al. 2011 ; Cai et al. 2014 ). Intrinsic and attenuated LFs converge below the knee of the LFs, again in qualitative agreement with the estimates by Bouwens et al. ( 2009 ) of a lower dust attenuation for fainter sources. The predicted level of dust attenuation at high redshift thus represents a powerful discriminant between different feedback schemes. Therefore, further insight into our understanding of galaxy evolution at is tightly connected to a better description of this key aspect. From a theoretical perspective, the implementation of a self-consistent dust treatment in theoretical models of galaxy evolution, able to follow dust production and destruction alongside with galaxy assembly (see, e.g., the recent work by Popping et al. 2016 ), represents a promising avenue. In addition, dust provides an important channel for molecular hydrogen formation and can therefore play a crucial role in regulating star formation at different cosmic epochs. This modeling is beyond the aims of this Letter and will be the subject of future work. Here, we just highlight that our conclusions will change dramatically if a substantial fraction of the SFR density is related to highly obscured objects, as some studies suggest at (Rowan-Robinson et al. 2016 ). In order to clearly assess the contribution of dusty sources to the SFR density at ,