TY - JOUR
TI - Reproducing the universe: A comparison between the EAGLE simulations and the nearby DustPedia galaxy sample
AU - Trčka, A.
AU - Baes, M.
AU - Camps, P.
AU - Meidt, S.E.
AU - Trayford, J.
AU - Bianchi, S.
AU - Casasola, V.
AU - Cassarà, L.P.
AU - de Looze, I.
AU - de Vis, P.
AU - Dobbels, W.
AU - Fritz, J.
AU - Galametz, M.
AU - Galliano, F.
AU - Katsianis, A.
AU - Madden, S.C.
AU - Mosenkov, A.V.
AU - Nersesian, A.
AU - Viaene, S.
AU - Xilouris, E.M.
JO - Monthly Notices of the Royal Astronomical Society
PY - 2020
VL - 494
TODO - 2
SP - 2823-2838
PB - Oxford University Press
SN - 0035-8711, 1365-2966
TODO - 10.1093/MNRAS/STAA857
TODO - null
TODO - We compare the spectral energy distributions (SEDs) and inferred physical properties for simulated and observed galaxies at low redshift. We exploit UV-submillimetre mock fluxes of ∼7000 z = 0 galaxies from the EAGLE suite of cosmological simulations, derived using the radiative transfer code SKIRT. We compare these to ∼800 observed galaxies in the UV-submillimetre range, from the DustPedia sample of nearby galaxies. To derive global properties, we apply the SED fitting code CIGALE consistently to both data sets, using the same set of ∼80 million models. The results of this comparison reveal overall agreement between the simulations and observations, both in the SEDs and in the derived physical properties, with a number of discrepancies. The optical and far-infrared regimes, and the scaling relations based upon the global emission, diffuse dust, and stellar mass, show high levels of agreement. However, the mid-infrared fluxes of the EAGLE galaxies are overestimated while the far-UV domain is not attenuated enough, compared to the observations. We attribute these discrepancies to a combination of galaxy population differences between the samples and limitations in the subgrid treatment of star-forming regions in the EAGLE-SKIRT post-processing recipe. Our findings show the importance of detailed radiative transfer calculations and consistent comparison, and provide suggestions for improved numerical models. © 2020 The Author(s)
ER -