Reproducing the Universe: a comparison between the EAGLE simulations and the nearby DustPedia galaxy sample. (arXiv:2003.12576v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Trcka_A/0/1/0/all/0/1">Ana Trčka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baes_M/0/1/0/all/0/1">Maarten Baes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Camps_P/0/1/0/all/0/1">Peter Camps</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meidt_S/0/1/0/all/0/1">Sharon E. Meidt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Trayford_J/0/1/0/all/0/1">James Trayford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bianchi_S/0/1/0/all/0/1">Simone Bianchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Casasola_V/0/1/0/all/0/1">Viviana Casasola</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cassara_L/0/1/0/all/0/1">Letizia P. Cassarà</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Looze_I/0/1/0/all/0/1">Ilse De Looze</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vis_P/0/1/0/all/0/1">Pieter De Vis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dobbels_W/0/1/0/all/0/1">Wouter Dobbels</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fritz_J/0/1/0/all/0/1">Jacopo Fritz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galametz_M/0/1/0/all/0/1">Maud Galametz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galliano_F/0/1/0/all/0/1">Frédéric Galliano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Katsianis_A/0/1/0/all/0/1">Antonios Katsianis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Madden_S/0/1/0/all/0/1">Suzanne C. Madden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mosenkov_A/0/1/0/all/0/1">Aleksandr V. Mosenkov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nersesian_A/0/1/0/all/0/1">Angelos Nersesian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Viaene_S/0/1/0/all/0/1">Sébastien Viaene</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xilouris_E/0/1/0/all/0/1">Emmanuel M. Xilouris</a>
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.
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.
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